text:
Stars/Sciences

A division of astronomical objects between rocky objects, liquid objects, gas objects (including gas giants and stars), and plasma objects may be natural and informative. This division allows moons like Io to be viewed as rocky objects like Earth as part of planetary science rather than as a satellite around a star like Jupiter.

A further benefit is the view of gaseous objects as potential stars, failed stars, or stars radiant over peak radiation bands. These objects may be best studied as a part of stellar science.

Each of the gas objects described are by approximate radius, increasing from apparent gas dwarfs, through gas giants, to large stars with examples.

Viewing a gaseous object with multiple radiation astronomy detectors may uncover what the object looks like beneath the gas. In some instances the gaseous object turns out to have a detectable rocky interior.

Accompanying higher temperatures is usually plasma with its ionized atoms. Around a gaseous object this plasma may be a coronal cloud.

Objects with parallax measurements available are especially helpful as such measurements allow the determination of the object's radius.

Astronomy
A nomy (Latin nomia) is a "system of laws governing or [the] sum of knowledge regarding a (specified) field."

When any effort to acquire a system of laws or knowledge focusing on an astr, aster, or astro, that is, any natural body in the sky especially at night, succeeds even in its smallest measurement, astronomy is the name of the effort and the result.

While natural objects in the sky, especially at night, may be sensed by sight, sound, smell, taste, or touch (vibration), many have been seen from the light they emit, absorb, reflect, transmit, or fluoresce.

Some of the natural emitters are stars.

Sciences
Nomology is the "science of physical and logical laws."

Stellar classification is a classification of stars based on their spectral characteristics. The spectral class of a star is a designated class of a star describing the ionization of its chromosphere, what atomic excitations are most prominent in the light, giving an objective measure of the temperature in this chromosphere.

The luminosity class is expressed by the Roman numbers I, II, III, IV and V, expressing the width of certain absorption lines in the star's spectrum.

Luminescences
Def. the natural medium emanating from the sun and other very hot sources (now recognised as electromagnetic radiation with a wavelength of 400-750 nm), within which vision is possible is called light.

Def. to shine light on something is called illuminate.

Def. emitting light is called luminous.

Def. any emission of light that cannot be attributed merely to the temperature of the emitting body is called luminescence.

Def.

 * 1) the state of being luminous or a luminous object,
 * 2) the ratio of luminous flux to radiant flux at the same wavelength, and
 * 3) the rate at which a star radiates energy in all directions

is called luminosity.

Stars
A star is a massive, luminous sphere of plasma held together by gravity. This is a traditional definition of a star. The term "luminous" relates to light, specifically visible light, as it is perceived by the human eye.

From a dictionary:

Def.

 * 1.a: "any natural luminous body visible in the sky [especially] at night",
 * 1.b: "a self-luminous gaseous celestial body of great mass whose shape is [usually] spheroidal and whose size may be as small as the earth or larger than the earth's orbit".

is called a star.

From astrophysics:

Def. "any object forming on a dynamical timescale, by gravitational instability", is called a star.

Def. a star that exists alone, is secluded or isolated from other stars, a reclusive or hermitary star, is called a solitary star.

Def. a separate, distinct, or individual star from others in a group is called a single star.

A solitary star differs from a single star in that the former exists alone, secluded or isolated from other stars. For example, Psi2 Aquarii (93 Aquarii) is a solitary star. Radial velocity measurements have not yet revealed the presence of planets orbiting it.

18 Scorpii is another solitary star.

Def. a star that shares a barycenter with one or more astronomical substellar objects is called a unary star.

A unary star contrasts with a binary star, trinary (three stars), and a multiple star. It is not necessarily alone like the solitary star.

Def. a star moving faster than 65 km/s to 100 km/s relative to the average motion of the stars in the Sun's neighbourhood is called a high-velocity star.

Def. a high-velocity star moving through space with an abnormally high velocity relative to the surrounding interstellar medium is called a runaway star.

Def. a star whose elliptical orbit takes it well outside the plane of [its galaxy] at steep angles is called a halo star.

Astrognosy
Stellar astrognosy, or perhaps stellagnosy as Latin for "star" is stella, deals with the materials of stars and their general exterior and interior constitution.

At right is a diagram of the internal rotation in the Sun, showing differential rotation in the outer convective region and almost uniform rotation in the central radiative region. The transition between these regions is called the tachocline.

Until the advent of helioseismology, the study of wave oscillations in the Sun, very little was known about the internal rotation of the Sun. The differential profile of the surface was thought to extend into the solar interior as rotating cylinders of constant angular momentum. Through helioseismology this is now known not to be the case and the rotation profile of the Sun has been found. On the surface the Sun rotates slowly at the poles and quickly at the equator. This profile extends on roughly radial lines through the solar convection zone to the interior. At the tachocline the rotation abruptly changes to solid body rotation in the solar radiation zone.

Radiative zones
From the experimentally derived diagram at the upper right using helioseismology, the apparent radiative zone begins at about 0.64 Rʘ and continues inward.

Tachoclines
With reference to the above helioseismology diagram, the tachocline extends outward from the radiative zone to at most 0.70 Rʘ.

Convection zones
The zone or spherical shell between the tachocline and the photosphere appears to consist of two shells: an inner apparent convective sphere and an outer shell beneath the photosphere of which the photosphere may be a part.

Photospheres
Def. a visible surface layer of a star, and especially that of a sun is called a photosphere.

"When we speak of the surface of the Sun, we normally mean the photosphere." "[T]he photosphere may be thought of as the imaginary surface from which the solar light that we see appears to be emitted. The diameter quoted for the Sun usually refers to the diameter of the photosphere." The photosphere emits visual, or visible, radiation.

Chromospheres
The chromosphere (literally, "sphere of color") is the second of the three main layers in the Sun's atmosphere and is roughly 2,000 kilometers deep. It sits just above the photosphere and just below the solar transition region.

"The density of the chromosphere is very small, it being only 10−4 times that of the photosphere, the layer just below it, and 10−8 times that of the atmosphere of Earth. This makes the chromosphere normally invisible and it can only be seen during a total eclipse, where its reddish color is revealed. The color hues are anywhere between pink and red. However, without special equipment, the chromosphere cannot normally be seen due to the overwhelming brightness of the photosphere.

"The density of the chromosphere decreases with distance from the center of the sun. This decreases logarithmically from 1017 particles per cubic centimeter, or approximately $2 kg/m^{3}$ to under $1.6 kg/m^{3}$ at the outer boundary.

The temperature begins to decrease from the inner boundary of about 6,000 K to a minimum of approximately 3,800 K, before increasing to upwards of 35,000 K at the outer boundary with the transition layer of the corona.

Transition regions
"The solar transition region is a region of the Sun's atmosphere, between the chromosphere and corona. It is visible from space using telescopes that can sense ultraviolet. It is important because it is the site of several unrelated but important transitions in the physics of the solar atmosphere:
 * "Below, most of the helium is not fully ionized, so that it radiates energy very effectively; above, it is fully ionized.
 * "Below, gas pressure and fluid dynamics dominate the motion and shape of structures; above, magnetic forces dominate the motion and shape of structures, giving rise to different simplifications of magnetohydrodynamics.

Stellar geography
As geography is the graphy of the geo or Earth, let stellagraphy be the graphy of the surface of any star.

"When we speak of the surface of the Sun [or a star], we normally mean the photosphere." "[T]he photosphere may be thought of as the imaginary surface from which the solar light that we see appears to be emitted. The diameter quoted for the Sun usually refers to the diameter of the photosphere."

The surface of a star may be often described by features observed. These are located using stellagraphic coordinates based on stellagraphic north and south poles. The surface of a star usually rotates, has a rotational north and south pole, and there may have an assignable central meridian.

Stellametry
Def. the measurement of the physical properties of a star may be called stellametry.

Temperatures
Def.

 * 1) a measure of cold or heat
 * 2) the degree or intensity of heat present in a substance or object

is called a temperature.

Def. the internal energy of a system in thermodynamic equilibrium is called heat, or thermal energy.

Def. having a low temperature is called cold.

Def.

 * 1) a quantity that denotes the ability to do work and is measured in a unit dimensioned in mass × distance²/time² (ML²/T²) or the equivalent
 * 2) the impetus behind all motion and all activity
 * 3) the capacity to do work

is called energy.

Pressures
A density (ρ) of up to 150 g cm-3 is predicted to produce nuclear fusion.

This may relate approximately to a pressure (p) given by

 * $$ p = \rho g h,$$

where h is the height z − z0 of the liquid column between the test volume and the zero reference point of the pressure. Note that this reference point should lie at or below the surface of the liquid.

Radius
Notation: let the symbol $$R_{\odot}$$ indicate the solar radius.

The "[s]olar radius is a unit of distance used to express the size of stars in astronomy equal to the current radius of the Sun:

 * $$R_{\odot} = 6.955\times 10^8\,\hbox{m} = 0.0046491\,\hbox{AU} = 2.254\times 10^{-8}\,\hbox{pc}$$

The solar radius is approximately 695,500 kilometres (432,450 miles) or about 110 times the radius of the Earth ($$R_\oplus$$), or 10 times the average radius of Jupiter. It varies slightly from pole to equator due to its rotation, which induces an oblateness of order 10 parts per million.

Stellar groupings
Def. two stars that appear to be one when seen with the naked eye is called a double star.

Def. a star that appears as a double due to an optical illusion; in reality, the stars may be far apart from each other is called an optical double.

Def. two and only two stars orbiting around their apparent barycenter is called a binary star.

Def. a binary star whose components can be visually resolved is called a visual binary.

Def. a group of gravitationally bound stars is called a star cluster.

Def. a more or less irregular star cluster containing tens to thousands of stars" is called an open cluster.

Def. a spherical star cluster containing thousands to millions of stars is called a globular cluster.

Def. a large group of many stars spread over a very many light-years of space a region of greater than average stellar density is called a star cloud.

Def. a group of stars moving together through space is called a stellar association.

Def. an association of stars stretched out along its orbit of a galaxy is called a stellar stream.

Def. a stellar association drifting through the galaxy as a somewhat coherent assemblage is called a moving group.

Def. any of the collections of many millions of stars existing as independent and coherent systems is called a galaxy.

Def. any galaxy, considerably smaller than the Milky Way, that has only several billions of stars is called a dwarf galaxy.

Def. a small group of stars that forms a visible pattern but is not an official constellation is called an asterism.

Def. any of the 89 officially recognized regions of the sky, including all stars is called a constellation.

Evolution
Def. gradual directional change especially one leading to a more advanced or complex form is called evolution.

Studies of stratigraphic data have suggested that the solar cycles have been active for hundreds of millions of years, if not longer; measuring varves in precambrian sedimentary rock has revealed repeating peaks in layer thickness, with a pattern repeating approximately every eleven years. It is possible that the early atmosphere on Earth was more sensitive to changes in solar radiation than today, so that greater glacial melting (and thicker sediment deposits) could have occurred during years with greater sunspot activity. This would presume annual layering; however, alternate explanations (diurnal) have also been proposed.

Analysis of tree rings has revealed a detailed picture of past solar cycles: Dendrochronologically dated [carbon-14] radiocarbon concentrations have allowed for a reconstruction of sunspot activity dating back 11,400 years, far beyond the four centuries of available, reliable records from direct solar observation.

The earliest surviving record of sunspot observation dates from 364 BC, based on comments by Chinese astronomer Gan De in a star catalogue. By 28 BC, Chinese astronomers were regularly recording sunspot observations in official imperial records.

Variations in the Sun's past indicate that at least one star may have undergone some changes over relatively long time periods.

Viewing distant stars millions of light years away may suggest historical changes, but whether these changes constitute an evolution by direct evidence seems unlikely.

Theoretical stars
Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.

Entities
"Where the aim is to understand the collective behavior of vast numbers of interacting entities, computation offers a more direct mode of investigation than has ever been possible in the past."

"The system implements intelligent agents, defined as computational entities that perform their actions with some level of proactivity and/or responsiveness."

"Are the Thin and Thick Disks Distinct Entities? Is the disk system adequately modeled by the superposition of a thin-disk and thick-disk population; that is, are these two components demonstrably distinct from one another?"

Objects
"The objects in this region remained undiscovered until 1992 when the first Trans-Neptunian Object (TNO) was discovered (Jewitt & Luu 1993)."

"Astronomy has its own megacatalog: the Sloan Digital Sky Survey [SDSS] will list 100 million objects."

"Gathering all the spectrophotometric information available for a given object implied, firstly, to identify the services of interest, then, submit the same query for each one the services and, once all the information has been collected, tackle problems related to the unit conversions, flux calibrations and/or data formats."

"Some of these stars are intended spectroscopic targets: there are standards of various kinds, stars targeted for stellar science and/or Galactic structure science, and objects that are assigned spectroscopic fibers due to their unusual location in 5-color space."

Continua
"We know that within 1.5 billion years after the Big Bang, some galaxies had formed; this is evidenced by galaxies observed to z ∼6. Even at this epoch most of the intergalactic medium was ionized as evidenced by the lack of continuum absorption redward of Lyman α (the Gunn-Peterson effect, Gunn & Peterson 1965). It must be concluded that some objects must have existed earlier that produced sufficient UV flux to ionise nearly all the baryonic matter in the Universe." Bold added.

"It [the Solar Oscillation Imager (SOI) onboard Ulysses] will provide high precision solar images 1024x1024 of line-of-sight velocity, line intensity, continuum intensity, longitudinal magnetic field and limb position." Bold added.

"Whereas white–light flares (flares detected in optical continuum emission) are rare on the Sun, they are common on active stars. Even the quiescent coronae in active stars can have X–ray luminosities that are 10-3 of the total stellar luminosity, compared to 10-6 or so for the quiet Sun." Bold added.

Emissions
"The Sun is characterised by high variability in its X-ray emission. This variability is attributed to flares that are defined as short duration X-ray bursts. ... [X-ray Solar Monitor (XSM) onboard SMART-1] XSM provides X-ray measurements for independent solar and stellar science."

"In particular emission from newly formed stars of type earlier than A, observed at wavelengths below 160nm, will allow study of the co-moving star formation density in the low-Z Universe."

"[A]t the relatively low level of coronal activity exhibited by the Sun, the FUV C IV λλ1548,50 doublet radiates nearly as much luminosity as the entire 0.2-2 keV corona. This is a rather curious fact, with regard to the traditional picture of coronal loops in which the X-ray radiation from the bulk of the ~ 106 K magnetically confined plasma is comparable to the conductive flux down through the loop footpoints ..., which ultimately is degraded into FUV transition zone emission (i.e., near 105 K). In particular, C IV is only one of several important TZ emissions (including the bright O V λ630 and C III λ977 lines), so LC IV is a lower limit to the true radiative loss from the subcoronal layers."

Absorptions
"Of particular importance has been access to high resolution R~40,000-100,000 echelle spectra providing an ability to study the dynamics of hot plasma and separate multiple stellar and interstellar absorption components."

"In these spectral regions, located near the gain peaks of Yb and Er, standard emission lamps and absorption cells have sparse coverage."

"The use of this isotopologue of methane shifts absorption features away from the more common telluric 12CH4 absorption features."

Bands
"Only the r- and i-band filters have additional short wavepass coatings to define the bandpass."

"WSO/UV can considerably improve our understanding of accretion processes onto supermassive black holes in active galaxies, as their main energy output is in the far UV/extreme UV domain, and rich emission lines and occasionally absorption lines associated with surrounding gas are visible in the far UV band."

Backgrounds
"The background was subtracted for RHESSI, whereas XSM background is negligible."

"We do believe that unresolved background stars explain the occasional cases where different colors predict very different temperatures. ... A significant contribution from background stars would in general combine light from stars with different temperatures."

"Do we know enough about the intergalactic medium to trust measurements of background sources seen through foreground structure?"

Meteors
At left is a radiated object, the binary star Mira, and its associated phenomena.

Ultra-violet studies of Mira by NASA's Galaxy Evolution Explorer (Galex) space telescope have revealed that it sheds a trail of material from the outer envelope, leaving a tail 13 light-years in length, formed over tens of thousands of years. It is thought that a hot bow-wave of compressed plasma/gas is the cause of the tail; the bow-wave is a result of the interaction of the stellar wind from Mira A with gas in interstellar space, through which Mira is moving at an extremely high speed of 130 kilometres/second (291,000 miles per hour). The tail consists of material stripped from the head of the bow-wave, which is also visible in ultra-violet observations. Mira's bow-shock will eventually evolve into a planetary nebula, the form of which will be considerably affected by the motion through the interstellar medium (ISM).

At second right is the only available X-ray image, by the Chandra X-ray Observatory, of Mira A on the right and Mira B (left). "Mira A is losing gas rapidly from its upper atmosphere [apparently] via a stellar wind. [Mira B is asserted to be a white dwarf. In theory] Mira B exerts a gravitational tug that creates a gaseous bridge between the two stars. Gas from the wind and bridge accumulates in an accretion disk around Mira B and collisions between rapidly moving particles in the disk produce X-rays."

Mira A, spectral type M7 IIIe, has an effective surface temperature of 2918–3192. Mira A is not a known X-ray source according to SIMBAD, but here is shown to be one.

Cosmic rays
There is "a correlation between the arrival directions of cosmic rays with energy above 6 x 1019 electron volts and the positions of active galactic nuclei (AGN) lying within ~75 megaparsecs."

"[T]he relative abundances of solar cosmic rays reflect those of the solar photosphere for multicharged nuclei with approximately the same nuclear charge-to-mass ratio."

Plasma objects
In addition to the Sun there are "many other plasma objects such as stars of different types [and] spherical lightning".

"The [beryllium] Be plasma concentrations and the changes in chemical and physical erosion were measured using a visible light spectroscopy system."

"During all experiments a bias voltage of −50 V was applied to the C target, the target temperatures were in the range from 500 to 1280 K and the Be plasma concentration was in the range from 0.02% to 0.2%."

Gaseous objects
"[T]he evolution of star accretion onto a supermassive gaseous object in the central region of an active galactic nucleus [may be addressed using] a gaseous model of relaxing dense stellar systems".

Liquid objects
"The influence of the reflection asymmetry degrees of freedom on the stability of rotating charged or gravitating liquid objects [shows] that the Poincaré instability can, indeed, appear in rotating gravitating objects, but is quite unlikely in rotating nuclei."

"The formation of liquid metallic hydrogen brings with it a new candidate for the interior of the Sun and the stars."

Rocky objects
"The presence of elements heavier than helium in white dwarf atmospheres is often a signpost for the existence of rocky objects that currently or previously orbited these stars."

"Al can be quite abundant in rocky objects formed at high temperatures".

Hydrogens
Early spectroscopy of the Sun using estimates of "the line intensities of several lines by eye [to derive] the abundances of ... elements ... [concluded] that the Sun [is] largely made of hydrogen."

Heliums
For the star HD 124448, "[s]pectrograms extending from Hα to about λ 3530, obtained at the McDonald Observatory, show no hydrogen lines either in absorption or in emission, although the helium lines are sharp and strong."

"The abundance of hydrogen appears to be very low in the atmosphere of this star. Besides the strong He I spectrum, lines of O II and C II are present."

"Two objects (SB 21 and TON-S 103) turn out to be extreme helium stars, with y ≈ 1.0."

Lithiums
TX Piscium (19 Piscium) is "a Li-rich carbon star".

"Super Lithium Rich giants (SLIR) are an elusive class of objects, serendipitously discovered."

"J37 has a Li abundance well above the meteoritic value ... Al, S, Si, Ca, Fe, and Ni are supersolar and that C is subsolar. ... Na, Sc, Ti are supersolar, while O is subsolar."

"J37 has a Li abundance near A(Li) = 4.3

 * $$ A(X) = 12 + log(N_X/N_H),$$

1 dex above the solar system meteoritic value."

Berylliums
"The atmospheres of the two program stars (HR 6158 = 28 Her = HD 149212; HR 8915 = 69 Peg = HD 220933) contain an inordinate amount of beryllium (Be); in fact, the Be abundances in these stars are among the highest known. ... lithium (Li) is detected in neither HR 6158 nor HR 8915."

Borons
A "sample of 23 stars contained objects with (1) strong Be and strong B, (2) weak Be and strong B, (3) strong Be and weak B, as well as (4) weak Be and B."

"Boron is estimated to be overabundant by at least 2.0 dex in these three stars [κ Cnc, HR 7361, and 20 Tau] ... Three [additional] stars (HR 2676, γ Crv, and HR 7143) show strong B II lines as in the case of κ Cnc".

Carbons
"[T[he hot PG1159 stars ... have a surface composition that is a mixture of helium, carbon, oxygen, and little or no hydrogen (Teff between ~75,000 and 200,000 K; typical abundances18), in mass fraction, of He, C, O and Ne are 33%, 50%, 15% and 2%)."

"H1504+65 ... is the hottest specimen of its class at Teff ≈ 200,000 K, and its atmospheric composition very unusual, with a mass fraction of ~ 50% C and ~ 50% O plus small traces of heavier elements, but no detectable helium or hydrogen."

Nitrogens
"[T]he sdO-star HD 127493 (Fig. 4) is nitrogen-rich. ... stars which exhibit a large 4542-discrepancy are nitrogen rich."

Oxygens
"H1504+65 ... [has] a mass fraction of ~ 50% C and ~ 50% O plus small traces of heavier elements, but no detectable helium or hydrogen."

Fluorines
"[E]xtreme fluorine abundances were determined in some stars (up to 200 times solar)".

Neons
"H 1504+65 is the hottest known white dwarf (Teff = 200 000 K). ... The atmosphere is primarily composed of carbon and oxygen, by equal amounts Werner (1991). In addition, a high abundance of neon [yields an] exotic surface chemistry (C = 49%, O = 49%, Ne = 2%, mass fractions) [modified by] soft X-ray spectrum ... with an abundance of about 2% [magnesium]".

Atmospheric sciences
Atmospheric sciences is an umbrella term for the study of the atmosphere, its processes, the effects other systems have on the atmosphere, and the effects of the atmosphere on these other systems.

Aeronomy is the study of the upper layers of the atmosphere, where dissociation and ionization are important.

Plasmas
Plasma is a state of matter similar to gas in which a certain portion of the particles are ionized. Heating a gas may ionize its molecules or atoms (reduce or increase the number of electrons in them), thus turning it into a plasma, which contains charged particles: positive ions and negative electrons or ions.

For plasma to exist, ionization is necessary. The term "plasma density" by itself usually refers to the "electron density", that is, the number of free electrons per unit volume. The degree of ionization of a plasma is the proportion of atoms that have lost or gained electrons, and is controlled mostly by the temperature. Even a partially ionized gas in which as little as 1% of the particles are ionized can have the characteristics of a plasma (i.e., response to magnetic fields and high electrical conductivity). The degree of ionization, α is defined as α = ni/(ni + na) where ni is the number density of ions and na is the number density of neutral atoms. The electron density is related to this by the average charge state  of the ions through ne =  ni where ne is the number density of electrons.

Gas dwarfs
There are astronomical bodies that initially appear as gas dwarfs. When examined via radiation astronomy, especially away from visual or optical astronomy, they may turn out to be small terrestrial or rocky objects.

How small a gas dwarf may be is unknown but explorable, at least among nearby objects.

Io
At right is an "eerie view of Jupiter's moon Io in eclipse ... acquired by NASA's Galileo spacecraft while the moon was in Jupiter's shadow. Gases above the satellite's surface produced a ghostly glow that could be seen at visible wavelengths (red, green, and violet). The vivid colors, caused by collisions between Io's atmospheric gases and energetic charged particles trapped in Jupiter's magnetic field, had not previously been observed. The green and red emissions are probably produced by mechanisms similar to those in Earth's polar regions that produce the aurora, or northern and southern lights. Bright blue glows mark the sites of dense plumes of volcanic vapor, and may be places where Io is electrically connected to Jupiter."

Titan
Titan like Venus is another gas dwarf when viewed in visible light. Much as with Venus prior to the Space Age, the dense, opaque atmosphere prevented understanding of Titan's surface until new information accumulated with the arrival of the Cassini–Huygens mission in 2004, including the discovery of liquid hydrocarbon lakes in the polar regions.

The atmosphere of Titan is largely composed of nitrogen; minor components lead to the formation of methane and ethane clouds and nitrogen-rich organic smog.

Titan has a mean radius of 2576 ± 2 km.

Mars
At right is an X-ray image of Mars. X-radiation from the Sun excites oxygen atoms in the Martian upper atmosphere, about 120 km above its surface, to emit X-ray fluorescence. A faint X-ray halo that extends out to 7,000 km above the surface of Mars has also been found. The Chandra X-ray Observatory image on the right is the first look at X-rays from Mars.

In X-ray astronomy, Mars is a gas dwarf.

Mars has an equatorial radius of 3,396.2 ± 0.1 km and a polar radius of 3,376.2 ± 0.1 km.

Sirius B
The image at right shows two sources and a spike-like pattern due to the support structure for the transmission grating. The bright source is Sirius B, a white dwarf star that has a surface temperature of about 25,000 degrees Celsius which produces very low energy X-rays. The dim source at the position of Sirius A – may be due to ultraviolet radiation from Sirius A leaking through the filter on the detector.

Sirius B clearly outshines Sirius A. The surface effective temperature of Sirius B (a white dwarf, DA2) is 25,200 K.

Sirius B has a radius of 5800 ± 200 km.

Venus
Violet photographs of the planet Venus taken in 1927 “recorded two nebulous bright streaks, or bands, running ... approximately at right angles to the terminator” that may be from the upper atmosphere.

When imaged in visible light (upper left) Venus appears like a gas dwarf rather than a rocky body. The same image result occurs when it is viewed in the ultraviolet (right).

Venus has a mean radius of 6,051.8 ± 1.0 km.

When Venus is viewed by radiation astronomy in addition to ultraviolet astronomy and visual astronomy, it is discovered to have a rocky interior suggesting that it is better understood and studied from the perspective of planetary science as a rocky object.

Procyon B
Procyon B has a radius of 8,542 ± 223 km and an effective surface temperature of 7,740 ± 50 K.

Procyon B is a faint white dwarf of spectral type DA. It lies at a distance of just 11.46 light-years (3.51 parsecs). It is more difficult to observe from Earth than Sirius B, due to a greater apparent magnitude difference and smaller angular separation from its primary. The average separation of the two components is 15.0 AUs, a little less than the distance between Uranus and the Sun, though the eccentric orbit carries them as close as 8.9 AUs and as far as 21.0 AU.

According to SIMBAD, Procyon B is ROSAT X-ray source 2RXP J073918.2+051334 and 2XMMi J073917.7+051324 by X-ray Multi-Mirror Mission - Newton.

Van Maanen's star
Van Maanen's star (van Maanen 2) is a white dwarf star. Out of the white dwarfs known, it is the third closest to the Sun, after Sirius B and Procyon B, in that order, and the closest known solitary white dwarf.

Van Maanen's star is located 14.1 light-years from the Sun in the constellation Pisces, about 2° to the south of the star Delta Piscium, with a relatively high proper motion of 2.98" annually.[6] It is too faint to be seen with the naked eye.

The optical negative at right was taken earlier than the current coordinates for Van Maanen's star, which are at the center of the negative.

Van Maanen's star has a radius of 9,000 ± 1,400 km. It's effective surface temperature is 6,220 ± 240 K.

Gas giants
Gas giants such as those astronomical objects in orbit around the Sun suggest themselves as failed stars or subdwarfs. At the least, they are usually larger than rocky objects. Whether there are rocky objects consistently larger than gas giants remains to be discovered.

A gas giant is an astronomical object within or relatively near in radius to those of the solar system.

Neptune
A trace amount of methane is also present. Prominent absorption bands of methane occur at wavelengths above 600 nm, in the red and infrared portion of the spectrum. As with Uranus, this absorption of red light by the atmospheric methane is part of what gives Neptune its blue hue, although Neptune's vivid azure differs from Uranus's milder cyan. Since Neptune's atmospheric methane content is similar to that of Uranus, some unknown atmospheric constituent is thought to contribute to Neptune's colour.

Neptune has an equatorial radius of 24,764 ± 15 km and a polar radius of 24,341 ± 30 km.

At right are three images of Neptune using infrared astronomy. "Thermal images of planet Neptune taken with VISIR on ESO's Very Large Telescope, obtained on 1 and 2 September 2006. These thermal images show a 'hot' south pole on Neptune. These warmer temperatures provide an avenue for methane to escape out of the deep atmosphere. Scientists say Neptune's south pole is 'hotter' than anywhere else on the planet by about 10°C. The average temperature on Neptune is about minus 200 degrees Celsius. The upper left image samples temperatures near the top of Neptune's troposphere (near 100 mbar pressure). The hottest temperatures are located at the lower part of the image at Neptune's south pole (see the graphic at the upper right). The lower two images, taken 6.3 hours apart, sample temperatures at higher altitudes in Neptune's stratosphere. They do show generally warmer temperatures near, but not at, the south pole. In addition they show a warm area which can be seen in the lower left image and rotated completely around the planet in the lower right image."

Uranus
In larger amateur telescopes with an objective diameter of between 15 and 23 cm, the planet appears as a pale cyan disk with distinct limb darkening.

Methane possesses prominent absorption bands in the visible and near-infrared (IR) making Uranus aquamarine or cyan in color.

Uranus has an equatorial radius of 25,559 ± 4 km and a polar radius of 24,973 ± 20 km.

Saturn
"Saturday is the day of Saturn, and the color of Saturn, according to astronomers, is said to be black".

Saturn is the sixth planet from the Sun and the second largest planet in the Solar System, after Jupiter. It is named after the Roman god Saturn. Saturn is a gas giant with an average radius about nine times that of Earth. Saturn has a ring system that consists of nine continuous main rings and three discontinuous arcs, composed mostly of ice particles with a smaller amount of rocky debris and dust. Sixty-two known moons orbit the planet; fifty-three are officially named. This does not include the hundreds of "moonlets" within the rings.

Saturn has an equatorial radius of 60,268 ± 4 km and a polar radius of 54,364 ± 10 km.

Jupiter
Jupiter has an equatorial radius of 71,492 ±4 km, a polar radius of 66,854 ±10 km, and a mean radius of 69,911 ± 6 km.

X-rays
The "image of Jupiter [at right] shows concentrations of auroral X-rays near the north and south magnetic poles." The Chandra X-ray Observatory accumulated X-ray counts from Jupiter for its entire 10-hour rotation on December 18, 2000. Note that X-rays from the entire globe of Jupiter are detected.

In the second at right is a diagram describing interaction with the local magnetic field. Jupiter's strong, rapidly rotating magnetic field (light blue lines in the figure) generates strong electric fields in the space around the planet. Charged particles (white dots), "trapped in Jupiter's magnetic field, are continually being accelerated (gold particles) down into the atmosphere above the polar regions, so auroras are almost always active on Jupiter. Electric voltages of about 10 million volts, and currents of 10 million amps - a hundred times greater than the most powerful lightning bolts - are required to explain the auroras at Jupiter's poles, which are a thousand times more powerful than those on Earth. On Earth, auroras are triggered by solar storms of energetic particles, which disturb Earth's magnetic field. As shown by the swept-back appearance in the illustration, gusts of particles from the Sun also distort Jupiter's magnetic field, and on occasion produce auroras."

Ultraviolets
"Experiments on the Voyager 1 and 2 spacecraft and observations made by the International Ultraviolet Explorer (IUE) have provided evidence for the existence of energetic particle precipitation into the upper atmosphere of Jupiter from the magnetosphere."

Visuals
"[O]range [is] the color of Jupiter".

The Great Red Spot (GRS) is a persistent anticyclonic storm, 22° south of Jupiter's equator, which has lasted for at least years and possibly longer than  years. The storm is large enough to be visible through Earth-based telescopes. Its dimensions are 24–40,000 km west–to–east and 12–14,000 km south–to–north. The spot is large enough to contain two or three planets the size of Earth. At the start of 2004, the Great Red Spot had approximately half the longitudinal extent it had a century ago, when it was 40,000 km in diameter. The Great Red Spot's latitude has been stable for the duration of good observational records, typically varying by about a degree.

It is not known exactly what causes the Great Red Spot's reddish color. Theories supported by laboratory experiments suppose that the color may be caused by complex organic molecules, red phosphorus, or yet another sulfur compound. The Great Red Spot (GRS) varies greatly in hue, from almost brick-red to pale salmon, or even white. The reddest central region is slightly warmer than the surroundings, which is the first evidence that the Spot's color is affected by environmental factors. The spot occasionally disappears from the visible spectrum, becoming evident only through the Red Spot Hollow, which is its niche in the South Equatorial Belt. The visibility of GRS is apparently coupled to the appearance of the SEB; when the belt is bright white, the spot tends to be dark, and when it is dark, the spot is usually light. The periods when the spot is dark or light occur at irregular intervals; as of 1997, during the preceding 50 years, the spot was darkest in the periods 1961–66, 1968–75, 1989–90, and 1992–93.

Infrareds
"Spectra from the Voyager I IRIS experiment confirm the existence of enhanced infrared emission near Jupiter's north magnetic pole in March 1979." "Some species previously detected on Jupiter, including CH3D, C2H2, and C2H6, have been observed again near the pole. Newly discovered species, not previously observed on Jupiter, include C2H4, C3H4, and C6H6. All of these species except CH3D appear to have enhanced abundances at the north polar region with respect to midlatitudes."

The image at lower right is "of Jupiter taken in infrared light on the night of [August 17, 2008,] with the Multi-Conjugate Adaptive Optics Demonstrator (MAD) prototype instrument mounted on ESO's Very Large Telescope. This false color photo is the combination of a series of images taken over a time span of about 20 minutes, through three different filters (2, 2.14, and 2.16 microns). The image sharpening obtained is about 90 milli-arcseconds across the whole planetary disc, a real record on similar images taken from the ground. This corresponds to seeing details about 186 miles wide on the surface of the giant planet. The great red spot is not visible in this image as it was on the other side of the planet during the observations. The observations were done at infrared wavelengths where absorption due to hydrogen and methane is strong. This explains why the colors are different from how we usually see Jupiter in visible-light. This absorption means that light can be reflected back only from high-altitude hazes, and not from deeper clouds. These hazes lie in the very stable upper part of Jupiter's troposphere, where pressures are between 0.15 and 0.3 bar. Mixing is weak within this stable region, so tiny haze particles can survive for days to years, depending on their size and fall speed. Additionally, near the planet's poles, a higher stratospheric haze (light blue regions) is generated by interactions with particles trapped in Jupiter's intense magnetic field."

Gliese 229B
Gliese 229B is a brown dwarf and has a radius approximately the same as Jupiter's.

Proxima Centauri
Proxima Centauri is a red dwarf star about 4.22 light-years (4.0×1013 km) distant in the constellation of Centaurus.

Proxima Centauri has a radius of 98,100 ± 4,900 km. Its surface effective temperature is 3,042 ± 117 K.

Although it has a very low average luminosity, Proxima is a flare star that undergoes random dramatic increases in brightness because of magnetic activity.

More than 85% of its radiated power is at infrared wavelengths.

The chromosphere of this star is active, and its spectrum displays a strong emission line of singly ionized magnesium at a wavelength of 280 nm. About 88% of the surface of Proxima Centauri may be active, a percentage that is much higher than that of the Sun even at the peak of the solar cycle. Even during quiescent periods with few or no flares, this activity increases the corona temperature of Proxima Centauri to 3.5 million K, compared to the 2 million K of the Sun's corona.

Proxima Centauri has a relatively weak stellar wind, resulting in no more than 20% of the Sun's mass loss rate from the solar wind.

TWA 5B
TWA 5B has an inferred radius between 167,000 and 216,000 km.

"Using NASA's Chandra X-ray Observatory, scientists have detected X-rays from a low-mass brown dwarf in a multiple star system. This is the first time that a brown dwarf this close to its parent star(s) (Sun-like stars TWA 5A) has been resolved in X-rays. "Our Chandra data show that the X-rays originate from the brown dwarf's coronal plasma which is some 3 million degrees Celsius", said Yohko Tsuboi of Chuo University in Tokyo. "This brown dwarf is as bright as the Sun today in X-ray light, while it is fifty times less massive than the Sun", said Tsuboi. "This observation, thus, raises the possibility that even massive planets might emit X-rays by themselves during their youth!"

At right is an image from NASA's Chandra X-ray Observatory which shows X-rays produced by TWA 5B, a brown dwarf orbiting a young binary star system "known as TWA 5A. The [star] system is 180 light years from the Sun and a member of a group of about a dozen young stars in the constellation Hydra. The brown dwarf orbits the binary star system at a distance about 2.75 times that of Pluto's orbit around the Sun." The sizes of the sources in the image are due to an instrumental effect that causes the spreading of pointlike sources.

"Brown dwarfs are often referred to as "failed stars" [because] they [may be] under the mass limit (about 80 Jupiter masses", or 8 percent of the mass of the Sun) needed to spark the nuclear fusion of hydrogen to helium which supplies the energy for stars such as the Sun. Lacking any central energy source, brown dwarfs are intrinsically faint and draw their energy from a very gradual shrinkage or collapse.

Young brown dwarfs, like young stars, have turbulent interiors. When combined with rapid rotation, this turbulent motion can lead to a tangled magnetic field that can heat their upper atmospheres, or coronas, to a few million degrees Celsius. "Our Chandra data show that the X-rays originate from the brown dwarf's coronal plasma which is some 3 million degrees Celsius," said Yohko Tsuboi of Chuo University in Tokyo.

"TWA 5B is estimated to be only between 15 and 40 times the mass of Jupiter, making it one of the least massive brown dwarfs known. Its mass is rather near the boundary, about 12 Jupiter masses, between planets and brown dwarfs", so these results could have implications for the possible X-ray detection of very massive planets around stars.

Sun
At right is a visual image of the Sun, which is the star around which the Earth orbits. This image shows the ball that is the photosphere of the Sun, the surface of the Sun.

"When we speak of the surface of the Sun, we normally mean the photosphere." "[T]he photosphere may be thought of as the imaginary surface from which the solar light that we see appears to be emitted. The diameter quoted for the Sun usually refers to the diameter of the photosphere."

The color of a star, as determined by the peak frequency of the visible light, depends on the temperature of the star's outer layers, including its photosphere. The effective temperature of the surface of the Sun's photosphere is 5,778 K. The temperature at the bottom of the Sun's photosphere is 6600 K", while the "[t]emperature at [the] top of [the] photosphere [is] 4400 K". The photosphere is "~400 km" in thickness.

The peak emittance wavelength of 501.5 nm (~0.5 eV) makes the photosphere a primarily green radiation source. The figure at the right shows the extraterrestrial solar spectral irradiance as compared with a blackbody spectrum. There is a sharper than black-body cutoff at the shorter wavelength end.

The Sun has an equatorial radius of 695,500 km

Betelgeuse
"The yellow/red "image" or "photo" of Betelgeuse usually seen is actually not a picture of the red giant but rather a mathematically generated image based on the photograph. The photograph was actually of much lower resolution: The entire Betelgeuse image fit entirely within a 10x10 pixel area on the Hubble Space Telescopes Faint Object Camera. The actual images were oversampled by a factor of 5 with bicubic spline interpolation, then deconvolved."

The image at right is "of the supergiant star Betelgeuse obtained with the NACO adaptive optics instrument on ESO’s Very Large Telescope. The use of NACO combined with a so-called “lucky imaging” technique, allows the astronomers to obtain the sharpest ever image of Betelgeuse, even with Earth’s turbulent, image-distorting atmosphere in the way. The resolution is as fine as 37 milliarcseconds, which is roughly the size of a tennis ball on the International Space Station (ISS), as seen from the ground. The image is based on data obtained in the near-infrared, through different filters. The field of view is about half an arcsecond wide, North is up, East is left."

Betelgeuse has an estimated diameter of ~8.21 x 106 km, but "[t]he precise diameter has been hard to define for several reasons:

 * 1) The rhythmic expansion and contraction of the photosphere [may mean] the diameter is never constant;
 * 2) There is no definable "edge" to the star as limb darkening causes the optical emissions to vary in color and decrease the farther one extends out from the center;
 * 3) Betelgeuse is surrounded by a circumstellar envelope composed of matter being ejected from the star—matter which both absorbs and emits light—making it difficult to define the edge of the photosphere;
 * 4) Measurements can be taken at varying wavelengths within the electromagnetic spectrum, with each wavelength revealing something different. Studies have shown that angular diameters are considerably larger at visible wavelengths, decrease to a minimum in the near-infrared, only to increase again in the mid-infrared.  The difference in reported diameters can be as much as 30–35%, yet because each wavelength measures something different, comparing one finding with another is problematic;
 * 5) Atmospheric twinkling limits the resolution obtainable from ground-based telescopes since turbulence degrades angular resolution.

"Assuming a distance of 197±45pc, an angular distance of 43.33±0.04 mas would equate to a radius of 4.3 AU".

"Images of hotspots on the surface of Betelgeuse [are] taken at visible and infra-red wavelengths using high resolution ground-based interferometers".

Chemistry
Laboratory conditions are often expressed in terms of standard temperature and pressure.

Standard condition for temperature and pressure are standard sets of conditions for experimental measurements established to allow comparisons to be made between different sets of data. The most used standards are those of the International Union of Pure and Applied Chemistry (IUPAC) and the National Institute of Standards and Technology (NIST), although these are not universally accepted standards. Other organizations have established a variety of alternative definitions for their standard reference conditions.

In chemistry, IUPAC established standard temperature and pressure (informally abbreviated as STP) as a temperature of 273.15 K (0 °C, 32 °F) and an absolute pressure of 100 kPa (14.504 psi, 0.986 atm, 1 bar), An unofficial, but commonly used standard is standard ambient temperature and pressure (SATP) as a temperature of 298.15 K (25 °C, 77 °F) and an absolute pressure of 100 kPa (14.504 psi, 0.986 atm). The STP and the SATP should not be confused with the standard state commonly used in thermodynamic evaluations of the Gibbs free energy of a reaction.

Standard conditions for gases: Temperature, 273.15 K and pressure of 105 pascals. The previous standard absolute pressure of 1 atm (equivalent to 1.01325 × 105 Pa) was changed to 100 kPa in 1982. IUPAC recommends that the former pressure should be discontinued.

NIST uses a temperature of 20 °C (293.15 K, 68 °F) and an absolute pressure of 101.325 kPa (14.696 psi, 1 atm). The International Standard Metric Conditions for natural gas and similar fluids are 288.15 K (59.00 °F, 15.00 °C) and 101.325 kPa.

Mountain tops
"The Canada-France-Hawaii Telescope (CFHT) is a 3.6 m optical-infrared telescope located on the summit of Mauna Kea on the island of Hawaii."

Ancient history
The ancient history period dates from around 8,000 to 3,000 b2k.

Ancient astronomers were able to differentiate between stars and planets, as stars remain relatively fixed over the centuries while planets will move an appreciable amount during a comparatively short time.

Mathematics
Ions accelerating past each other at relativistic speeds generate synchrotron radiation. Depending on the ion concentration, this radiation may contribute significantly to stellar spectra as may cyclotron or bremsstrahlung radiation from similar ion and electron interactions at slower speeds.

Physics
This beautiful galaxy imaged at right is tilted at an oblique angle on to our line of sight, giving a "birds-eye view" of the spiral structure.

This image combines data from the Hubble Space Telescope, the Spitzer Space Telescope, and the Galaxy Evolution Explorer (GALEX) missions. The GALEX ultraviolet data were from the far-UV portion of the spectrum (135 to 175 nanometers). The Spitzer infrared data were taken with the IRAC 4 detector (8 microns). The Hubble data were taken at the blue portion of the spectrum.

Technology
The Hubble Space Telescope (HST) is an excellent example of a radiation astronomy satellite designed for more than one purpose: the various astronomies of optical astronomy.

The HST is an optical astronomy telescope that incorporated a set of 48 filters isolating spectral lines of particular astrophysical interest.

The Wide Field Camera 3 (WFC3) is the Hubble Space Telescope's last and most technologically advanced instrument to take images in the visible spectrum. It was installed as a replacement for the Wide Field and Planetary Camera 2 during the first spacewalk of Space Shuttle mission STS-125 on May 14, 2009.

Hypotheses

 * 1) All known stars that give off X-rays at least from a nearby coronal cloud have nuclear fusion taking place above their photospheres.

title: Stars/Sciences


text:
Portal:French/Updates

Updates include: page creations, major renovations to pages, and project improvements.

July 7th, 2012
 * Page What is French? created.
 * Page Alphabet created.

Go To Archives

license: Creative Commons - Attribution Share-Alike - https://creativecommons.org/licenses/by-sa/4.0/

title: Portal:French/Updates


text: Talk:French/Alphabet

title: Talk:French/Alphabet


text:
French/Updates/Archives

There are currently no archived updates.

title: French/Updates/Archives


text:
French/Courses

The following is a list of all courses offered in the French Language Division divided by departments.

title: French/Courses


text: Talk:French/Courses

title: Talk:French/Courses


text: Portal:French/Staff

title: Portal:French/Staff


text:
Template:French/Contributor

Contributor template for French language course
 * parameter 1: contributor's name (as you'd like to be known here)
 * parameter 2: background (short, relevant CV; may include other Wiki activities)
 * parameter 3: contributions (to this book)
 * parameter 4: signature (automatic signature and time/date stamp)

title: Template:French/Contributor


text:
Portal:France

 * Things you can do}}

Other Wikimedia and Wikiportals

Parent portals: Europe | European Union

Related portals: French literature | Lyon | Paris | Military history of France | New France | French language and French-speaking world

title: Portal:France


text:
Template:Browsebar

Wikiversity Portals: Arts · Biology · Chemistry · Geography · History · Law · Music · Physics and Astronomy · Science · Secondary Education · Writing Center

title: Template:Browsebar


text: Portal:France/box-header-tabs

title: Portal:France/box-header-tabs


text: Portal:France/TabsTop

title: Portal:France/TabsTop


text:
Portal:France/Tab1

| style="padding:0 .3em; background-color:; border:1px solid #ef4135; ; color: #80737C; font-weight: bold; font-size:0.9em; border-bottom:none; text-align:center;" width="32%" |
 * style="background-color:#f8fcff; border-bottom:none" width="2%" |

title: Portal:France/Tab1


text:
Portal:France/Tab2

| style="padding:0 .3em; background-color:; border:1px solid #ef4135; color: #80737C; padding: .1em; text-align: center; font-weight:bold; font-size:0.9em; border-bottom:none; text-align:center;" width="32%" |
 * style="background-color:#f8fcff; border-bottom:none" width="2%" |

title: Portal:France/Tab2


text:
Portal:France/Tab3

| style="padding:0 .3em; background-color:; border:1px solid #ef4135; color: #80737C; padding: .1em; text-align: center; font-weight:bold; font-size:0.9em; border-bottom:none; text-align:center;" width="32%" |

title: Portal:France/Tab3


text:
Portal:France/TabsBottom

|}

title: Portal:France/TabsBottom


text: Template:Featured portal

title: Template:Featured portal


text: Template:Portal other

title: Template:Portal other


text:
Portal:France/Introduction

The French Republic or France (French: République française or France) is a country whose metropolitan territory is located in Western Europe and that also comprises a collection of overseas islands and territories located in North America, the Caribbean, South America, the Indian Ocean and the Pacific Ocean. After Ukraine, France is the largest country in Europe (643,427 km² with its overseas départements). With a population of over 66 million inhabitants, France is the second most populous country in Western Europe (after Germany) and the 20th largest in the world. Paris is the most populous city in France with over 12 million people in its aire urbaine, Marseille is the second largest city with 1.7 million people, and the third is Lyon with just 1.6 million people, associated with Villeurbanne.

The French Republic is a democracy which is organised as a unitary semi-presidential republic. It has the fifth-largest economy in the world in nominal terms. Its main ideals are expressed in the Declaration of the Rights of Man and of the Citizen. France is one of the founding members of the European Union, and has the largest land area of all members. France is also a founding member of the United Nations, and a member of the G8, NATO, and the Latin Union. It is one of the five permanent members of the United Nations Security Council wielding veto power, and it is also one of eight acknowledged nuclear powers. With almost 82 million foreign tourists each year, France is the most popular international tourist destination in the world.

French is the official language of France, but each region has its own unique accent; in addition to French, there are several other languages of France traditionally spoken, although use of these languages has greatly decreased over the past two hundred years. French is also an official language in 41 countries, most of which form what is called in French la Francophonie, the community of French-speaking nations.

title: Portal:France/Introduction


text: Portal:France/box-footer

title: Portal:France/box-footer


text: Portal:France/box-header

title: Portal:France/box-header


text:
Portal:France/Featured article

An archive is viewable at Portal:France/Featured Article Archive/2024

title: Portal:France/Featured article


text:
Portal:France/Featured picture/07

 w:Pont du Gard:Pont du Gard, taken from the North Bank at the level of the water course. Photo credit: ChrisO

title: Portal:France/Featured picture/07


text: Portal:France/WikiProject

title: Portal:France/WikiProject


text:
Portal:French/Where to Start

{| cellpadding="15" cellspacing="5" style="width: 100%; background-color: inherit; margin-left: auto; margin-right: auto"
 * style="width: 15%; background-color: white; border: 0px solid Gray; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px; height: 60px;" colspan="1" |[[Image:Flag of France.svg|center|200px]]

 * style="width: 100%; background-color: #ffffff; border: 1px solid #777777; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px;" colspan="1"|

Where to start?
Are you feeling a bit overwhelmed? We can help! The French Language Division is overwhelming because it has so much to offer, which is great! But sometimes having so many resources makes it difficult figuring out where to begin. We have created this page to give you an understanding of how the French Language Division works and what it has to offer you. If you are still confused after this guide we have included people who you can contact for further help. Our community is warm and welcoming and we look forward to getting to know you. {| cellpadding="10" cellspacing="5" style="width: 100%; background-color: inherit; margin-left: auto; margin-right: auto" |
 * }

 * style="width: 60%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px;" rowspan="2" |
 * style="width: 60%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px;" rowspan="2" |

French Language Division Guide

 * Learning Links: Topic:French/Learn French

 * style="width: 50%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px;" |

Helpful Links

 * Courses
 * Colloquium
 * Frequently Asked Questions
 * Help
 * Resources
 * Staff Members
 * style="width: 40%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px; height: 200px;" |
 * style="width: 40%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px; height: 200px;" |
 * style="width: 40%; background-color: ffffff; border: 1px solid Gray; vertical-align: top; -moz-border-radius-topleft: 8px; -moz-border-radius-bottomleft: 8px; -moz-border-radius-topright: 8px; -moz-border-radius-bottomright: 8px; height: 200px;" |

Staff Members You Can Contact
The following is a list of staff members who are extremely active in the French Language Division. If you have any questions or need help with something, ask one of them, and they will get back to you promptly.

 * Hérisson grognon (discuss)
 * Readyokaygo (inactive since 2013)

Also, it never hurts to check out this page's (or any page's) Talk Page as people often participate in conversation on various issues there.
 * }

title: Portal:French/Where to Start


text: Topic talk:French/Where to Start

title: Topic talk:French/Where to Start


text:
Portal:French/What is French

French (le français or la langue française ) is today spoken around the world by 72 to 130 million people as a native language, and by about 190 to 600 million people as a second or third language, with significant speakers in 54 countries. Most native speakers of the language live in France, where the language originated. The rest live in Canada, Belgium, Switzerland and Lebanon. It is an official language in 31 countries, most of which form what is called in French "La Francophonie": the community of French-speaking nations. It is an official language of all United Nations agencies and a large number of international organizations.

French is a descendant of the Latin language, whose development was influenced by the native Celtic languages of Roman Gaul and by the Germanic language of the post-Roman Frankish invaders. Some might say that Latin is a "dead language", but unlike the endangered languages of today, Latin never even faced extinction. It was the commonly spoken language throughout the Roman Empire, and during the Empires decline, and after it's fragmentation in the fifth century, varieties, or dialects, began to diverge within each local area at an accelerated rate, evolving into similar, but different languages which we now know as the Romantic or Romance languages; not called so because speaking it makes you enthralled with love and romance, but because of it's origins with Rome (though the modern sense of the word "romance" does come from the same origin). It's difficult to determine the number of contemporary Romance languages in existence, but the largest by number of native speakers are Spanish (385 million), Portuguese (210 million), French (75 million), Italian (60 million), and Romanian (23 million) (Numbers from 2007 the five most widely spoken Romance languages by number of native speakers) . Many of these languages also have large numbers of non-native speakers; this is especially the case for French, in widespread use throughout the Maghreb, Central and West Africa and Madagascar.

Why learn French?
France is considered by many to be the cosmopolitan center of the world. The French people have contributed substantially to art, literature, music, architecture, fashion, political thought, and film. Learning French allows you to access the rich culture and history of the French people.

In addition to access to France, French is an international language and the only language other than English that is spoken on five continents. It is the second most commonly taught language in the world, after English, and the official language of thirty nations. It is a working language of the United Nations, UNESCO, NATO, Organization for Economic Cooperation and Development, the International Labor Bureau, the International Olympic Committee, the International Red Cross, and many others. Learning French will give you the ability to communicate with people across the world.

Jobs Using French

 * The French-speaking world accounts for approximately 19% of all global trade.
 * France has the 5th largest economy in the world.
 * There are over 900,000 French-speaking teachers worldwide.
 * French is the 3rd most widely used language on the internet.
 * TV5MONDE is the 3rd largest international television market and is broadcast in 202 nations.

title: Portal:French/What is French


text:
Portal:French/Help

{| cellspacing="0" cellpadding="0" style="margin:0em 0em 1em 0em; width:100%" French Language Division Help Contents
 * style="width:50%; vertical-align:top; border:1px solid Black; background-color:#faf6ed;" |

 * style="padding:0em 0.5em 0em 0.5em;" |

Wikiversity Help Contents
 * style="width:50%; vertical-align:top; border:1px solid Black; background-color:#f1f5fc;" |

Editors' help
Beginners' information:

 * Sandbox (for experimenting)
 * Introduction
 * Getting involved, History of Wikiversity, The Wikiversity community, Who are Wikiversity participants?
 * Frequently asked questions, Browsing Wikiversity, Category System, Namespaces

Software helpful for Wikiversity:

 * Media playback help

 * Software and tutorials for editing media files
 * Media Help

Copyright Information:

 * Code of Conduct, discrimination policy , Image Licensing policy
 * OTRS can be reached through email at info-en@ wikimedia.org for copyright and licensing matters

Learning content:

 * Learning resources, Learning projects, Learning model, Resources by completion status

Template creation:

 * Colors, Pretty boxes, Icons, Style Sheet 1, Style Sheet 2, eMail for Teachers,

 * Quiz-Simple, Quiz, CSS at Wikiversity, Table  , Table 2,  List, Formula, Syndication

 * HTML in wikitext, Variable, Wiki markup examples, Wikitext quick reference

Wikiversity templates:

 * Using Wikiversity, Administering Wikiversity, Learning innovation

Community Pages
Basic pages:

 * Main page, Welcome page,  Community Portal, Community News,  Colloquium

Maintenance pages:

 * Administrators votes and overview, Deletion requests, Changing Username

Legal information and contact

 * Contact us, Press kit, Privacy policy, GNU Free Documentation License
 * }

title: Portal:French/Help


text: Topic talk:French/Help

title: Topic talk:French/Help


text:
Portal:French/FAQ

Read below to explore some questions and answers about the French Language Division.

title: Portal:French/FAQ


text: Topic talk:French/FAQ

title: Topic talk:French/FAQ


text: Portal:French/Colloquium

title: Portal:French/Colloquium


text:
Template:French/Colloquium

__NEWSECTIONLINK__

[ Purge Cache] - Colloquium Archives

title: Template:French/Colloquium


text: Template talk:French/Colloquium

title: Template talk:French/Colloquium


text: Template:Infobox language

title: Template:Infobox language


text: Template:Infobox language/genetic

title: Template:Infobox language/genetic


text: Template:Infobox language/linguistlist

title: Template:Infobox language/linguistlist


text: Template:Infobox language/ref

title: Template:Infobox language/ref


text: Template:Collapsible list

title: Template:Collapsible list


text:
Template:Infobox language/IPA notice

 * colspan=3 class="boilerplate metadata" style="line-height: 10pt; padding: 0.5em" | This page contains IPA phonetic symbols in Unicode.  Without proper rendering support, you may see question marks, boxes, or other symbols instead of Unicode characters.
 * colspan=3 class="boilerplate metadata" style="line-height: 10pt; padding: 0.5em" | This page contains IPA phonetic symbols in Unicode.  Without proper rendering support, you may see question marks, boxes, or other symbols instead of Unicode characters.

title: Template:Infobox language/IPA notice


title: Template:Ethnologue16


text: Template:Flag

title: Template:Flag


text: Template:Flagicon

title: Template:Flagicon


text: Template:Flagicon/core

title: Template:Flagicon/core


text: Template:Infobox language/family-color

title: Template:Infobox language/family-color


text: Template:Str number/trim

title: Template:Str number/trim


text: Template:Str number

title: Template:Str number


text: Template:Str number/logic

title: Template:Str number/logic


text:
Topic talk:French/What is French

Here is sometimes a brilliantly
Here is sometimes a brilliantly mobile full review of in what way little come plants systematically contain them

title: Topic talk:French/What is French


text: Template:Country data France

title: Template:Country data France


text:
Template:Country showdata

{{documentation|content= is an internal data container not intended to be transcluded directly. It is used indirectly by templates such as,  , and others.

{{ombox|text=This template is within the scope of WikiProject Flag Template, a collaborative effort to maintain flag templates on Wikipedia. A more thorough discussion of the flag template system, including parameters not described here, can be found on the project page.}}

Standard parameters
Main article name

Image name (File:, shown on right) {{#if: {{{var1|{{{flag alias-naval|}}}}}} |

Flag variants
   }} }} {{#if: {{{flag alias-naval|}}}{{{link alias-naval|}}}{{{flag alias-air force|}}}{{{link alias-air force|}}}{{{flag alias-army|}}}{{{link alias-army|}}} |

Military ensigns
}} {{#if: {{{redir1|}}} |

Redirect aliases
This template can also be used via an alias name (implemented as a redirect to this template): ( [ view] )   undefined   undefined  }} See [ What links here] for a full list of redirects. }}

Example usage
{{#if: {{{var1|}}} |
 * → undefined

Using a flag variant
}} {{#if: {{{redir1|}}} |
 * → undefined

Using a redirect alias
}} {{#if: {{{related1|}}} |
 * → undefined
 * → undefined
 * → undefined

Related templates
Please see the following related  templates: {{#ifexist:{{FULLPAGENAME}}/doc | {{#if:{{Suppress categories|{{{{FULLPAGENAME}}/doc}}}}|
 * Template:Country data  undefined }}

Other information
}}

}}

TemplateData
{ "description": "This template should not be used directly. It is used indirectly by flag templates such as Template:Flag and Template:Flagicon. See Category:Flag template system for a full list of flag templates and Wikipedia:WikiProject Flag Template for further documentation.", "params": {} }

Please after making any changes to this template. }}
 * link box=This is the documentation for Template:. It is automatically generated by Template:Country showdata.

title: Template:Country showdata


text:
Template:Flag/core

|

title: Template:Flag/core


text: Template:Country data Lebanon

title: Template:Country data Lebanon


text: Template:Flagcountry

title: Template:Flagcountry


text:
Template:Flagcountry/core

  |

title: Template:Flagcountry/core


text: Template:Navy

title: Template:Navy


text: Template:Navy (color)

title: Template:Navy (color)


text: File:Nils überschreitet eine Brücke.jpeg


text:
Template:Navy/core

es:Plantilla:Banderanavalpaís

title: Template:Navy/core


text: Template:IPA-fr

title: Template:IPA-fr


text: Template:IPA audio link

title: Template:IPA audio link


text: Template:Pp-semi-indef

title: Template:Pp-semi-indef


text: Template:IPA-en

title: Template:IPA-en


text:
Category:IPA templates

Formatting templates for text in the International Phonetic Alphabet.

bg:Категория:IPA шаблони bn:বিষয়শ্রেণী:আইপিএ টেমপ্লেট da:Kategori:IPA-skabeloner efter sprog eo:Kategorio:IFA ŝablonoj fa:رده:الگوهای آوا id:Kategori:Templat IPA jv:Kategori:IPA templates mk:Категорија:Шаблони за МФА ms:Kategori:Templat IPA ro:Categorie:Formate IPA se:Category:IPA-mállet simple:Category:IPA templates sh:Kategorija:IPA Šabloni tr:Kategori:IPA şablonları ur:زمرہ:باابجدیہ سانچے zh:Category:IPA模板

title: Category:IPA templates


text:
Category:User simple-2

Users in this category indicate they have skill level 2 for language Simple English.

title: Category:User simple-2


text:
User:Seti6908

de:Benutzer:Seti6908

title: User:Seti6908


text:
User:Planotse

x

title: User:Planotse


text:
User:Planotse/Top

Attention new Wikiversity users! You can Click here for details.

title: User:Planotse/Top


text: User:Planotse/Welcome

title: User:Planotse/Welcome


text:
User:Planotse/Nav

Leave Tony a message

[mailto:tonysoftwareengineer@gmail.com Send Tony an email]

Learn more about Tony

Personal Toolbox

Personal projects

title: User:Planotse/Nav


text: User:Planotse/Showcase

title: User:Planotse/Showcase


text:
Template:Usermenulikeplanotse

My Sandbox My Notepad   My Showcase

title: Template:Usermenulikeplanotse


text: User:Planotse/Tools

title: User:Planotse/Tools


text: User:Planotse/Tools/Nav

title: User:Planotse/Tools/Nav


text:
User:Planotse/Tools/Nav/SampleTextBoxes

Sample Text Boxes
Green Pointer

Yellow Note

Yellow Warning

title: User:Planotse/Tools/Nav/SampleTextBoxes


text:
User:Planotse/Projects

Project 1

 * Basic Tutorials

Project 2
http://en.wikiversity.org/wiki/Special:Random

Project 3

 * Project 3
 * is part of
 * my project set.

title: User:Planotse/Projects


text:
User:Planotse/Projects/CurrentProject

Current Project

 * Setting up the user page here

title: User:Planotse/Projects/CurrentProject


text:
User:Planotse/Tools/Nav/SampleIcons

Samples
Icons by Subject

Interesting user pages

title: User:Planotse/Tools/Nav/SampleIcons


text: User:Planotse/Notepad

title: User:Planotse/Notepad


text:
User:Planotse/Showcase/BottomMenu

Top Note Project Edit

title: User:Planotse/Showcase/BottomMenu


text:
User:Planotse/Showcase/Contributions

My Contributions

 * (coming soon)

title: User:Planotse/Showcase/Contributions


text:
User:Planotse/Showcase/Services

My services

 * (coming soon)

Current Activities

 * Wikiverscript

title: User:Planotse/Showcase/Services


text: User:Planotse/Sandbox

title: User:Planotse/Sandbox


text: User:Planotse/Userboxes

title: User:Planotse/Userboxes


text: Template:User American English

title: Template:User American English


text: Template:User Texas

title: Template:User Texas


text: Template:User language/en

title: Template:User language/en


text: Template:User language/vi

title: Template:User language/vi


text: Template:User language/de

title: Template:User language/de


text: Template:User facebook

title: Template:User facebook


text:
Gunnison, Colorado

This is an School Project. Gunnison, Colorado, U.S.A.

Gunnison, Colorado on Wikiversity
This page is intended as a Learning resource for Gunnison, Colorado, U.S.A.
 * Public Library in Gunnison, Colorado, U.S.A.
 * Leslie Savage Library of Western State College at Gunnison, Colorado, U.S.A.
 * Colorado Historic Newspapers, Colorado State Library and Colorado Historic Society

/Default/Skins/Colorado/Client.asp?Skin=Colorado&AW=1341185526089&AppName=2

This page is primarily interested in Education resource for Gunnison, Colorado, U.S.A.
 * Colorado Department of Education
 * Western State College in Gunnison, Colorado, U.S.A.
 * Gunnison Watershed RJ1E School District in Gunnison, Colorado, U.S.A.
 * Public Schools in Gunnison, Colorado, U.S.A.
 * Non Public Schools in Gunnison, Colorado, U.S.A.

This page is collectively seeking information on Geology resource in Gunnison, Colorado, U.S.A.
 * U.S.D.S. Soil Survey Gunnison
 * Uranium in Gunnison and Saguache Counties.
 * Pre-Cambrian artifacts in Gunnison, Colorado, U.S.A.
 * Gunnison River Valley, Gunnison Basin, Gunnison National Forest, Gunnison Wilderness

This page looks forward to Cartographic resource pertaining to Gunnison, Colorado, U.S.A.
 * John Williams Gunnison surveys

This page pursues History resource related to Gunnison, Colorado, U.S.A.
 * Denver & Rio Grande in Gunnison, Colorado, U.S.A.
 * Hisorical Societies in Gunnison, Colorado, U.S.A.

This page reserves space for Future resource from Gunnison, Colorado, U.S.A.
 * Gunnison County, Colorado, U.S.A.
 * City of Gunnison Planning Commission, Chamber of Commerce, Home Rule (governance)

Annotations

title: Gunnison, Colorado


text: Template:User gmail

title: Template:User gmail


text: Template:User yim

title: Template:User yim


text: Template:User skype

title: Template:User skype


text: Template:User twitter

title: Template:User twitter


text: Template:User BS

title: Template:User BS


text: Template:User wordpress

title: Template:User wordpress


text: Template:Programming language

title: Template:Programming language


text:
Template:Programming language/category

This template categorizes users based on the standard programming language system, but does not display a box. This is intended for users who don't like language boxes, or who prefer to use custom code. For example: will categorize the page where the box appears under  without displaying the c-1 box.

The opposite effect (displaying the language box without categorizing the user page) is achieved by specifying  in the Programming language call. For example: will display the c-1 box without categorizing the page where the box appears.

title: Template:Programming language/category


text:
Wikiversity:Userboxes/Programming

Placing the userbox template on your user page automatically lists you in the category system under the corresponding category so that other users may find you based on your skills. See below for details on the template's use as well as a list of the languages supported.

You can place a box around all your userboxes by putting above them and  below them, though the programming userboxes will automatically float to the right side of the page by default and need no box to enclose them.

Usage
Copy and paste the example code above, and replace "c" with the desired language's code and "4" with one of the following characters representing your proficiency level:

Customizing format
It is possible to customize the behavior and appearance of the template with the following override parameters (for example, ).

Languages supported
Below are the languages supported by the userbox template along with their codes.
 * ActionScript -  acsct
 * Ada -  ada
 * AppleScript -  apsct
 * ASP -  asp
 * Assembly -  asm
 * Bash -  bash
 * Batch -  batch
 * BASIC -  basic
 * Bourne Shell Script -  bsh
 * C -  c
 * C++ -  c++
 * C# -  csharp
 * COBOL -  cobol
 * ColdFusion -  coldf
 * CSS -  css
 * Erlang -  erlang
 * Forth -  fth
 * Fortran -  for
 * HTML -  html
 * Haskell -  hs
 * Java -  java
 * JavaScript -  js
 * LaTeX -  latex
 * Lisp -  lisp
 * Lua -  lua
 * Mathematica -  math
 * MySQL -  mysql
 * Objective-C -  objc
 * Objective Caml -  ocaml
 * Pascal -  pas
 * Perl -  perl
 * PHP -  php
 * Prolog -  pro
 * Python -  py
 * REXX -  rexx
 * Ruby -  ruby
 * Scheme -  sch
 * SQL -  sql
 * Tcl -  tcl
 * VBScript -  vbs
 * Visual Basic -  vb
 * Visual Basic .NET -  vbn
 * XHTML -  xhtml
 * XML -  xml
 * XQuery -  xquery

title: Wikiversity:Userboxes/Programming


text:
Template:Use the template Userpagelikeplanotse to set up your user page in a hurry

Hello, I'm and my username is. You can use the template Userpagelikeplanotse to set up your user page in a hurry. Detail instruction is provided here on this page.


text:
User:Planotse/How to Write a Wikibook and How to Use Wikibooks

Getting Started with Wikiversity
If you're a casual reader of Wikiversity, there is plenty of guidance on Wikiversity for you here on this page. This text, How to Write a Wikibook and How to Use Wikiversity, is my personal help for those who want to do some serious writing on Wikiversity without struggling so much with all the technicalities here at the site.

Hello, my name is Tony. I work as a Software Engineer and I live in Plano, Texas. The TSE in my user name stands for Tony - Software Engineer. You might have guessed it right, outside of my professional hours, which include time to raise my son, I spend time with Wikiversity. Whenever you have the urge to contact me, never hesitate. This page has several handy contact links for your use.

Step A. Set up your user page
Back to work, the first thing I want to show you how to do is to quickly create the content for your user page. For the purpose of this discussion, let's consider your user name as Stefalyn and your user page is User:Stefalyn. For my text, instead of using your page at User:Stefalyn, I use this page. Go there, edit that page and you should see the following line. Copy the entire line over to your own, real user page and replace Stefalyn with your own, real user name. Do not include any space. All is case sensitive!

Userpagelikeplanotse is the name of a wiki template. The result should be three red links similar to what you see here:
 * User:Stefalyn/Nav
 * User:Stefalyn/Showcase
 * User:Stefalyn/Userboxes

Step B. Set up your navigation bar
Click on the first red link, User:Stefalyn/Nav, then enter the following text but use your own user name, nickname and email address.

Step C. Set up your showcase
Click on the second red link, e.g. User:Stefalyn/Showcase, then enter the following lines or use your own imagination:  === Attention People ===  This is my showcase.  === Another Shelf ===  This is another shelf in my showcase.

Step D. Set up your userboxes
Click on the third red link, e.g. User:Stefalyn/Userboxes, then enter the following text, but delete any line not applicable to you. For more choices, see Userboxes.  === Attention People ===

Step E. How to delete a page in your work
Don't try this at home, or on your user page. You cannot on your own delete a page in your work but you can following this procedure to have this done for you:
 * Please delete my page

Step F. Help other users
You can help other users to do the same. All you have to do is click on the Discussion link on their user page, click on the Add Topic link near the top right corner, then paste the following text string in your message to them. You must include all four curly brackets as shown:

Step G. Boxing
In your text, by placing a blank space at the start of a short phrase, you put that phrase in a box. You can combine as many such lines as you want. What you see here is the result of doing so three times in a row.

Article message box is another way. If you write in your article the following text: You will get the following result: For more information on how to use this style of text boxing, see Template:Ambox.

Step H. Create a Notepad and a Sandbox
A notepad is where you can save your notes. Remember, all writing, including your own notes are public. There is absolutely no privacy here! A sandbox is like a notepad but its purpose is to experiment with some writing or even scripting. Do the following steps to create your notepad and sandbox:
 * 1) Go to your user page
 * 2) Append "/Notepad" behind your user page's URL then press enter to create a notepad page, e.g. User:Planotse/Notepad.
 * 3) Do the same, append "/Sandbox" behind your user page's URL then press enter to create a sandbox page, e.g. User:Planotse/Sandbox.

Step I. TBD
This topic is intentionally left blank.

Step J. Create an easy access to your pages
By now you should have created the following pages but with your own username, not mine: You can create a personal menu for easy access to your pages, in two different ways, either J1 or J2.
 * http://en.Wikiversity.org/wiki/User:Planotse/Notepad
 * http://en.Wikiversity.org/wiki/User:Planotse/Sandbox

Alternative Step J1. Create a menu based on an existing template
If you do not want to deal with scripting, go to your showcase page, e.g. User:Planotse/Showcase, then enter the following line of text. Save the page then go back to your main user page and see the result.

Alternative Step J2. Create a menu based on your own code
If J1 does not work or you do not like the result from J1, use the following code at the top of you showcase page. Replace my Planotse with your own user name. Change the captions Sand, Note and Show to whatever you want. Sand &nbsp; Note &nbsp; Show

Step K. Review what you've done so far
Showing you how to create a user page similar to mine is a way to show you how to get started in writing on Wikiversity. Below is a list of concepts you've touched so far:
 * User Page
 * Wiki Template
 * Text Headers
 * Subjects & Categories
 * Notepad & Sandbox
 * Wiki-style Menu Links

Making a Smarter User Page
Learning how to make a smarter user page is a way to learn how to write a better wikibook. The prior section shows you how to get started with Wikiversity by quickly creating a basic user page. Now I show you how to turn your user page into a personal writing toolbox.

Step L. TBD
This topic is intentionally left blank.


text:
Template:Navlikeplanotse

Leave a message

[mailto: Send an email]

Personal Toolbox

title: Template:Navlikeplanotse


text: Template:Userpagelikeplanotse

title: Template:Userpagelikeplanotse


text: Template:Userpagelikeplanotsego

title: Template:Userpagelikeplanotsego


text: Template:Country data Belgium

title: Template:Country data Belgium


text: Template:Country data Canada

title: Template:Country data Canada


text:
Template:Country data Haiti

af:Sjabloon:Landdata Haïti sl:Predloga:Podatki države Haiti

title: Template:Country data Haiti


text:
Template:Country data Madagascar

sl:Predloga:Podatki države Madagaskar

title: Template:Country data Madagascar


text:
Template:Country data Azawad

id:Templat:Country data Azawad ja:Template:Country data Azawad ka:თარგი:ქვეყნის მონაცემები აზავადი ko:틀:나라자료 아자와드 mk:Шаблон:Country data Азавад pt:Predefinição:Country data Azauade ro:Format:Country data Azawad

title: Template:Country data Azawad


text: Template:Country data Benin

title: Template:Country data Benin


text: Template:Country data Burkina Faso

title: Template:Country data Burkina Faso


text: Template:Country data Burundi

title: Template:Country data Burundi


text: Template:Country data Cameroon

title: Template:Country data Cameroon


text: Template:Country data Central African Republic


text: Template:Country data Chad

title: Template:Country data Chad


text: Template:Country data Comoros

title: Template:Country data Comoros


text:
Template:Country data Côte d'Ivoire

Country data Côte d&

title: Template:Country data Côte d'Ivoire


text: Template:Country data Democratic Republic of the Congo


text: Template:Country data Djibouti

title: Template:Country data Djibouti


text: Template:Country data Equatorial Guinea

title: Template:Country data Equatorial Guinea


text: Template:Country data Gabon

title: Template:Country data Gabon


text: Template:Country data Guinea

title: Template:Country data Guinea


text: Template:Country data Luxembourg

title: Template:Country data Luxembourg


text:
Template:Country data Mali

sl:Predloga:Podatki države Mali

title: Template:Country data Mali


text:
Template:Country data Monaco

sl:Predloga:Podatki države Monako

title: Template:Country data Monaco


text: Template:Country data Niger

title: Template:Country data Niger


text: Template:Country data Republic of the Congo


text: Template:Country data Rwanda

title: Template:Country data Rwanda


text: Template:Country data Senegal

title: Template:Country data Senegal


text: Template:Country data Seychelles

title: Template:Country data Seychelles


text:
Template:Country data Switzerland

ml:ഫലകം:Country data Switzerland sl:Predloga:Podatki države Švica

title: Template:Country data Switzerland


text:
Template:Country data Togo

sl:Predloga:Podatki države Togo

title: Template:Country data Togo


text: Template:Country data Vanuatu

title: Template:Country data Vanuatu


text:
Template:Country data Algeria

sl:Predloga:Podatki države Alžirija

title: Template:Country data Algeria


text:
Template:Country data Morocco

sl:Predloga:Podatki države Maroko

title: Template:Country data Morocco


text: Template:Country data Mauritius

title: Template:Country data Mauritius


text: Template:Country data Mauritania

title: Template:Country data Mauritania


text:
Template:Country data Tunisia

sl:Predloga:Podatki države Tunizija

title: Template:Country data Tunisia


text:
Template:Country data Aosta Valley

bn:টেমপ্লেট:Country data Aosta Valley fa:الگو:Country data Aosta Valley pt:Predefinição:Country data Aosta Valley simple:Template:Country data Aosta Valley

title: Template:Country data Aosta Valley


text:
Template:Country data French Southern and Antarctic Lands

ar:قالب:معطيات أراضي فرنسية جنوبية وأنتارتيكية da:Skabelon:Lande data Franske Sydterritorier es:Plantilla:Geodatos Tierras Australes y Antárticas Francesas eu:Txantiloi:Herrialde info Frantziaren lurralde austral eta antartikoak fa:الگو:Country data French Southern and Antarctic Lands id:Templat:Country data Daratan Selatan dan Antarktika Perancis mk:Шаблон:Country data Француски јужни и антарктички територии arz:قالب:Country data French Southern and Antarctic Lands ja:Template:Country data French Southern and Antarctic Lands pt:Predefinição:Country data Terras Austrais e Antárticas Francesas ro:Format:Country data Teritoriile australe și antarctice franceze simple:Template:Country data French Southern and Antarctic Lands sv:Mall:Landsdata Franska sydterritorierna ur:سانچہ:معطیات اراضی فرانسیسی جنوبی اور انٹارکٹیکا vi:Bản mẫu:Country data French Southern and Antarctic Lands war:Batakan:Country data French Southern and Antarctic Lands zh:Template:Country data French Southern and Antarctic Lands


text: Template:Country data French Polynesia

title: Template:Country data French Polynesia


text: Template:Country data Guernsey

title: Template:Country data Guernsey


text: Template:Country data Jersey

title: Template:Country data Jersey


text: Template:Country data Louisiana

title: Template:Country data Louisiana


text: Template:Country data United States

title: Template:Country data United States


text:
Template:Country data Mayotte

sl:Predloga:Podatki države Mayotte

title: Template:Country data Mayotte


text: Template:Country data New Caledonia

title: Template:Country data New Caledonia


text:
Template:Country data India

af:Sjabloon:Landdata Indië sl:Predloga:Podatki države Indija ta:வார்ப்புரு:நாட்டுத் தகவல் இந்தியா

title: Template:Country data India


text: Template:Country data Saint Barthélemy

title: Template:Country data Saint Barthélemy


text: Template:Country data Saint Martin

title: Template:Country data Saint Martin


text:
Template:Country data Saint Pierre and Miquelon

sl:Predloga:Podatki države Saint Pierre in Miquelon


text: Template:Country data Wallis and Futuna

title: Template:Country data Wallis and Futuna


text:
Category:Blog posts by Samwilson

This category contains all posts in User:Samwilson's blog.

title: Category:Blog posts by Samwilson


text:
User:Planotse/Tools/Nav/TestAreas

Test Areas
Tony's sandbox on Wikibooks

Creating a new toolbar

Showcase on the user page

title: User:Planotse/Tools/Nav/TestAreas


text:
User:Planotse/Tools/Nav/NewTools

New Tools

 * Help:Magic words
 * MediaWiki ParserFunctions
 * Nuvola Icons
 * Parser Functions

title: User:Planotse/Tools/Nav/NewTools


text:
User:Planotse/Sandbox/Test1

function outputTable( columns, table ) { append "{| class='wikitable'\n"; for( name : title in columns ) { append "! " + title + "\n"; }

for( row in table ) { append "|-\n"; for( name : title in columns ) { append "| " + row[name] + "\n"; } }

append "|}\n"; }

function getHeaders { return { "a" : "A's", "b" : "B's", "c" : "C's" }; }

function getTable { yield { "c" : 42, "b" : 22, "a" : 33 }; yield { "c" : 10, "b" : 21, "a" : 31 }; yield { "a" : "abc", "b" : "def", "c" : "ghi" }; yield { "b" : "Hello, world!", "a" : "Lol wut?", "c" : "Testing 12345" }; }

function main( a, b, c ) { return self::outputTable(   self::getHeaders,    self::getTable + { "a" : a, "b" : b, "c" : c }; }

title: User:Planotse/Sandbox/Test1


text: User:Planotse/Wikiverscript

title: User:Planotse/Wikiverscript


text: Template:Navigate

title: Template:Navigate


text: Template:FULLCHAPTERNAME

title: Template:FULLCHAPTERNAME


text:
Template:Book Search

fr:Modèle:Moteur

title: Template:Book Search


text:
User:Planotse/Wikiverscript/Cover Page

Project Documentation

title: User:Planotse/Wikiverscript/Cover Page


text: User:Planotse/Wikiverscript/Dedication

title: User:Planotse/Wikiverscript/Dedication


text: User:Planotse/Wikiverscript/How to Turn the Page


text:
User:Planotse/Wikiverscript/Table of Contents

Front Matter

 * Project Summary
 * Cover Page
 * Problem Statement
 * Table of Contents
 * Dedication
 * How to Turn the Page

General Process

 * Topic 1
 * Topic 2
 * Topic 3

Specific Procedures

 * Topic 1
 * Topic 2
 * Topic 3

Reference Materials

 * Topic 1
 * Topic 2
 * Topic 3

Back Matter

 * Glossary


text: User:Planotse/Wikiverscript/Introduction


text:
User:Planotse/Wikiverscript/Problem Statement

Problem Statement
For example, in creating a template, students and teachers should not struggle with something like this:

Instead, they should be able to work with something like this: ifempty arg1 then arg3 else arg2

The ultimate goal for the Wikiverscript is to help students, teachers spend more time with the learning, teaching here at Wikiversity and less time with the learning curve.

Proposed Activities
How to get started


title: File:SBF.1.A.Aperture.20120702.pdf


title: File:BGND.5.A.MPI.20120702.pdf


text: Template:Templates:French/box-header

title: Template:Templates:French/box-header


text: Template:Templates:French/boxheader/box-footer


text: Template:French/boxheader/box-footer

title: Template:French/boxheader/box-footer


text: Template:French/box-header

title: Template:French/box-header


text: File:Sampling.6.B.Prefilter.20120702.pdf


text: File:Sampling.7.B.Postfilter.20120702.pdf


text:
Template:Wayback

__NONEWSECTIONLINK__

title: Template:Wayback


text:
Moment distribution

Moment distribution method was developed by Hardy Cross to solve the problems of Indeterminate Structures. In this method all the joints are considered locked (restrained) in the beginning and the fixed end moments are determined at each joint. The stiffness coefficients are calculated which in turn determine the distribution factors for different members connected at a joint.
 * The next step is to release the locked joint and allow it to rotate (if not fixed in reality) and distribute that fixed-end-moment to the members connected at that joint in the proportion of distribution factors; this step is known as balancing of joint. This process continues till all the joints are balanced. When we unlock and joint and apply the balancing moment at that joint half of the moment will be developed at the far end which is known as carry-over moment. These cycle of balancing and carry-over continue till a desired accuracy is achieved at all the joint. This can be easily understood with the help of solved example

title: Moment distribution


text: File:Nils und eine Freundin.jpeg

title: File:Nils und eine Freundin.jpeg


text:
User talk:Yanick

Copyright problems on photos
Hello. There is a problem with one or more files you have uploaded. Every file you upload must have a clear statement of the copyright position. If you took the photos yourself, add PD-self if you are placing it unreservedly in the public domain. If you wish to retain minimal rights, add Cc-by-sa-3.0. If you did not take the photo, please add an explanation of why it can be hosted here. I am afraid that if you do not do this, the file wil be deleted. Let me know if you have any problems.--Collingwood (talk) 12:01, 2 July 2012 (UTC)

title: User talk:Yanick


text:
User talk:Dablee

Copyright problems on photos
Hello. There is a problem with one or more files you have uploaded. Every file you upload must have a clear statement of the copyright position. If you took the photos yourself, add PD-self if you are placing it unreservedly in the public domain. If you wish to retain minimal rights, add Cc-by-sa-3.0. If you did not take the photo, please add an explanation of why it can be hosted here. I am afraid that if you do not do this, the file wil be deleted. Let me know if you have any problems.--Collingwood (talk) 12:04, 2 July 2012 (UTC)

title: User talk:Dablee


text:
User talk:Tlaw627

Copyright problems on photos
Hello. There is a problem with one or more files you have uploaded. Every file you upload must have a clear statement of the copyright position. If you took the photos yourself, add PD-self if you are placing it unreservedly in the public domain. If you wish to retain minimal rights, add Cc-by-sa-3.0. If you did not take the photo, please add an explanation of why it can be hosted here. I am afraid that if you do not do this, the file wil be deleted. Let me know if you have any problems.--Collingwood (talk) 12:05, 2 July 2012 (UTC)

title: User talk:Tlaw627


text:
Topic talk:Oncology

I consider, that you are mistaken. I suggest it to discuss. Write to me in PM.

title: Topic talk:Oncology


text:
User talk:J4knee21

Copyright problems on photos
Hello. There is a problem with one or more files you have uploaded. Every file you upload must have a clear statement of the copyright position. If you took the photos yourself, add PD-self if you are placing it unreservedly in the public domain. If you wish to retain minimal rights, add Cc-by-sa-3.0. If you did not take the photo, please add an explanation of why it can be hosted here. I am afraid that if you do not do this, the file wil be deleted. Let me know if you have any problems.--Collingwood (talk) 12:05, 2 July 2012 (UTC)

title: User talk:J4knee21


text:
User talk:MundaneUser

Copyright problems on photos
Hello. There is a problem with one or more files you have uploaded. Every file you upload must have a clear statement of the copyright position. If you took the photos yourself, add PD-self if you are placing it unreservedly in the public domain. If you wish to retain minimal rights, add Cc-by-sa-3.0. If you did not take the photo, please add an explanation of why it can be hosted here. I am afraid that if you do not do this, the file wil be deleted. Let me know if you have any problems.--Collingwood (talk) 12:12, 2 July 2012 (UTC)

title: User talk:MundaneUser