Omega Andromedae
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Andromeda |
Right ascension | 01h 27m 39.38177s[1] |
Declination | +45° 24′ 24.0727″[1] |
Apparent magnitude (V) | +4.83[2][3] |
Characteristics | |
Spectral type | F5 IVe[4] or F3 V + F5 V[5] |
U−B color index | +0.00[3] |
B−V color index | +0.42[3] |
Astrometry | |
Radial velocity (Rv) | +14.7[2] km/s |
Proper motion (μ) | RA: +356.99[1] mas/yr Dec.: –109.40[1] mas/yr |
Parallax (π) | 34.94 ± 0.31 mas[1] |
Distance | 93.3 ± 0.8 ly (28.6 ± 0.3 pc) |
Absolute magnitude (MV) | +2.57[2] |
Details | |
ω And A | |
Mass | 0.963±0.049[5] M☉ |
Radius | 2.2[6] R☉ |
Luminosity | 7.1[7] L☉ |
Temperature | 6,628[7] K |
Metallicity [Fe/H] | –0.16[2] dex |
Rotational velocity (v sin i) | 57.1[8] km/s |
Age | 2.1[2] Gyr |
ω And B | |
Mass | 0.860±0.051[5] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
Omega Andromedae (ω And, ω Andromedae) is the Bayer designation for a slowly co-rotating binary star system[9] in the northern constellation of Andromeda. Parallax measurements made during the Hipparcos mission make this system to be approximately 93.3 light-years (28.6 parsecs) from Earth. Its apparent visual magnitude is +4.83,[2] which makes it bright enough to be seen with the naked eye.
The primary component has a stellar classification of F5 IVe.[4] The IV luminosity class indicates that it is probably a subgiant star that is in the process of evolving away from the main sequence as the supply of hydrogen at its core depletes. However, Abt (1985) gives a classification of F3 V, suggesting it is an F-type main sequence star.[5] The measured angular diameter of the primary star is 0.70 ± 0.03 mas.[10] At the system's estimated distance this yields a size of about 2.2 times that of the Sun.[6] It is emitting about seven times solar luminosity from its outer atmosphere at an effective temperature of 6,628 K.[7] This heat gives it the yellow-white hued glow of an F-type star.[11]
In 2008, the companion star was resolved using adaptive optics at the Lick Observatory. Later observations showed the magnitude difference between the two stars is 3.65 ± 0.03 and they are separated by 0.669 arcseconds.[9] Abt (1985) lists the class as F5 V.[5]
References
- ^ a b c d e van Leeuwen, F. (November 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.
- ^ a b c d e f Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418: 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
- ^ a b c Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J.
- ^ a b c "ome And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-06-26.
{{cite web}}
: CS1 maint: postscript (link) - ^ a b c d e Farrington, C. D.; et al. (September 2014), "Separated Fringe Packet Observations with the CHARA Array. II. ω Andromeda, HD 178911, and ξ Cephei", The Astronomical Journal, 148 (3): 8, arXiv:1407.0639, Bibcode:2014AJ....148...48F, doi:10.1088/0004-6256/148/3/48, S2CID 12909818, 48.
- ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
- ^ a b c do Nascimento, J. D. Jr.; et al. (July 2003), "On the link between rotation, chromospheric activity and Li abundance in subgiant stars", Astronomy and Astrophysics, 405 (2): 723–731, arXiv:astro-ph/0307196, Bibcode:2003A&A...405..723D, doi:10.1051/0004-6361:20030633, S2CID 1106754.
- ^ Schröder, C.; Reiners, A.; Schmitt, J. H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377.[permanent dead link]
- ^ a b Gladysz, Szymon; Christou, Julian C. (June 2009), "Reference-Less Detection, Astrometry, and Photometry of Faint Companions with Adaptive Optics", The Astrophysical Journal, 698 (1): 28–42, arXiv:0805.1870, Bibcode:2009ApJ...698...28G, doi:10.1088/0004-637X/698/1/28, S2CID 44505644.
- ^ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 10, 2012, retrieved 2012-01-16.