Astronomy:O Velorum
  | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vela |
| Right ascension | 09h 43m 42.24s[citation needed] |
| Declination | −53° 53′ 28.6″ |
| Apparent magnitude (V) | +5.55[citation needed] |
| Characteristics | |
| Spectral type | A0V[citation needed] |
| Astrometry | |
| Radial velocity (Rv) | 10.0[citation needed] km/s |
| Proper motion (μ) | RA: −67.451±0.069 mas/yr Dec.: 33.101±0.058 mas/yr |
| Parallax (π) | 9.3543 ± 0.0513[citation needed] mas |
| Distance | 349 ± 2 ly (106.9 ± 0.6 pc) |
| Absolute magnitude (MV) | +0.45[citation needed] |
| Details | |
| Mass | 2.70±0.03 M☉ |
| Radius | 2.7 R☉ |
| Luminosity | 77 L☉ |
| Surface gravity (log g) | 4.0[citation needed] cgs |
| Temperature | 10,023[citation needed] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
O Velorum (O Vel / HD 84461)[1][2] is a star in the constellation of Vela, one of the parts into which the constellation Argo Navis was divided. It has an apparent magnitude +5.55 and the "O" refers to its Bayer designation.
Characteristics
O Velorum is classified as a white subgiant of spectral type A0IV,[3] [1] although a recent study indicates that it has not yet left the main sequence and that it still has 31% of its way through that stage.[4] Given its classification as a subgiant, it would be a star similar to Alhena (γ Geminorum), but its luminosity —77 times greater than that of the Sun— is more comparable to that of an A0 main sequence star such as Phecda (γ Ursae Majoris), Sadachbia (γ Aquarii) or ε Herculis.
O Velorum has an effective temperature of 10,023 kelvins (10,350 according to another source) of 10,350 K.[5] and a mass of 2.70 ± 0.03 solar masses.[4] Its radius is estimated to be 2.7 times larger than the Sun's radius[6] and it spins on its axis with a rotation speed of at least 40 km/s.
References
- ↑ 1.0 1.1 1.2 HR 3875 -- Star (SIMBAD)
- ↑ "O Vel (Alcyone)". Archived from the original on March 4, 2016. https://web.archive.org/web/20160304204525/http://www.alcyone.de/cgi-bin/search.pl?object=HR3875. Retrieved October 21, 2012.
- ↑ Cite error: Invalid
<ref>tag; no text was provided for refs namedXHIP - ↑ 4.0 4.1 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy and Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. A120. Bibcode: 2012A&A...537A.120Z. http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2012A%26A...537A.120Z&db_key=AST.
- ↑ Castelli, F.; Hubrig, S. (2004). "The Ca II infrared triplet as indicator of anomalous Ca isotopic mixture in HgMn stars". Astronomy and Astrophysics 421: L1–L4. doi:10.1051/0004-6361:20040164. L1-L4. Bibcode: 2004A&A...421L...1C. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2004A%26A...421L...1C&db_key=AST&nosetcookie=1.
- ↑ HD 84461 (CADARS)
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