Omicron Virginis
In this article, we will explore the topic of Omicron Virginis in depth, analyzing its origins, evolution, relevance today and possible future developments. Omicron Virginis is a topic widely discussed and studied in different areas, arousing the interest of academics, researchers, professionals and the general public. Throughout history, Omicron Virginis has played a crucial role in various contexts, significantly influencing society, culture and everyday life. Through a comprehensive analysis, we will address the different perspectives and approaches that have been used to understand Omicron Virginis, as well as the implications and challenges it currently poses. Through this article, we seek to offer a comprehensive vision of Omicron Virginis and its impact on society, promoting a constructive and enriching debate on this very relevant topic.
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Virgo |
| Right ascension | 12h 05m 12.54049s[1] |
| Declination | +08° 43′ 58.7498″[1] |
| Apparent magnitude (V) | 4.12[2] |
| Characteristics | |
| Evolutionary stage | Red-giant branch[3] |
| Spectral type | G8 IIIa CN-1Ba1CH1[4] |
| Astrometry | |
| Radial velocity (Rv) | −29.62[5] km/s |
| Proper motion (μ) | RA: −225.029 mas/yr[6] Dec.: +33.282 mas/yr[6] |
| Parallax (π) | 19.4936±0.1658 mas[6] |
| Distance | 167 ± 1 ly (51.3 ± 0.4 pc) |
| Absolute magnitude (MV) | +0.52[7] |
| Orbit[8] | |
| Primary | A |
| Companion | B |
| Period (P) | 50.70±3.30 yr |
| Semi-major axis (a) | 21.1±1.7 au |
| Eccentricity (e) | 0.12±0.04 |
| Inclination (i) | 147.8±1.6° |
| Longitude of the node (Ω) | 34±2° |
| Periastron epoch (T) | 2460663±500 |
| Argument of periastron (ω) (secondary) | 180±17° |
| Details[5] | |
| A | |
| Mass | 2.7±0.2[8] M☉ |
| Radius | 11.2±0.3[9] R☉ |
| Luminosity | 57 L☉ |
| Surface gravity (log g) | 3.17 cgs |
| Temperature | 5,107 K |
| Metallicity | −0.30 dex |
| Rotational velocity (v sin i) | 2.23 km/s |
| Age | 0.88 Gyr |
| B | |
| Mass | 0.94±0.14[8] M☉ |
| Other designations | |
| 9 Virginis, ο Vir, BD+09°2583, FK5 450, GJ 3703, HD 104979, HIP 58948, HR 4608, SAO 119213 | |
| Database references | |
| SIMBAD | data |
Omicron Virginis (ο Vir, ο Virginis) is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of +4.12.[7] Based upon parallax measurements, it is at a distance of 163 light years.
Characteristics
The components are orbiting around the system's center of mass at a period of 50.7 years, and a nearly circular orbit with eccentricity 0.12 and an average separation of 21 astronomical units.[8]
The primary star is a G-type giant with a stellar classification of G8 IIIa CN-1Ba1CH1.[4] This indicates that it is a Barium star. It is around 11 times larger than the Sun.[9] Although it is slightly cooler, it is radiating about 57 times the luminosity of the Sun. It is over twice as massive as the Sun and is around a billion years old.[5] A simplified statistical analysis suggests that ο Virginis is likely to be a red-giant branch star fusing hydrogen in a shell around an inert helium core, but there is about a 22% chance that it is a horizontal branch star fusing helium in its core.[10]
The secondary is a white dwarf with 94% of the Sun's mass. It contamined the surface of the giant primary with s-process elements when it was on the asymptotic giant branch, causing it to be a Barium star.[8] It may also explain the unexpected SiIV emission flux coming from Omicron Virginis.[11]
References
- ^ a b van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
- ^ Mallik, Sushma V. (December 1999). "Lithium abundance and mass". Astronomy and Astrophysics. 352: 495–507. Bibcode:1999A&A...352..495M.
- ^ Laney, C. D.; Joner, M. D.; Pietrzyński, G. (2012). "A new Large Magellanic Cloud K-band distance from precision measurements of nearby red clump stars". Monthly Notices of the Royal Astronomical Society. 419 (2): 1637. arXiv:1109.4800. Bibcode:2012MNRAS.419.1637L. doi:10.1111/j.1365-2966.2011.19826.x.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- ^ a b c Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
- ^ a b Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Takeda, Yoichi; et al. (August 2008). "Stellar Parameters and Elemental Abundances of Late-G Giants". Publications of the Astronomical Society of Japan. 60 (4): 781–802. arXiv:0805.2434. Bibcode:2008PASJ...60..781T. doi:10.1093/pasj/60.4.781.
- ^ a b c d e Escorza, A.; De Rosa, R. J. (March 2023). "Barium and related stars, and their white-dwarf companions: III. The masses of the white dwarfs". Astronomy & Astrophysics. 671: A97. arXiv:2301.04232. Bibcode:2023A&A...671A..97E. doi:10.1051/0004-6361/202244782. ISSN 0004-6361.
- ^ a b Baines, Ellyn K.; Clark, James H.; Kingsley, Bradley I.; Schmitt, Henrique R.; Stone, Jordan M. (2025-05-07). "Vintage NPOI: New and Updated Angular Diameters for 145 Stars". The Astronomical Journal. 169 (6): 293. arXiv:2506.02912. Bibcode:2025AJ....169..293B. doi:10.3847/1538-3881/adc930. ISSN 1538-3881.
- ^ Reffert, Sabine; Bergmann, Christoph; Quirrenbach, Andreas; Trifonov, Trifon; Künstler, Andreas (2015). "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity". Astronomy & Astrophysics. 574: A116. arXiv:1412.4634. Bibcode:2015A&A...574A.116R. doi:10.1051/0004-6361/201322360. hdl:10722/215277. S2CID 59334290.
- ^ Böhm-Vitense, Erika; Carpenter, Kenneth; Robinson, Richard; Ake, Tom; Brown, Jeffery (2000). "Do All BA II Stars Have White Dwarf Companions?". The Astrophysical Journal. 533 (2): 969. Bibcode:2000ApJ...533..969B. doi:10.1086/308678.
