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{{Starbox begin
|name = Beta Virginis
}}
{{Starbox observe
|epoch = J2000
|ra = 11<sup>h</sup> 50<sup>m</sup> 41.7<sup>s</sup>
|dec = +1° 45&prime; 53&Prime;
|ra = {{RA|11|50|41.7185}}
|dec = {{DEC|+1|45|52.985}}
|appmag_v = 3.61
|constell = [[Virgo (constellation)|Virgo]]
}}
{{Starbox character
|class = F9&nbsp;V
|b-v = 0.55
|u-b = 0.11
|variable = none
}}
{{Starbox astrometry
|radial_v = 4.6
|prop_mo_ra = 740.96
|prop_mo_dec = -271.18
|parallax = 91.74
|p_error = 0.77
|absmag_v = 3.40
}}
{{Starbox detail
|mass = 1.25<ref name="na10">{{cite journal
|author=Carrier, F.; Eggenberger, P.; D'Alessandro, A.; Weber, L.
|title=Solar-like oscillations in the F9 V &beta; Virginis
|journal=New Astronomy |year=2005 |volume=10
|issue=4 |pages=315–323
|url=http://www.citebase.org/fulltext?format=application%2Fpdf&identifier=oai%3AarXiv.org%3Aastro-ph%2F0502014
|accessdate=2007-06-05
|doi=10.1016/j.newast.2004.11.003}}</ref>
|radius = 1.66<ref name="na10"/>
|luminosity = 3.51<ref name="na10"/>
|temperature = 6,140<ref name="na10"/>
|metal = [Fe/H]&nbsp;=&nbsp;0.20<ref name="aaa65"/>
|gravity = 4.25<ref name="aaa65"/>
|rotation = 4.3&nbsp;km/s<ref name="na10"/>
|age = 2.8×10<sup>9</sup><ref name="spocs" >[http://adsabs.harvard.edu/abs/2005ApJS..159..141V Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs]</ref>
}}
{{Starbox catalog
|names = Zavijava, Zavijah, Alaraph, Minelauva, 5 Virginis, [[Henry L. Giclas catalogue|Gl]] 449, [[Harvard Revised catalogue|HR]] 4540, [[Bonner Durchmusterung|BD]] +02°2489, [[Henry Draper catalogue|HD]] 102870, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 119076, FK5 445, GC 16215, CCDM 11507+0146, [[Hipparcos catalogue|HIP]] 57757.
}}
{{Starbox reference
|Simbad = HD+102870
|ARICNS = 00916
}}
{{Starbox end}}

'''Beta Virginis''' (β Vir / β Virginis) is a [[star]] in the [[constellation]] [[Virgo (constellation)|Virgo]]. It has the traditional names '''Zavijava''' (also '''Zavijah''') and '''Alaraph'''<ref>Atlas of the Heavens, part II, catalogue, Antonín Bečvář</ref>. Despite being the ''beta'' star of the constellation Virgo it is only the fifth star in order of brightness.

Physically, Beta Virginis is larger and more massive than the Sun, and is comparatively metal-rich. That is, it has a higher preponderance of elements heavier than helium.<ref name="aaa65">{{cite journal
|author=Gehren, T.
|title=On the chemical composition and age of Beta VIR
|journal=Astronomy and Astrophysics |year=1978
|volume=65 |issue=3 |pages=427–433
|url=http://adsabs.harvard.edu/abs/1978A&A....65..427G
|accessdate=2007-06-05}}</ref>

Since it is close to the [[ecliptic]], it can be [[Occultation|occulted]] by the [[Moon]] and (very rarely) by [[planet]]s. The next planetary [[occultation]] of Zavijava will take place on 11 August 2069 by [[Venus]].

This was the star Einstein used during the solar eclipse of September 21, 1922 to determine the speed of light in space, as it fell close to the Sun.

==Etymology==
The medieval name Zavijava (Zavijah, Zavyava, Zawijah) is from the Arabic زاوية العوى ''zāwiyat al-<sup>c</sup>awwa’'' "Corner of the barking (dog)". Another name was Alaraph.

== Hunt for substellar objects ==
According to Nelson & Angel (1998)<ref name="1998ApJ">[http://adsabs.harvard.edu/abs/1998ApJ...500..940N The Range of Masses and Periods Explored by Radial Velocity Searches for Planetary Companions]</ref>, Beta Virginis could host two or three [[jovian planets]] either [brown dwarfs] in wide orbits. The authors have set an upper limit of 1.9, 5 and 23 [[Jupiter masses]] for the putative planets with orbital periods of 15, 25 and 50 years respectively. Also Campbell et al. 1988<ref name="substellar" >[http://adsabs.harvard.edu/abs/1993ApJ...413..349M A search for substellar companions to southern solar-type stars]</ref> inferred the existence of planetary objects or even [[brown dwarfs]] around Beta Virginis.
However more recent studies have not confirmed the existence of any substellar companion around Beta Virginis yet. [[McDonald Observatory]] team has set limits to the presence of one or more planets <ref name="Limits" >[http://arxiv.org/abs/astro-ph/0604171 Detection Limits from the McDonald Observatory Planet Search Program]</ref> with masses between 0.16 and 4.2 [[Jupiter masses]] and average separations spanning between 0.05 and 5.2 [[Astronomical Units]].

{{przypisy}}

==External links==
* {{cite web |last=Kaler |first=Jim |year=2007 |url=http://www.astro.uiuc.edu/~kaler/sow/zavijava.html |title=Zavijava |publisher=Stars: Portraits of Stars and their Constellations |accessdate=2007-06-06}}
* {{cite web |url=http://www.alcyone.de/SIT/mainstars/SIT000833.htm |title=Zavijah |publisher=Alcyone |accessdate=2007-06-06}}

<nowiki>
[[Category:Virgo constellation]]
[[Category:Bayer objects|Virginis, Beta]]
[[Category:F-type main sequence stars]]
[[Category:Stars with proper names]]

[[cs:Zavijava]]
[[de:Zavijava]]

[[en:Beta Virginis]]
[[es:Zavijava]]
[[fr:Beta Virginis]]
[[ko:자비야바]]
[[it:Zavijava]]
[[nl:Zavijah]]
[[ja:おとめ座ベータ星]]
[[ru:Завийява]]
[[sk:Zavijava]]

</nowiki>
[[zh:右執法]]

Wersja z 23:43, 10 sie 2010

Szablon:Starbox begin Szablon:Starbox observe Szablon:Starbox character Szablon:Starbox astrometry Szablon:Starbox detail Szablon:Starbox catalog Szablon:Starbox reference Szablon:Starbox end

Beta Virginis (β Vir / β Virginis) is a star in the constellation Virgo. It has the traditional names Zavijava (also Zavijah) and Alaraph[1]. Despite being the beta star of the constellation Virgo it is only the fifth star in order of brightness.

Physically, Beta Virginis is larger and more massive than the Sun, and is comparatively metal-rich. That is, it has a higher preponderance of elements heavier than helium.[2]

Since it is close to the ecliptic, it can be occulted by the Moon and (very rarely) by planets. The next planetary occultation of Zavijava will take place on 11 August 2069 by Venus.

This was the star Einstein used during the solar eclipse of September 21, 1922 to determine the speed of light in space, as it fell close to the Sun.

Etymology

The medieval name Zavijava (Zavijah, Zavyava, Zawijah) is from the Arabic زاوية العوى zāwiyat al-cawwa’ "Corner of the barking (dog)". Another name was Alaraph.

Hunt for substellar objects

According to Nelson & Angel (1998)[3], Beta Virginis could host two or three jovian planets either [brown dwarfs] in wide orbits. The authors have set an upper limit of 1.9, 5 and 23 Jupiter masses for the putative planets with orbital periods of 15, 25 and 50 years respectively. Also Campbell et al. 1988[4] inferred the existence of planetary objects or even brown dwarfs around Beta Virginis. However more recent studies have not confirmed the existence of any substellar companion around Beta Virginis yet. McDonald Observatory team has set limits to the presence of one or more planets [5] with masses between 0.16 and 4.2 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.

  1. ↑ Atlas of the Heavens, part II, catalogue, Antonín Bečvář
  2. ↑ Szablon:Cite journal
  3. ↑ The Range of Masses and Periods Explored by Radial Velocity Searches for Planetary Companions
  4. ↑ A search for substellar companions to southern solar-type stars
  5. ↑ Detection Limits from the McDonald Observatory Planet Search Program

External links

[[Category:Virgo constellation]] [[Category:Bayer objects|Virginis, Beta]] [[Category:F-type main sequence stars]] [[Category:Stars with proper names]] [[cs:Zavijava]] [[de:Zavijava]] [[en:Beta Virginis]] [[es:Zavijava]] [[fr:Beta Virginis]] [[ko:자비야바]] [[it:Zavijava]] [[nl:Zavijah]] [[ja:おとめ座ベータ星]] [[ru:Завийява]] [[sk:Zavijava]]

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