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60 Aquarii

60 Aquarii is a star located 375 light years away from the Sun in the equatorial constellation of Aquarius. 60 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.89. The star is moving closer to the Earth with a heliocentric radial velocity of –8 km/s.

This is an aging giant star with a stellar classification of G6 III, most likely on the horizontal branch. It is 437 million years old with 2.77 times the mass of the Sun. Having exhausted the hydrogen at its core, this star has evolved away from the main sequence and expanded to 11 times the Sun's radius. It is radiating 65 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,820 K.

A magnitude 11.54 companion star is located at an angular separation of $11.13$ along a position angle of 299°, as of 2013.

title: 60 Aquarii


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45 Aquarii

45 Aquarii is a star in the zodiac constellation of Aquarius. 45 Aquarii is its Flamsteed designation. Its apparent magnitude is 5.96.

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

title: 45 Aquarii


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17 Aquarii

17 Aquarii, abbreviated 17 Aqr, is a spectroscopic binary star system in the constellation of Aquarius. 17 Aquarii is the Flamsteed designation. It appears to the naked eye as a faint sixth magnitude star, having a combined apparent visual magnitude of 5.99. The distance to 17 Aqr can be estimated from its annual parallax shift of $1.516$, which yields a separation of around 660 light years. It is moving further away with a heliocentric radial velocity of 18 km/s.

A preliminary orbit for the pair gives a period of 7290 days and an eccentricity of 0.4. The primary component is an aging giant star with a stellar classification of K4/5 III. It is radiating 495 times the Sun's luminosity from its photosphere at an effective temperature of 3,951 K.

title: 17 Aquarii


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39 Aquarii

39 Aquarii is a star in the zodiac constellation of Aquarius. 39 Aquarii is its Flamsteed designation. It is a faint naked eye star with an apparent visual magnitude of 6.03. Based upon an annual parallax shift of 23.78 measured with a 3% margin of error, this star is at a distance of around 137 ly from Earth. It is a double star with a magnitude 9.3 companion at an angular separation of 0.6 arcseconds along a position angle of 257°.

The stellar classification of this star is F0 V; hence it belongs to the category of F-type main sequence stars that generate energy through hydrogen fusion at the core. It is 1.8 billion years old with 1.35 times the mass of the Sun and 1.79 times the Sun's radius. The star is radiating 6.1 times the luminosity of the Sun from its photosphere at an effective temperature of 6,806 K.

title: 39 Aquarii


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59 Arietis

59 Arietis is a star in the northern constellation of Aries. 59 Arietis is the Flamsteed designation. It is dimly visible to the naked eye with an apparent visual magnitude of 5.91. Based upon an annual parallax shift of $0.86$, it is located approximately 212 ly distant from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −4.7 km/s.

The spectrum of this object is that of a subgiant star with a stellar classification of G7 IV, which would suggest it has exhausted the supply of hydrogen at its core and has begun to evolve into a giant star. It is around 1.7 billion years old with a projected rotational velocity of 1.8 km/s. The star has nearly double the mass of the Sun and almost six times the Sun's radius. It is radiating 20 times the luminosity of the Sun from its photosphere at an effective temperature of 5,044 K.

title: 59 Arietis


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49 Arietis

49 Arietis is a single star in the northern constellation of Aries. 49 Arietis is the Flamsteed designation. It is visible to the naked eye as a faint, white hued star with an apparent visual magnitude of 5.90. The star is located at a distance of about 223 ly distant from Earth based on parallax.

This object is classified as an Am star, or non-magnetic chemically peculiar star of the CP1 class, which means the spectrum displays abnormal abundances of certain heavier elements. It has a stellar classification of kA2hA6mA7, which means it has the calcium K line of an A2 class star, the hydrogen lines of an A6 star, and the metal lines of an A7 star. 49 Arietis has a moderately high rate of spin, showing a projected rotational velocity of $0.141$, and is radiating 16 times the luminosity of the Sun from its photosphere at an effective temperature of $52 km/s$.

title: 49 Arietis


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82 Aquarii

82 Aquarii is a star in the equatorial constellation of Aquarius. 82 Aquarii is its Flamsteed designation. It has an apparent visual magnitude of 6.15, which, according to the Bortle Dark-Sky Scale, means it is a faint star that requires dark rural skies to view. The annual parallax shift of 82 Aquarii is $−3.59$, which equates to a distance of roughly 890 ly from Earth. Because this star is positioned near the ecliptic, it is subject to lunar eclipses.

This object is an aging red giant star currently on the asymptotic giant branch with a stellar classification of M2 III, having exhausted both the hydrogen and helium at its core and expanded to 56 times the Sun's radius. It is a suspected variable star of unknown type that ranges in magnitude between 6.24 and 6.29. The star is radiating 693 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 3,946 K.

title: 82 Aquarii


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Basketball Australia

BA Limited, trading as Basketball Australia, is a not-for-profit company promoting basketball in Australia at all levels. It is recognised by FIBA as the national body organising international basketball in Australia.

Basketball Australia operates the Women's National Basketball League (WNBL) and the Centre of Excellence at the Australian Institute of Sport (AIS) in Canberra.

History
In 1939, the National Federation of Basketball was formed, which later became known as the Amateur Basketball Union of Australia. This body did not become fully effective until 1946, when the first Australian Championships were held. The organisation eventually changed its name to the Australian Basketball Federation. In 1949, Australia became the fifty-second affiliated member of the International Basketball Federation (FIBA). The Basketball Australia trading name was registered in 1996.

National Teams
'' Each national team and their performance at the most recent international events are listed above. ''

Leagues

 * Men

 * Women

Partnerships
Since 2018, there has been an ongoing partnership with the Japan Basketball Association.

In August 2023, Basketball Australia announced a major partnership with Ford Australia. As part of the multi-year deal, the Ford logo will feature on the jerseys of the Australia men's national basketball team and the Australia women's national basketball team.

title: Basketball Australia


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Wikipedia:Articles for deletion/The qwesi

 * The following discussion is an archived debate of the proposed deletion of the article below. Please do not modify it. Subsequent comments should be made on the appropriate discussion page (such as the article's talk page or on a Votes for Undeletion nomination).  No further edits should be made to this page.

The result of the debate was Delete Ryan Norton T 01:48, 22 October 2005 (UTC)

The qwesi
Vanity, non notable, just 352 hits, groups named there are NN as well (Her Rigormorts: 21 hits, The Studiofix: 209 hits, Volkpenis: 2 hits) -- ReyBrujo 03:16, 14 October 2005 (UTC)

 * Delete Hmm, oddly enough, I actually know the people in these bands. While I wish them well (and I think some of their songs have real potential), they aren't notable yet.  Sigh.  It's a rough day when my Wikipedian integrity wars with my sense of friendship, but hey, so it goes.  Besides, they're better off making music instead of creating articles about themselves.  Anville 10:22, 14 October 2005 (UTC)
 * Delete - nn CLW 13:20, 14 October 2005 (UTC)

 * The above discussion is preserved as an archive of the debate. Please do not modify it. Subsequent comments should be made on the appropriate discussion page (such as the article's talk page or in an undeletion request). No further edits should be made to this page.


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70 Aquarii

70 Aquarii is a variable star located 425 light years away from the Sun in the equatorial constellation of Aquarius. It has the variable star designation FM Aquarii; 70 Aquarii is the Flamsteed designation. It is near the lower limit of visibility to the naked eye, appearing as a dim, yellow-white hued star with a baseline apparent visual magnitude of 6.19. This star is moving closer to the Earth with a heliocentric radial velocity of –5.8 km/s.

This is an F-type main-sequence star with a stellar classification of F0 V. Located in the lower part of the instability strip, it is a Delta Scuti-type variable that ranges in brightness from magnitude 6.16 down to 6.19 with a period of 0.087 days. The star has a high rate of spin, showing a projected rotational velocity of 110 km/s. It has four times the Sun's radius and is radiating 45 times the luminosity of the Sun from its photosphere at an effective temperature of around 7,314 K.

title: 70 Aquarii


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78 Aquarii

78 Aquarii (abbreviated 78 Aqr) is a star in the constellation of Aquarius. 78 Aquarii is its Flamsteed designation. Based on stellar parallax measurements made by Gaia, it is located about 600 light-years (180 parsecs) from the Sun.

78 Aquarii has a spectral type of K2III, indicating a giant star with a reddish color. Its apparent magnitude is 6.18, indicating it is not visible to the sky for all but the best viewing conditions. At its surface, its temperature is estimated to be roughly 4,400 K. It has no known exoplanets.

title: 78 Aquarii


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11 Aquarii

11 Aquarii is a sun-like star in the zodiac constellation of Aquarius, located 88.5 light years away from the Sun. 11 Aquarii is the Flamsteed designation. It is difficult to see with the naked eye, appearing as a dim, yellow-hued star with an apparent visual magnitude of 6.22. This body is moving closer to the Earth with a heliocentric radial velocity of −17.8 km/s, and is expected to come as close as 19.96 pc in 700,000 years.

It is a G-type main-sequence star with a stellar classification of G1 V. Compared to the Sun, this star has a higher abundance of elements more massive than helium. This indicates it belongs to a class of stars called metal-rich. The star is slightly older than the Sun, but it has slightly more mass and has a larger radius. It is radiating 2.24 times the luminosity of the Sun from its photosphere at an effective temperature of 5,973 K.

title: 11 Aquarii


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81 Aquarii

81 Aquarii is a star in the constellation of Aquarius. It has an orange hue and is barely visible to the naked eye with an apparent visual magnitude of 6.23. 81 Aquarii is its Flamsteed designation. The star is located at a distance of approximately 451 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +1.6 km/s. It is positioned near the ecliptic and thus is subject to lunar occultations.

This is an aging giant star with a stellar classification of K5 III, indicating it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. The stellar spectrum displays strong lines of cyanogen. It presently has 18 times the radius of the Sun and is radiating 102 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,324 K.

title: 81 Aquarii


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54 Arietis

54 Arietis is a star in the northern zodiac constellation of Aries. 54 Arietis is the Flamsteed designation. It is a challenge to view with the naked eye even under good viewing conditions, having an apparent visual magnitude of 6.27. Based upon an annual parallax shift of $1.56$, it is located approximately 740 ly distant from Earth, and it is drifting further away with a radial velocity of +44 km/s. The brightness of the star is diminished by 0.15 in magnitude from extinction caused by interstellar gas and dust. The star is positioned near the ecliptic and thus is subject to lunar occultations.

This is an aging red giant star with a stellar classification of M0 III that is currently evolving along the asymptotic giant branch. Having exhausted the supply of hydrogen at its core, the star has expanded to 41 times the Sun's radius. It varies slightly in brightness, with a periodicity of 6.2 days and an amplitude change of 0.0096 in magnitude. On average it is radiating 387 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,013 K.

title: 54 Arietis


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Overlapping consensus

Overlapping consensus is a term coined by John Rawls in A Theory of Justice and developed in Political Liberalism. The term overlapping consensus refers to how supporters of different comprehensive normative doctrines—that entail apparently inconsistent conceptions of justice—can agree on particular principles of justice that underwrite a political community's basic social institutions. Comprehensive doctrines can include systems of religion, political ideology, or morality.

Rawls explains that an overlapping consensus on principles of justice can occur despite "considerable differences in citizens' conceptions of justice provided that these conceptions lead to similar political judgements." The groups are able to achieve this consensus in part by refraining from political/public disputes over fundamental (e.g. metaphysical) arguments regarding religion and philosophy. Rawls elaborates that the existence of an overlapping consensus on conceptions of justice among major social groups holding differing—yet reasonable—comprehensive doctrines is a necessary and distinctive characteristic of political liberalism. Rawls also explains that the overlapping consensus on principles of justice is itself a moral conception and is supported by moral reasoning—although the fundamental grounds of this support may differ for each of the various groups holding disparate comprehensive doctrines, and these lines of reasoning may also differ from the public reasons provided for supporting the principles. These latter features distinguish his idea of an overlapping consensus from a mere modus vivendi, which is a strategic agreement entered into for pragmatic purposes, and therefore potentially unprincipled and unstable. The overlapping consensus could in sum be said to "depend, in effect, on there being a morally significant core of commitments common to the 'reasonable' fragment of each of the main comprehensive doctrines in the community".

It has been argued that reasonable forms of religious and moral public education may be agreed by considering which common values and principles may be determined through overlapping consensus between those of otherwise incommensurable comprehensive doctrines (e.g. those of a given religion and secularists).

title: Overlapping consensus


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27 Arietis

27 Arietis is a binary star system in the northern constellation of Aries. 27 Arietis is the Flamsteed designation. It is a dim, yellow-hued star that is close to the lower limit of what can be viewed with the naked eye, having an apparent visual magnitude is 6.21. The annual parallax shift of $0.908$ corresponds to a physical distance of approximately 280 ly from Earth. It is advancing closer to the Earth with a heliocentric radial velocity of −122.7 km/s, and may come as close as 25.85 pc in around 643,000 years.

This appears to be a single-lined spectroscopic binary system with an orbital period of 130.7 days and an eccentricity of 0.366. It has an "a sin i" value of 10.00 ±, where a is the semimajor axis and i is the inclination to the line of sight from the Earth. This value provides a lower bound on the actual semimajor axis. The visible component has a stellar classification of G8 III-IV Fe-2, displaying mixed spectral traits of an evolved subgiant and a giant star, with a strong underabundance of iron. The CN bands of this star are very weak.

title: 27 Arietis


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100 Aquarii

100 Aquarii is a star in the zodiac constellation of Aquarius. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It is near the lower limit of visibility to the naked eye, appearing as a dim, yellow-white hued star with an apparent visual magnitude of 6.24. The heliocentric radial velocity is poorly constrained, but the star appears to be moving closer to the Earth at the rate of around −8 km/s.

This is an ordinary F-type main-sequence star with a stellar classification of F0 V. The star has a high rate of spin, showing a projected rotational velocity of 123 km/s. It has 1.8 times the mass of the Sun and 2.5 times the Sun's radius. The star is radiating 16 times the luminosity of the Sun from its photosphere at an effective temperature of 7,063 K.

title: 100 Aquarii


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User talk:DOLLFACED

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:18, 14 October 2005 (UTC)
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title: User talk:DOLLFACED


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60 Arietis

60 Arietis is a star in the northern constellation of Aries. 60 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 6.14, making it a challenge to view with the naked eye. Based upon an annual parallax shift of $23.85$, this star is located 341 ly away from the Sun. It is receding from the Earth with a heliocentric radial velocity of +24 km/s.

This object is an aging giant star with a stellar classification of K3 III, having exhausted the supply of hydrogen at its core and expanded to 11 times the Sun's radius. It is 5.3 billion years old with 1.36 times the mass of the Sun. The star shines with 49 times the Sun's luminosity; this energy is being radiated from the photosphere at an effective temperature of 4,449 K, giving it the orange-hued glow of a K-type star.

title: 60 Arietis


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26 Arietis

26 Arietis is a variable star in the northern constellation of Aries. 26 Arietis is the Flamsteed designation; it also bears the variable star designation UU Arietis. The apparent visual magnitude of this star is 6.14, which, according to the Bortle Dark-Sky Scale, is within the naked eye visibility limit in dark rural skies. The annual parallax shift of $2.32$ is equivalent to a distance of approximately 215 ly from Earth. The star is receding from the Earth with a heliocentric radial velocity of +15 km/s.

This is an A-type main sequence star with a stellar classification of A9 V. It is a Delta Scuti variable with a variability period of 0.0676 days and an amplitude of 0.010 in magnitude. The star is around a billion years old with 1.74 times the mass of the Sun and 2.32 times the Sun's radius. The star is radiating 15 times the luminosity of the Sun from its photosphere at an effective temperature of 7,430 K.

title: 26 Arietis


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User talk:Cynhtia Lilly

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:18, 14 October 2005 (UTC)
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title: User talk:Cynhtia Lilly


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56 Aquarii

56 Aquarii, abbreviated 56 Aqr, is a star in the constellation of Aquarius. 56 Aquarii is its Flamsteed designation. It is a sixth magnitude star, having an apparent visual magnitude of 6.36, and thus is a challenge to view with the naked eye. Based upon an annual parallax shift of $−0.047$, it is located around 643 light years from the Earth. At that distance, the visual magnitude is diminished by an extinction of 0.12 due to interstellar dust. The star is moving closer with a heliocentric radial velocity of −28 km/s. It is a candidate runaway star showing a transverse peculiar velocity of 213.87 km/s.

Houk and Smith-Moore (1978) gave this star a stellar classification of B8 II, matching a B-type bright giant. In contrast, Cowley et al. (1969) found a class of B8 Vs, corresponding to a B-type main-sequence star with narrow ("sharp") absorption lines due to a relatively low projected rotation. Zorec and Royer (2012) modeled it as a dwarf star that is 67% of the way through its main sequence lifespan. It is a chemically peculiar mercury-manganese star, showing abnormally strong absorption lines of mercury and magnesium with weak lines of helium. The star has 3.4 times the mass of the Sun and about 2.8 times the Sun's radius. It is radiating 185 times the Sun's luminosity from its photosphere at an effective temperature of 11,912 K.

title: 56 Aquarii


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53 Arietis

53 Arietis (abbreviated 53 Ari) is a variable star in the northern constellation of Aries. 53 Arietis is the Flamsteed designation; it also bears the variable star designation UW Arietis. It is a B-type main sequence star with a stellar classification of B1.5 V and mean apparent magnitude of 6.10, which is near the lower limit for naked eye visibility. Based upon an annual parallax shift of $7.5$, the estimated distance to this star is roughly 314 pc.

53 Arietis is a Beta Cephei variable. It is a runaway star with a peculiar velocity of 48.1 km/s relative to its neighbors. The star was ejected from the Orion nebula some 4–5 million years ago, possibly when an orbiting companion exploded as a supernova.

title: 53 Arietis


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User talk:Marcellus1~enwiki

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:19, 14 October 2005 (UTC)
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Your account will be renamed
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title: User talk:Marcellus1~enwiki


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20 Aquarii

20 Aquarii, abbreviated 20 Aqr, is a star in the constellation Aquarius. 20 Aquarii is the Flamsteed designation. It is a dim star with an apparent visual magnitude of 6.38. Based upon an annual parallax shift of $0.334$, it is located 213 light years away but is moving closer to the Earth with a heliocentric radial velocity of −23 km/s. The star is predicted to come to within 34.61 pc in around 1.9 million years.

This is an F-type main-sequence star with a stellar classification of F0 V. (Cowley and Fraquelli [1974] had given it a class of F0 III.) It is a suspected chemically peculiar Am star showing metallic lines. It is 761 million years old with a high projected rotational velocity of 92 km/s. The star has 1.52 times the mass of the Sun and is radiating 9 times the Sun's luminosity from its photosphere at an effective temperature of about 7,314 K.

title: 20 Aquarii


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User:Jackandjiro

Please stop adding nonsense to Wikipedia. It is considered vandalism. If you would like to experiment, use the sandbox. Thank you. Karmafist 03:19, 14 October 2005 (UTC)

title: User:Jackandjiro


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65 Arietis

65 Arietis is a star in the northern constellation of Aries, located near Tau Arietis. 65 Arietis, abbreviated '65 Ari', is the Flamsteed designation. It has an apparent visual magnitude of 6.07, which, according to the Bortle Dark-Sky Scale, means it is faintly visible to the naked eye when viewed from dark suburban skies. Based upon an annual parallax shift of $−0.028$, it is approximately 345 ly distant from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of around −6 km/s.

This is an ordinary A-type main sequence star with a stellar classification of A1 V. It has about 2.45 times the mass of the Sun and shines with 40 times the Sun's luminosity. This energy is being radiated into outer space at an effective temperature of 10.300 K, giving it the white-hued glow of an A-type star. It is roughly 23% of the way through its lifetime on the main sequence of core hydrogen burning stars.

title: 65 Arietis


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User talk:Just4jesus

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:19, 14 October 2005 (UTC)
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Regarding the 'Christine gooch' entry: Thanks for experimenting with Wikipedia. Your test worked, and has been reverted or removed. Please use the sandbox for any other tests you want to do. Take a look at the welcome page if you would like to learn more about contributing to our encyclopedia. Thanks. Jasmol 23:48, 21 November 2005 (UTC)

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43-Man Squamish
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Image copyright problem with Image:Psaltymain.jpg
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Proposed deletion of Psalty

The article Psalty has been proposed for deletion  because of the following concern:
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Nomination of 43-Man Squamish for deletion
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Nomination of Summit College for deletion
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title: User talk:Just4jesus


text:
66 Arietis

66 Arietis (abbreviated 66 Ari) is a double star in the northern constellation of Aries. 66 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 6.03, putting it near the limit for naked eye visibility. The magnitude 10.4 companion is located at an angular separation of 0.810 arcseconds from the primary along a position angle of 65°. The distance to this pair, as determined from parallax measurements made during the Hipparcos mission, is approximately 210 ly.

The spectrum of the primary component matches a stellar classification of K0 IV, with the luminosity class of IV indicating this is a subgiant star. It has 6 times the radius of the Sun and shines with 18 times the Sun's energy. This energy is radiated from the outer atmosphere at an effective temperature of 4,864 K, giving it the cool orange-hued glow of a K-type star.

title: 66 Arietis


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29 Aquarii

29 Aquarii is a binary star system located around 590 light years away from the Sun in the equatorial constellation of Aquarius. 29 Aquarii is the Flamsteed designation; the system also bears the variable star designation DX Aquarii. It is a challenge to view with the naked eye, appearing as a dim star with a combined apparent visual magnitude of 6.39. The system is moving further from the Earth with a heliocentric radial velocity of about +15 km/s.

This is a spectroscopic binary system with a close circular orbit taking just 0.945 days to complete. Despite their proximity, this does not appear to be a contact binary system. The orbital plane of the two stars lies near the line of sight, so they form an Algol-type eclipsing binary. The first component of the system is an A-type main sequence star with a stellar classification of A2 V. Its companion is giant star with a classification of K0 III.

The variability of this system was first noticed in 1965 by W. Strohmeier of Remeis-Observatory in Bamberg, Germany. He later discovered that the variability was caused by a binary companion eclipsing the primary star.

title: 29 Aquarii


text:
User talk:Justinshred

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:19, 14 October 2005 (UTC)
 * The five pillars of Wikipedia
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title: User talk:Justinshred


text:
30 Arietis

30 Arietis (abbreviated 30 Ari) is a 6th-apparent-magnitude multiple star system in the constellation of Aries. 30 Arietis is the Flamsteed designation. 30 Arietis A and B are separated by $136.862$ or about $−15.188$ at a distance of 130 light years away. The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores. The 30 Arietis system is 910 million years old, one fifth the age of the Sun.

Star system
30 Arietis A and B are separated by 38.1", corresponding to 1,500 AU at a distance of 130 light years. The pair are at almost the same distance, have very similar proper motions, and are considered almost certain to be gravitationally bound with a likely period around 34,000 years.  The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores.

30 Arietis A is a spectroscopic binary with an orbital period of 1.1 days. The primary Aa is an F-type main sequence star about 31% more massive than the Sun, while the companion Ab is a faint red dwarf only about 15% the mass of the Sun.

30 Arietis B has been reported to have a red dwarf companion at a distance of $141.411$ and another red dwarf Bb at about $−10.677$. In 2020, after the inclination of the planetary orbit was measured, the "planet" was found to fall in the mass range of a brown or red dwarf. The more distant companion was referred to as C to distinguish it from Bb, and at about 0.5" it has been imaged using adaptive optics.

30 Arietis Bb
30 Arietis Bb (sometimes abbreviated 30 Ari Bb) is a red dwarf which orbits the F-type main sequence star 30 Arietis Ba, located in a quintuple star system approximately 146 light years away in the constellation Aries. The red dwarf, initially believed to be a massive planet or brown dwarf, was announced in a paper published online on September 24, 2009. It was discovered by using precision radial velocity measurements from the echelle spectrograph installed on the Alfred-Jensch telescope in Karl Schwarzschild Observatory. The star had a minimum mass of nearly 10 times that of Jupiter. In 2020, after the inclination of the planetary orbit was measured to be just 4.14$4.14$°, the "planet" was found to fall in the mass range of red dwarf stars.

title: 30 Arietis


text: User talk:68.73.119.50

title: User talk:68.73.119.50


text:
16 Arietis

16 Arietis (abbreviated 16 Ari) is a star in the northern constellation of Aries. 16 Arietis is the Flamsteed designation. Its apparent magnitude is 6.01. Based upon the annual parallax shift of 6.27 ± 0.07 mas, this star is approximately 520 ly distant from Earth. The brightness of this star is diminished by 0.40 in magnitude from extinction caused by interstellar gas and dust. This is an evolved giant star with a stellar classification of K3 III.

title: 16 Arietis


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58 Aquarii

58 Aquarii, abbreviated 58 Aqr, is a star in the constellation of Aquarius. 58 Aquarii is its Flamsteed designation. It is a sixth magnitude star with an apparent visual magnitude of 6.39, which means it is a challenge to view with the naked eye. Based upon an annual parallax shift of $0.29$, it is located 243 light years from the Sun. This has been identified as a visual binary system with an orbital period of 829.976 days in a circular orbit (eccentricity of zero).

The primary component has a stellar classification of A9/F0 V, matching a main sequence star with a spectrum showing mixed traits of an A/F-type. (Cowley and Fraquelli [1974] has previously assigned it a giant star class of A8 III.) It is a chemically peculiar Am star, showing metallic lines with no magnetic field. The star has 1.7 times the mass of the Sun and 2.1 times the Sun's radius. It is radiating 12 times the Sun's luminosity from its photosphere at an effective temperature of 7,477 K.

title: 58 Aquarii


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User:Sjkebab

I'm SJKebab, and I work in a lab. That's about all I can say really

title: User:Sjkebab


text:
11 Arietis

11 Arietis (abbreviated 11 Ari) is a star in the northern constellation of Aries. 11 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 6.01, which makes it a challenging target to view with the naked eye in suitably dark skies. Based upon an annual parallax shift of 3.72 mas, the distance to this star is approximately 880 ly.

11 Arietis has a stellar classification of B9 IV-Vn, which may indicate that it is beginning to evolve away from the main sequence into a subgiant as the supply of hydrogen at its core becomes exhausted. At present, it has an estimated radius of 2.8 times that of the Sun, but this will increase as it continues to evolve into a giant star. 11 Arietis is spinning rapidly with a projected rotational velocity of 249 km/s. This motion, combined with the Doppler effect, is causing the absorption lines in the spectrum to spread out and become 'nebulous', as indicated by the 'n' suffix in the classification.

title: 11 Arietis


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61 Aquarii

61 Aquarii, abbreviated 61 Aqr, is an orange-hued star in the zodiac constellation of Aquarius. 61 Aquarii is its Flamsteed designation. It has an apparent visual magnitude of 6.39, which indicates it is a dim star that requires good seeing conditions to view. Based upon an annual parallax shift of $1.42$ as seen from Earth's orbit, the star is located around 500 light years away. It is moving closer to the Earth with a heliocentric radial velocity of −8 km/s.

This is an evolved K-type giant star with a stellar classification of K4 III, which indicates it has consumed the hydrogen at its core and expanded. It has an estimated 0.57 times the mass of the Sun but with over 11 times the Sun's radius. The star is radiating 127 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,430 K.

title: 61 Aquarii


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Operation Culverin

Operation Culverin was a planned operation in World War II, in which Allied troops would recapture the northern tip of Sumatra (the present day province of Aceh) from the Japanese. "Culverin" was a code name for "Operations against northern Sumatra / Malaya" and "First Culverin" (originally "Junior Culverin") was "Operations against northern Sumatra" alone. It was never carried out. Lack of resources prevented it being mounted as originally planned, and other events later made it unnecessary.

The idea was first put forward by Winston Churchill at the Quebec Conference on August 20, 1943, for an operation in May and June 1944. He was dissatisfied by the existing scope of Allied plans for the South East Asian Theatre for 1943 and 1944. In his vision, by seizing northern Sumatra, "we should be striking and seizing a point of our own against which the Japanese would have to beat themselves if they wished to avoid the severe drain which would be imposed on their shipping by our air action from Sumatra".

No detailed staff study of the operation had been made yet, and the Combined Chiefs of Staff were opposed. The British Chiefs of Staff said a whole front could not be supplied from the air, but an attack on northern Sumatra or Malaya leading to the capture of Singapore might be carried out in spring 1945. The matter was allowed to lapse.

It was revived in February 1944, when a delegation from Admiral Mountbatten, the Supreme Commander of the South East Asia Command, reported to the Defence Committee in London. Mountbatten proposed amphibious operations in cooperation with the American South West Pacific Area. "Culverin" would be a necessary first part of the plan. However, Mountbatten and the British Chiefs of Staff saw three objections to "Culverin" (or "Vanguard", a plan to capture Rangoon from the sea): "Culverin" might not have the effect that Churchill hoped since the Japanese in Burma could not be bypassed and would still be a threat. The CIGS said that only "Vanguard" could kill "Champion" (a plan to advance into central Burma from the north). "Vanguard" was a complement to preliminary operations further north. Also, a decision had to be made by 1 September.

The American Joint Chiefs of Staff did not favour "Culverin", partly because Mountbatten's Deputy Supreme Commander, the American General Joseph Stilwell, had sent a separate mission to Washington, DC, to represent his own differing views to the Joint Chiefs of Staff.

In the event, most of the Imperial Japanese Navy's battleships and cruisers were transferred to Singapore at about the same time. As amphibious operations depended on local naval superiority, "Culverin" had to be abandoned. The Royal Navy could not reinforce its fleet in the Indian Ocean with sufficient strength to face the Japanese main battle fleet, and the US Navy was committed to operations in the Central Pacific and South West Pacific and unwilling to divert their fleets from the Pacific.

The South East Asia Command was far more cautious in its estimates for resources required for successful amphibious operations than Churchill. For the much less ambitious Operation Buccaneer, the proposed capture of the Andaman Islands, they proposed a land force of 50,000 men, but Churchill had assumed that only a single division (14,000 men) would be necessary. Also, since no land-based air support would be available until a very large beachhead had been secured, Mountbatten demanded the use of almost every aircraft carrier possessed by the Royal Navy, which would have had adverse effects on other operations.

In mid-1945, the matter was finally dropped. The Japanese fleet had been destroyed or immobilised, but the preferred plan was Operation Zipper, a landing on the coast of Malaya. The final major landing in the area was the May 1945 assault on Rangoon, Operation Dracula.

title: Operation Culverin


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51 Arietis

51 Arietis is a star in the northern constellation of Aries. 51 Arietis is the Flamsteed designation. It is a dim, yellow-hued star – a challenge to view with the naked eye, having an apparent visual magnitude of 6.6. Based upon parallax measurements, the star is located at an estimated distance of 67.3 ly from the Sun. It is receding from the Earth with a heliocentric radial velocity of +9.5 km/s, and is a member of the IC 2391 moving group.

This is an ordinary G-type main sequence star with a stellar classification of G8 V. Similar to the Sun, it has 1.04 times the mass and 0.99 times the Sun's radius. It is 1.4 billion years old with a leisurely rotation rate, showing a projected rotational velocity of 4 km/s. The atmospheric metallicity is higher than solar. The star radiates 92% of the Sun's luminosity from its photosphere at an effective temperature of 5,666 K. This heat gives it the golden-hued glow of a G-type star.

title: 51 Arietis


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24 Aquarii

24 Aquarii is a triple star system in the equatorial constellation of Aquarius. 24 Aquarii is the Flamsteed designation. The apparent magnitude of this system is 6.66, which, according to the Bortle Dark-Sky Scale, means it is a faint star that is just visible to the naked eye from dark, rural skies. It has an annual parallax shift of $−15.86$, which is equivalent to a distance of 130 ly from Earth. The system is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.

The calculated orbit of the visual binary has a period of 48.65 years and a large eccentricity of 0.868. The primary, component A, is itself a single-lined spectroscopic binary with a period of 5.8839 days and an eccentricity of $1.42$. One study gives the system a stellar classification of F7 III, suggesting it contains an evolved giant star. Other classifications give classes matching F-type main-sequence stars for components Aa and B.

title: 24 Aquarii


text:
HR 515

HR 515 is a variable star in the zodiac constellation of Pisces, near the eastern constellation border with Aries. Before the constellation borders were officially set, it held the Flamsteed designation of 3 Arietis, abbreviated 3 Ari). This star has the variable star designation VY Piscium, or VY Psc for short. It is a white-hued star that is near the lower limit of visibility to the naked eye with an apparent visual magnitude that ranges from 6.54 down to 6.59. Parallax measurements provide a distance estimate of approximately 503 light years from the Sun.

Gray and associates (1989) found a stellar classification of A8 III for this object, matching an evolved A-type giant star. Abt and Morrell (1995) listed a class of F0V, suggesting it is an F-type main-sequence star. It is a Delta Scuti variable whose brightness varies between magnitudes 6.54 and 6.59 with a period of 0.219 days. The star shows a high rate of spin with a projected rotational velocity of 96 km/s. It has 4.7 times the size of the Sun and is radiating 60 times the Sun's luminosity from its photosphere at an effective temperature of 7,401 K.

title: HR 515


text:
Talk:Active runway

Merge
Most of this is covered at runway. Seems like this may be better as a section of that article than on it's own, for better context. Friday (talk) 03:21, 14 October 2005 (UTC)

title: Talk:Active runway


text:
36 Arietis

36 Arietis is a star in the northern constellation of Aries. 36 Arietis is the Flamsteed designation. It is a dim, orange-hued star that is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40. Based upon an annual parallax shift of $1.143$, this star is located 380 ly away from the Sun. It is moving closer to the Earth with a heliocentric radial velocity of −34 km/s, and is a member of the Wolf 630 moving group of stars that share a common motion through space.

This object is an evolved giant star with a stellar classification of K2 III. It is around two million years old with a similar mass as the Sun. With the hydrogen at its core exhausted, the star has expanded to ten times the girth of the Sun. It has a higher than solar metallicity, showing a high abundance of iron in its spectrum. The star is radiating 44 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,749 K.

title: 36 Arietis


text:
25 Arietis

25 Arietis is a star in the equatorial constellation of Cetus, near the modern constellation boundary with Aries for which it is named. 25 Arietis is the Flamsteed designation. It has an apparent visual magnitude of 6.45, placing it near the lower limit of visibility to the naked eye. The distance to this star can be estimated from its annual parallax shift of $0.45$, which yields a separation of 119 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −40 km/s, and is predicted to come as close as 31.51 pc in 259,000 years. It has a relatively high proper motion, traversing the celestial sphere at the rate of $−39.54$ per year.

This is an ordinary F-type main-sequence star with a stellar classification of F5 V. It is about 1.6 billion years old with an estimated 1.19 times the mass of the Sun and 1.44 times the Sun's radius. The star is radiating 2.9 times the Sun's luminosity from its photosphere at an effective temperature of around 6,274 K.

title: 25 Arietis


text:
User talk:Buck O'Nollege

Archives: a1(welcome) a2(suggest)

Inappropriate comment on the Keeping Up With The Kardasians talk page
Here is the comment: The series premiere date is listed as October 14,2007 in the article, which would fit with E!'s airing of new episodes on Sunday night. However, Zap2It's page on KUWtK list a premiere date of October 13,2007. Does anyone know if E! aired a "sneak preview" on Saturday, or is Zap2It wrong (Heaven Forbid!)?Buck O'Nollege 04:20, 16 March 2008 (UTC) OBMA IS FUCKING HOT

The inappropriate part being "OBMA IS FUCKING HOT." — Preceding unsigned comment added by User: (talk • contribs)

Overlinking of Pioneer League
Hi, Buck O'Nollege. The Manual of Style for disambiguation pages specifies that there should only be one navigable (blue) link per entry, so I adjusted you edit to this article. Best wishes. Gwguffey (talk) 05:26, 23 February 2008 (UTC)

 * You are so right about learning something new every day around here. I think that's the best part. Happy editing until our paths cross, again.  Gwguffey (talk) 06:41, 24 February 2008 (UTC)

Max disambiguation
Hi. First I'd like to thank you for pointing out the WP guideline that each bulleted entry should have exactly one navigable (blue) link. This makes sense and explains your concerns about my first edit of max in mathematics. However, let me explain the rationale for changing the original link that pointed to mathematics. A reader who is looking for the meaning of max is not much helped by a link pointing to the general mathematics article, since there is no definition of neither maximal element, greatest element, nor extreme value there. There isn't even a helpful link under "See also" in that article. For this reason, my second attempt had one blue link only, pointing to the article Maxima and minima, which explains the difference between the three concepts referred to on the disambiguation page. Can you follow my line of reasoning? Isheden (talk) 06:38, 13 October 2010 (UTC)

Speedy deletion nomination of Ellipsis humor

A tag has been placed on Ellipsis humor, requesting that it be speedily deleted from Wikipedia. This has been done under section G1 of the criteria for speedy deletion, because the page appears to have no meaningful content or history, and the text is unsalvageably incoherent. If the page you created was a test, please use the sandbox for any other experiments you would like to do. Feel free to leave a message on my talk page if you have any questions about this.

If you think that this notice was placed here in error, you may contest the deletion by adding to the top of the page that has been nominated for deletion (just below the existing speedy deletion, or "db", tag; if no such tag exists, then the page is no longer a speedy delete candidate and adding a hang-on tag is unnecessary), coupled with adding a note on the talk page explaining your position, but be aware that once tagged for speedy deletion, if the page meets the criterion, it may be deleted without delay. Please do not remove the speedy deletion tag yourself, but don't hesitate to add information to the page that would render it more in conformance with Wikipedia's policies and guidelines. Fæ (talk) 07:16, 17 November 2010 (UTC)

question
So you read my user page; very funny. But even if I could see, how would I know how many fingers you're holding up when we don't have photo or video communication here?

Academic Challenger (talk) 07:35, 17 November 2010 (UTC)

 * Doctor, we have a patient here in need of an emergecy stickectomy!

Notification: changes to "Mark my edits as minor by default" preference
Hello there. This is an automated message to tell you about the gradual phasing out of the preference entitled "Mark all edits minor by default", which you currently have (or very recently had) enabled.

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Thank you for your understanding and happy editing :) Editing on behalf of User:Jarry1250 18:11, 14 March 2011 (UTC)

title: User talk:Buck O'Nollege


text:
International Capoeira Angola Foundation

ICAF (International Capoeira Angola Foundation) or FICA (Fundaçao Internacional de Capoeira de Angola) is the name of a capoeira angola group. FICA is the group's name in Brazil, which is an acronym for Fundacao International de Capoeira de Angola, while it is ICAF in English, which stands for the International Capoeira Angola Foundation. The English name is a literal translation of the words which make up the acronym FICA.

The word "fica" in Portuguese means "you stay" (second person declarative) which is not necessarily significant, but because it has a meaning it is slightly more catchy in Portuguese than ICAF is in English. FICA/ICAF is the largest Capoeira Angola organization in the world, consisting of many local chapters incorporated as not-for-profits in the United States which charge nominal annual membership fees, as well as having locations in many other countries.

The three founders of FICA are Mestre Cobra Mansa, Mestre Jurandir, and Mestre Valmir. As of 2020, there are 12 Mestres of FICA: The three founders, Mestre Silvinho, Mestre Leninho Sa, Mestre Gunter, Mestre Fabio, Mestre Beto, Mestre Kamau, Mestre Kojo, Mestre Skher, and Mestre Santemu. Former leaders of FICA include Mestra Gege and Mestre Rogerinho.


text:
User talk:Marxfonseca

Welcome!

Hello, and welcome to Wikipedia! Thank you for your contributions. I hope you like the place and decide to stay. Here are a few good links for newcomers: I hope you enjoy editing here and being a Wikipedian! Please sign your name on talk pages using four tildes (~~); this will automatically produce your name and the date. If you have any questions, check out Where to ask a question or ask me on my talk page. Again, welcome! ≈ jossi fresco ≈ 03:22, 14 October 2005 (UTC)
 * The five pillars of Wikipedia
 * How to edit a page
 * Help pages
 * Tutorial
 * How to write a great article
 * Manual of Style

title: User talk:Marxfonseca


text:
Ballad of a Thin Man

"Ballad of a Thin Man" is a song written and recorded by Bob Dylan, and released in 1965 on his sixth studio album, Highway 61 Revisited.

Recording
Dylan recorded "Ballad of a Thin Man" in Studio A of Columbia Records in New York City, located at 799 Seventh Avenue, just north of West 52nd Street on August 2, 1965. Record producer Bob Johnston was in charge of the session, and the backing musicians were Mike Bloomfield on lead guitar, Bobby Gregg on drums, Harvey Brooks on bass, Al Kooper on organ, and Dylan himself playing piano. Driven by Dylan's sombre piano chords, which contrast with a horror movie organ part played by Al Kooper, this track was described by Kooper as "musically more sophisticated than anything else on the Highway 61 Revisited album."

Kooper has recalled that at the end of the session, when the musicians listened to the playback of the song, drummer Bobby Gregg said, "That is a nasty song, Bob." Kooper adds, "Dylan was the King of the Nasty Song at that time."

Meaning
Dylan's song revolves around the mishaps of a Mr. Jones, who keeps blundering into strange situations, and the more questions he asks, the less the world makes sense to him. Critic Andy Gill called the song "one of Dylan's most unrelenting inquisitions, a furious, sneering, dressing-down of a hapless bourgeois intruder into the hipster world of freaks and weirdoes which Dylan now inhabited."

In August 1965, soon after recording the song, when questioned by Nora Ephron and Susan Edmiston about the identity of Mr. Jones, Dylan was deadpan: "He's a real person. You know him, but not by that name... I saw him come into the room one night and he looked like a camel. He proceeded to put his eyes in his pocket. I asked this guy who he was and he said, 'That's Mr. Jones.' Then I asked this cat, 'Doesn't he do anything but put his eyes in his pocket?' And he told me, 'He puts his nose on the ground.' It's all there, it's a true story." At a press conference in San Francisco in December 1965, Dylan supplied more information about Mr. Jones: "He's a pinboy. He also wears suspenders."

In March 1986, Dylan told his audience in Japan: "This is a song I wrote a while back in response to people who ask me questions all the time. You just get tired of that every once in a while. You just don't want to answer no more questions. I figure a person’s life speaks for itself, right? So, every once in a while you got to do this kind of thing, you got to put somebody in their place... So this is my response to something that happened over in England. I think it was about '63, '64. [sic] Anyway the song still holds up. Seems to be people around still like that. So I still sing it. It's called 'Ballad Of A Thin Man'."

There has been speculation whether Mr. Jones was based on a specific journalist. In 1975, reporter Jeffrey Jones "outed" himself in a Rolling Stone article, describing how he had attempted to interview Dylan at the 1965 Newport Folk Festival. When Dylan and his entourage later chanced on the hapless reporter in the hotel dining room, Dylan shouted mockingly, "Mr. Jones! Gettin' it all down, Mr. Jones?" When Bill Flanagan asked Dylan, in 1990, whether one reporter could claim all the credit for Mr. Jones, Dylan replied: "There were a lot of Mister Joneses at that time. Obviously there must have been a tremendous amount of them for me to write that particular song. It was like, 'Oh man, here's the thousandth Mister Jones'."

In the John Lennon-penned Beatles song "Yer Blues", Lennon describes the character as feeling "suicidal, just like Dylan's Mr. Jones".

Interpretation
Dylan critic Mike Marqusee writes that "Ballad of a Thin Man" can be read as "one of the purest songs of protest ever sung", with its scathing take on "the media, its interest in and inability to comprehend [Dylan] and his music." For Marqusee, the song became the anthem of an in-group, "disgusted by the old, excited by the new... elated by their discovery of others who shared their feelings", with its central refrain "Something is happening here/ But you don't know what it is/ Do you, Mr. Jones?" epitomizing the hip exclusivity of the burgeoning counterculture. Dylan biographer Robert Shelton describes the song's central character, Mr. Jones, as "one of Dylan's greatest archetypes", characterizing him as "a Philistine, a person who does not see... superficially educated and well bred but not very smart about the things that count."

Critic Andy Gill refers to "a fascinating, albeit very idiotic and moronic, interpretation of the song as 'outing' a homosexual". Gill writes that this interpretation is based upon "the cumulative inference of references" to a series of images in the song: "pen in your hand", "hands you a bone", "contacts among the lumberjacks", "sword swallower", "he clicks his high heels", "he says, 'Here is your throat back, thanks for the loan'", "one-eyed midget" and "give me some milk". Gill is skeptical about this idea which he claims has appeared on internet sites devoted to Dylan's work, and writes that it "is probably more indicative of the pitfalls of interpretation than Dylan’s intention with the song"; he adds that the song "condemns the urge to interpret pruriently that which we don’t immediately understand."

Huey P. Newton and others in the Black Panther Party admired the song, as well as Stokely Carmichael. Newton interpreted the lyrics as being about racism.

Releases
The song was originally released in 1965 on the album Highway 61 Revisited. An incomplete early take of the song, immediately preceding the master and featuring organ fills by Paul Griffin, was released on the 6-disc and 18-disc editions of The Bootleg Series Vol. 12: The Cutting Edge 1965–1966 in 2015.

Dylan has released live recordings of the song on Before the Flood (1974; recorded February 14, 1974), Bob Dylan at Budokan (1979; recorded March 1, 1978), Real Live (1984; recorded July 7, 1984), Hard to Handle (video, 1986; recorded February 24, 1986), The Bootleg Series Vol. 4: Bob Dylan Live 1966, The "Royal Albert Hall" Concert (1998; recorded May 17, 1966), The Bootleg Series Vol. 7: No Direction Home: The Soundtrack (2005; recorded May 20, 1966; also released in 2018 on Live 1962–1966: Rare Performances From The Copyright Collections), and The Bootleg Series Vol. 13: Trouble No More 1979–1981 (Deluxe Edition) (2017; recorded June 27, 1981). In 2016, all the 1966 live performances of the song were assembled on the box set The 1966 Live Recordings, with the May 26, 1966 performance released separately on the album The Real Royal Albert Hall 1966 Concert.

Personnel

 * Bob Dylan – vocals, piano
 * Mike Bloomfield – lead guitar
 * Al Kooper – organ
 * Harvey Brooks – bass guitar
 * Bobby Gregg – drums

title: Ballad of a Thin Man


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12 Aquilae

12 Aquilae (abbreviated 12 Aql) is a star in the equatorial constellation of Aquila. 12 Aquilae has the Bayer designation of i Aquilae and is most easily recognized in the sky being next to the brighter star λ (lambda) Aquilae.

In Chinese, 天弁 (Tiān Biàn), meaning Market Officer, refers to an asterism consisting of 12 Aquilae, α Scuti, δ Scuti, ε Scuti, β Scuti, η Scuti, λ Aquilae, 15 Aquilae and 14 Aquilae. Consequently, 12 Aquilae itself is known as 天弁六 (Tiān Biàn liù, the Sixth Star of Market Officer.)

This star has an apparent visual magnitude of 4.02, which is bright enough to be seen with the naked eye, although, according to the Bortle Dark-Sky Scale, it is a challenge to view from the inner city. Based upon an annual parallax shift of 22.66 mas, the distance to this star is 144 ly with a margin of error of one light-year. This is an evolved giant star of stellar class K1 III. It has 12 times the radius of the Sun and shines with 60 times the Sun's luminosity. This energy is being radiated from its outer atmosphere at an effective temperature of 4,603 K, giving it the cool orange hue of a K-type star.

title: 12 Aquilae


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71 Aquilae

71 Aquilae (abbreviated 71 Aql) is a binary star in the equatorial constellation of Aquila. 71 Aquilae is its Flamsteed designation though it also bears the Bayer designation l Aquilae. The apparent visual magnitude of the system is 4.33, making it bright enough to be viewed by the naked eye. It has an annual parallax shift of 9.67 mas, which equates to a physical distance of 340 ly from Earth, give or take a 30 light-year margin of error. At this distance, the brightness of the system is diminished by 0.065 in visual magnitude from extinction caused by interstellar gas and dust.

This is a spectroscopic binary system where the presence of an orbiting companion is revealed by shifts in the spectral lines caused by the Doppler effect. The primary component is a giant star with a stellar classification of G8 III. The secondary is following a circular orbit with a period of 205.2 days.

title: 71 Aquilae


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69 Aquilae

69 Aquilae, abbreviated 69 Aql, is a star in the equatorial constellation of Aquila. 69 Aquilae is its Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.91. Based upon an annual parallax shift of $−22.51$, it is located 201 light years away. The star is moving closer to the Earth with a heliocentric radial velocity of −22.5 km/s.

The stellar classification of 69 Aquilae is K1/2 III, which means this is an evolved giant star. It belongs to a sub-category called the red clump, indicating that it is on the horizontal branch and is generating energy through helium fusion at its core. The star is about 3.4 billion years old with 1.54 times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 45.7 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,529 K.

title: 69 Aquilae


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70 Aquilae

70 Aquilae, abbreviated 70 Aql, is a single orange-hued star in the equatorial constellation of Aquila. 70 Aquilae is its Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.90. The distance to 70 Aquilae, as determined from its annual parallax shift of $1.606$, is around 940 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.

Classification
Perkins et al. (1989) found a stellar classification of K4+ III Ba1 for this star, suggesting it is a K-type giant with abundance anomaly of barium. Houk and Swift (1999) matched an ordinary giant with a class of K3 III. Many sources    still use the 1991 Bright Star Catalogue classification of K5 II, which instead suggests a bright giant star.

Size and temperature
The interferometry-measured angular diameter of this star, after correcting for limb darkening, is $−9.4$, which, at its estimated distance, equates to a physical radius of roughly 102 times the radius of the Sun. 70 Aquilae is about 63 million years old with 6 times the mass of the Sun. It is radiating 4,072 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,900 K.

title: 70 Aquilae


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26 Aquilae

26 Aquilae (abbreviated 26 Aql) is a binary star system in the equatorial constellation of Aquila. 26 Aquilae is its Flamsteed designation though it also bears the Bayer designation f Aquilae. It has an apparent visual magnitude of 5.00, which means it is faintly visible to the naked eye. As the Earth orbits the Sun, this star system undergoes a parallax shift of 21.15 mas. This means it is located at a distance of approximately 154 ly from Earth, give or take a three-light-year margin of error.

This is a single-lined spectroscopic binary system, meaning that the presence of an orbiting companion is revealed through shifts in the spectrum of the primary star. The pair orbit each other with a period of 266.544 days at a high eccentricity of 0.833. Little is known about this companion, although its mass can be estimated as 140% of the Sun's.

The primary component has a stellar classification of G8 III-IV. The luminosity class of III-IV indicates the spectrum resembles that of a star part way between the subgiant and giant stages of its evolution. It has more than three times the mass of the Sun and six times the Sun's radius. It is radiating 21 times as much luminosity as the Sun from this enlarged outer envelope at an effective temperature of $-16.91$. At this heat, the star glows with the characteristic yellow hue of a G-type star.

title: 26 Aquilae


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Wikipedia talk:Today's featured article/October 11, 2005

Rather than He first appears in the 1992 video game ...

shouldn't it say He first appeared in the 1992 video game ...

in keeping with the article?


text:
Talk:Maria Olaru

Untitled
In 1997 how could she be both 2nd and 3rd in vault?

Is this significant: She was coached by Octavian Belu.?

I reformatted it, looks good to me, but I don't know if there is a standard format for gymnist entries. RJFJR 03:25, 14 October 2005 (UTC)

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title: Talk:Maria Olaru


text:
4 Aquilae

4 Aquilae, abbreviated 4 Aql, is a single, white-hued star in the equatorial constellation of Aquila. 4 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.02, making it a faint star visible to the naked eye. The distance to 4 Aql can be estimated from its annual parallax shift of $−0.055$, yielding an estimated range of around 480 light years. It is moving closer to the Earth with a heliocentric radial velocity of −13 km/s.

This is a B-type main-sequence star with a stellar classification of B9 V. It was classed as a Be star by Arne Sletteback in 1982, indicating it has ionized circumstellar gas. The star is spinning rapidly, showing a projected rotational velocity of 259 km/s, and is being viewed almost equator-on. It has 3.6 times the mass of the Sun and 3 times the Sun's radius. The star is radiating 294 times the Sun's luminosity from its photosphere at an effective temperature of 10,965 K.

title: 4 Aquilae


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Runako Morton

Runako Shakur Morton (22 July 1978 – 4 March 2012) was a Nevisian cricketer who played for West Indies in all formats of the game. He was a right-handed batsman and a right-handed offbreak bowler.

Domestic career
A lively, often unpredictable character, Morton was expelled from the West Indian cricketing academy in July 2001 for bad behaviour but continued to play for the Leeward Islands in the Busta Cup.

International career
Upon his return in February 2002, he was called into the West Indies squad as a replacement for Marlon Samuels, but he was dropped once again when he lied about his non-appearance in the ICC Champions Trophy in September 2002.

Following a stabbing incident in January 2004, he was arrested but was given a third chance in May 2005 when he was recalled for the South African Test.

He was involved in a bizarre run-out with Shivnarine Chanderpaul in the third Test against New Zealand in 2006. Morton drove the ball to mid-on where Daniel Vettori was fielding and ran to the non-striker end. Chanderpaul, at the other end, initially took a few steps down the wicket but then turned and went back to the non-striker's end. Morton believed he was out, and, furious at his captain, began to walk off. However, following a call to the third umpire, it was decided that Morton had grounded his bat at the non-striker's end just before Chanderpaul, and hence was safe and that Chanderpaul was out. Video evidence suggests that the umpire's decision was wrong: although Morton made his ground first, he then left it before the run-out was made, so he should have been the one dismissed.

As a batsman, Morton had a reputation for hitting the ball very hard, but had problems picking up singles in between boundaries. He has the dubious record of the slowest ODI duck which lasted 31 balls in the final of the DLF Cup against Australia.

Morton died on 4 March 2012, when he lost control of the car he was driving along the Sir Solomon Hochoy Highway, hitting a utility pole at Chase Village in Chaguanas, Trinidad and Tobago.

title: Runako Morton


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36 Aquilae

36 Aquilae (abbreviated 36 Aql) is a star in the equatorial constellation of Aquila. 36 Aquilae is its Flamsteed designation though it also bears the Bayer designation e Aquilae. With an apparent visual magnitude of 5.02, this star is faintly visible to the naked eye. It has an annual parallax shift of 6.17 mas, indicating a physical distance of 530 ly with a 30 light-year margin of error.

The spectrum of this star matches a stellar classification of M1 III. It is a red giant star with 54 times the radius of the Sun that is currently on the asymptotic giant branch. This means the star is generating energy by the fusion of hydrogen along an outer shell and helium along a concentric inner shell, surrounding an inert core of carbon and oxygen. 36 Aquilae undergoes small, periodic variations in luminosity, changing by 0.0063 magnitudes about 11.5 times per day, or once every 2 hours and 5.2 minutes.

title: 36 Aquilae


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18 Aquilae

18 Aquilae (abbreviated 18 Aql) is a triple star system in the constellation of Aquila. 18 Aquilae is the Flamsteed designation; it also bears the variable star designation Y Aquilae. It has an apparent visual magnitude of 5.07. The distance to this system can be estimated from the annual parallax shift of 6.43 mas, yielding a value of around 510 ly away from Earth.

The inner pair of stars in this system form a spectroscopic binary with a combined magnitude of 5.44 and an orbital period of 1.302 days. The primary component is a giant star with a stellar classification of B8 III. Because the orbital plane is inclined near the line of sight, two form an eclipsing binary system. The eclipse of the primary component causes a 0.04 drop in magnitude, while the eclipse of the secondary results in a decrease of 0.03. At an angular separation of 0.310 arcseconds is the magnitude 6.39 tertiary component. This system has a high peculiar velocity of 29.7 ± 3.9 km/s relative to the neighboring stars.

title: 18 Aquilae


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23 Aquilae

23 Aquilae is a binary star system in the equatorial constellation of Aquila. 23 Aquilae is its Flamsteed designation. It is at a distance of about 400 ly with an apparent visual magnitude of 5.10, which is bright enough to be faintly visible to the naked eye as an orange-hued star. The brightness of the star is diminished by 0.21 in magnitude because of extinction from interstellar dust and gas. The system is moving closer to the Earth with a heliocentric radial velocity of –23 km/s.

The primary component of this system is a magnitude 5.31 K-type giant star or bright giant with a stellar classification of K1. The star is radiating 165 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,740 K. Orbiting at an angular separation of 3.25 arcseconds is a magnitude 8.76 companion star.

title: 23 Aquilae


text: User talk:24.205.59.223

title: User talk:24.205.59.223


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Ann Austin

Ann Austin (n.d. – 1665) was one of the first Quaker travelling preachers. She and Mary Fisher became the first Quakers to visit the English North American colonies.

Mission to the New World
Austin was a resident of London and the mother of five children when she left England with Mary Fisher to take the Quaker message of George Fox to the New World. She may well have then been in her sixties as she was described at the time as being ‘stricken in years’.

They were subsidised in their mission by Quaker charitable funds and first sailed to Barbados in the Caribbean where they were well received and where they converted the Lieutenant Governor of the island to Quakerism. On 11 July 1656 they became the first Quakers to visit the English North American colonies, arriving at Boston in the Massachusetts Bay Colony on the Swallow. There they met with fierce hostility from the Puritan population and the Deputy Governor of the colony, Richard Bellingham, as news of the heretical views of the Quakers had preceded them.

On arrival, they were taken ashore and imprisoned. They were forced to undress in public, and their bodies were intimately examined for signs of witchcraft, Ann reporting that one of the female searchers was ‘a man in a  [sic] apparel’. Their books and pamphlets were seized and burned by the Boston hangman. An innkeeper, Nicholas Upsall, offered to pay their fines if he were permitted to speak with them in prison but the magistrates, having ordered their prison window to be boarded up so as to isolate them refused his request, the intention being to starve them to death. Upsall then bribed their warder by paying him five shillings a week to allow him to bring food to the women and so saved their lives. Fisher and Austin were deported back to Barbados on the Swallow after five weeks' imprisonment, having been unable to share their faith with anyone except Upsall, who became the first North American Puritan convert to Quakerism.

Fisher and Austin returned to England in 1657. The Boston council declared on 11 July 1656, the day of their arrival that: "there are several laws long since made and published in this jurisdiction bearing testimony against heretics and erroneous persons," and that Ann Austin and Mary Fisher, "upon examination are found not only to be transgressors of the former laws, but to hold very dangerous, heretical, and blasphemous opinions; and they do also acknowledge that they came here purposely to propagate their said errors and heresies, bringing with them and spreading here sundry books, wherein are contained most corrupt, heretical, and blasphemous doctrines contrary to the truth of the gospel here professed amongst us."

On her return from Boston, Ann Austin's ministry continued until her death in prison during the Great Plague of London in 1665. She was buried in the Quaker Burying Ground, Bunhill Fields, London's first Quaker burial ground. It has also been speculated that Austin may have settled, as did Mary Fisher, among the Quakers of South Carolina in the 1680s.

title: Ann Austin


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37 Aquilae

37 Aquilae, abbreviated 37 Aql, is a star in the equatorial constellation of Aquila. 37 Aquilae is its Flamsteed designation. It has an apparent visual magnitude of approximately 5.12, which is bright enough to be visible to the naked eye. The distance to 37 Aql can be estimated from its annual parallax shift of $−30.17$, yielding a range of 444 light years. The star is moving closer to the Earth with a heliocentric radial velocity of −30 km/s, and is predicted to come to within 21.97 pc in around 4.4 million years.

This is an aging giant star with a stellar classification of G8 IIIa. It is uncertain whether this star is on the red giant branch or the horizontal branch; Reffert et al. (2015) give 57% odd that it is the latter. In that case, their model shows an estimated age of 1.2 billion years with 2.3 times the mass of the Sun and 23 times the Sun's radius. It is radiating 219 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,594 K. These coordinates are a source of X-ray emission, which is most likely coming from the star.

title: 37 Aquilae


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21 Aquilae

21 Aquilae is a solitary variable star in the equatorial constellation of Aquila. It has the variable star designation V1288 Aql; 21 Aquilae is its Flamsteed designation. This object is visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of about 5.1. The star is located at a distance of around 680 ly from Earth, give or take a 20 light-year margin of error. It is moving closer to the Earth with a heliocentric radial velocity of –5 km/s.

The stellar classification of this star is B8 II-III, with the luminosity class of II-III suggesting that the spectrum displays elements of both a giant star and a bright giant. It is a chemically peculiar star of the Mercury-Manganese type (CP3), although some catalogues consider that status to be doubtful. This is a probable Alpha2 Canum Venaticorum variable that ranges in visual magnitude from 5.06 down to 5.16. The star is radiating 704 times the luminosity of the Sun from its photosphere at an effective temperature of $9.3 days$; this gives it the blue-white glow of a B-type star.

21 Aquilae is catalogued as an optical double star, having a 12th magnitude companion $12,014 K$ away as of 2010. It was first identified as a double star by John Herschel. The companion is a distant background object.

title: 21 Aquilae


text:
Talk:Inclusionism

Add a link to M:Inclusionism
Link M:Inclusionism to the Meta-wikipedia article!

Canadianism 03:28, 14 October 2005 (UTC)

title: Talk:Inclusionism


text:
31 Aquilae

31 Aquilae (abbreviated 31 Aql) is a star in the equatorial constellation of Aquila. 31 Aquilae is its Flamsteed designation though it also bears the Bayer designation b Aquilae. This star has an apparent visual magnitude of 5.16 and is 49.5 light years from Earth. It has no known companions.

Properties
31 Aquilae has an apparent visual magnitude of 5.16, making it bright enough to be seen with the naked eye in dark skies. The annual parallax shift of 65.89 mas yields a distance estimate of 49.5 ly from Earth. It is a variable star with a magnitude change of less than 0.02.

With a stellar classification of G8 IV, the luminosity class of IV indicates this is a subgiant star. Compared to the Sun, it has 116% of the mass and 138% of the radius. It is radiating nearly double the luminosity of the Sun from its outer atmosphere at an effective temperature of 5,510 K, giving it the yellow hue of a G-type star. Its age is probably similar to NGC 188, the oldest open cluster known, which was calculated to be over 5 billion years. For its age, it is surprisingly rich in elements other than hydrogen or helium, contrary to common assumptions that the oldest stars should be metal-poor.

No certain substellar companion has been detected so far around 31 Aquilae. McDonald Observatory team has set limits to the presence of one or more planets around 31 Aquilae with masses between 0.22 and 1.9 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.

Optical companions
The following stars are optical companions that are coincidentally aligned near the line of sight to 31 Aquilae.

title: 31 Aquilae


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19 Aquilae

19 Aquilae is a single star located 142 ly away from the Sun in the equatorial constellation of Aquila. 19 Aquilae is the Flamsteed designation. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.23. The star is moving closer to the Earth with a heliocentric radial velocity of −46.7 km/s.

This object has a stellar classification of F0 III-IV, with the luminosity class matching an evolving star transitioning from the subgiant to a giant stage. Poretti et al. (2003) list it as a suspected Gamma Doradus variable, and it is located near the cooler end of the instability strip on the Hertzsprung–Russell diagram. These spatial coordinates are a source of X-ray emission, which is most likely coming from the star.

19 Aquilae is an estimated 2.25 billion years old with a moderately high rate of spin, showing a projected rotational velocity of 57.0 km/s. It has 1.54 times the mass of the Sun and 2.50 times the Sun's radius. The star is radiating 12.8 times the luminosity of the Sun from its photosphere at an effective temperature of 6,784 K.

title: 19 Aquilae


text:
Wikipedia:Requests for mediation/Price-Anderson Nuclear Industries Indemnity Act

Summary of dispute
The Price-Anderson Act arranges insurance for U.S. nuclear power plants and Department of Energy facilities.

At this point, the consensus of the goal appears to be to build an encyclopedia-grade article acceptable to all parties. In particular, one cannot easily discern how the act works from the current text. Simesa 00:36, 14 October 2005 (UTC)

Summary of situation
This topic was contentious from the day it was written. It has been through the RfC and RfP processes, and went into Mediation with Ed Poor, who appears to no longer be able to continue. There is an extreme amount of history, which the Mediator may or may not wish to consider.

The last technique applied by Ed Poor was for each user to select text that they felt was contentious, and "embargo" it to the Talk page pending mediated resolution. Thus, there is text on the Talk page to be mediated as well.

A mediator can expect to be discussing how to mention the Chernobyl accident in the article. Simesa 00:36, 14 October 2005 (UTC)

Users involved

 * user:Simesa
 * user:Benjamin Gatti
 * user:Katefan0 (admin)
 * user:Woohookitty (admin)

I'll assign Ral315 to this case. I hope he knows the procedure (Ral contact me in IRC if you need help) R  e  dwolf24  (talk—How's my driving?) 03:26, 14 October 2005 (UTC)

 * Yeah, I'll take this.  Ral  315   WS  03:36, 14 October 2005 (UTC)
 * (sigh) My first failure. Oh, well, it's better to admit it than to remain in denial. Now this matter can move forward again. And maybe I'll jump in and start editing! Uncle Ed 18:37, 16 October 2005 (UTC)


text:
11 Aquilae

11 Aquilae (abbreviated 11 Aql) is a single star in the equatorial constellation of Aquila. 11 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.2, which means it is faintly visible to the naked eye. Based upon an annual parallax shift of $3.49$, the distance to this star is approximately 156 ly. The brightness of this star is diminished by 0.33 in magnitude because of extinction from interstellar gas and dust.

This is an F-type main sequence star with a stellar classification of F8 V. It is radiating about 15.4 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 6,118 K, giving it the yellow-white glow of an F-type star. 11 Aquilae has been listed as a candidate for membership in the Ursa Major Moving Group, but most likely does not belong to that association.

title: 11 Aquilae