Beta Virginis
 | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 11h 50m 41.71824s[1] |
| Declination | +1° 45′ 52.9910″[1] |
| Apparent magnitude (V) | 3.604[2] |
| Characteristics | |
| Spectral type | F9 V[3] |
| U−B color index | +0.090[2] |
| B−V color index | +0.553[2] |
| Astrometry | |
| Radial velocity (Rv) | +4.1[4] km/s |
| Proper motion (μ) | RA: +740.23[1] mas/yr Dec.: -270.43[1] mas/yr |
| Parallax (π) | 91.50 ± 0.22 mas[1] |
| Distance | 35.65 ± 0.09 ly (10.93 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.41[4] |
| Details | |
| Mass | 1.25[5] M☉ |
| Radius | 1.681 ± 0.008[6] R☉ |
| Luminosity | 3.572 ± 0.052[6] L☉ |
| Surface gravity (log g) | 4.25[7] cgs |
| Temperature | 6,132 ± 26[6] K |
| Metallicity [Fe/H] | 0.20[7] dex |
| Rotational velocity (v sin i) | 4.3[5] km/s |
| Age | 2.9 ± 0.3[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| ARICNS | data |
Beta Virginis (β Vir, β Virginis) is a star in the constellation Virgo. It has the traditional names Zavijava (also Zavijah) and Alaraph.[9] 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).[7]
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,[dubious – discuss] as it was close to the Sun.
Etymology
The medieval name Zavijava (Zavijah, Zavyava, Zawijah) is from the Arabic زاوية العواء zāwiyat al-cawwa’ "Corner of the barking (dog)". Another name was Alaraph.
Hunt for substellar objects
According to Nelson & Angel (1998),[10] Beta Virginis could host two or three jovian planets 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[11] 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 [12] with masses between 0.16 and 4.2 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.
In fiction
- Beta Virginis was the original destination of the Bussard scoopship Leonora Christine in Poul Anderson's Tau Zero.
References
- ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
{{citation}}: Unknown parameter|month=ignored (help) - ^ a b c Gutierrez-Moreno, Adelina; Moreno, Hugo (1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168
{{citation}}: Unknown parameter|month=ignored (help) - ^ Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics, 11 (1): 29, Bibcode:1973ARA&A..11...29M, doi:10.1146/annurev.aa.11.090173.000333
- ^ a b c Holmberg, J.; Nordström, B.; Andersen, J. (2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191
{{citation}}: Unknown parameter|month=ignored (help) - ^ a b Carrier, F.; Eggenberger, P.; D'Alessandro, A.; Weber, L. (2005). "Solar-like oscillations in the F9 V β Virginis". New Astronomy. 10 (4): 315–323. arXiv:astro-ph/0502014. Bibcode:2005NewA...10..315C. doi:10.1016/j.newast.2004.11.003. Retrieved 2007-06-05.
- ^ a b c Boyajian, Tabetha S.; et al. (2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal, 746 (1): 101, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101
{{citation}}: Unknown parameter|month=ignored (help). See Table 10. - ^ a b c Gehren, T. (1978). "On the chemical composition and age of Beta VIR". Astronomy and Astrophysics. 65 (3): 427–433. Bibcode:1978A&A....65..427G.
- ^ "LHS 2465 -- High proper-motion Star", SIMBAD Astronomical Object Database, Centre de Données astronomiques de Strasbourg, retrieved 2012-03-20
- ^ Atlas of the Heavens, part II, catalogue, Antonín Bečvář
- ^ The Range of Masses and Periods Explored by Radial Velocity Searches for Planetary Companions
- ^ A search for substellar companions to southern solar-type stars
- ^ Detection Limits from the McDonald Observatory Planet Search Program
External links
- Kaler, Jim (2007). "Zavijava". Stars: Portraits of Stars and their Constellations. Retrieved 2007-06-06.
- "Zavijah". Alcyone. Retrieved 2007-06-06.
