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Binary star system in the constellation Andromeda
Omega Andromedae (ω And, ω Andromedae) is the Bayer designation for a slowly co-rotating[failed verification binary star system[ 9] northern constellation of Andromeda . Parallax measurements made during the Gaia light-years (28.8 parsecs ) from Earth . Its apparent visual magnitude is +4.83,[ 2]
The primary component has a stellar classification of F5 IVe.[ 4] 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] angular diameter of the primary star is 0.70 ± 0.03 mas .[ 10] that of the Sun .[ 6] solar luminosity from its outer atmosphere at an effective temperature of K [ 7] 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 arcsecond .[ 9] [ 5]
^ a b c d e Brown, A. G. A. ; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties" . Astronomy & Astrophysics 649 : A1. arXiv :2012.01533 Bibcode :2021A&A...649A...1G . doi :10.1051/0004-6361/202039657 S2CID 227254300 . (Erratum: doi :10.1051/0004-6361/202039657e ) . Gaia EDR3 record for this source at VizieR .^ 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): 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 Birkhäuser , ISBN 3-540-29692-1 * ) is given by:
2
⋅
R
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28.6
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0.70
⋅
10
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3
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AU
0.0046491
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R
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4.31
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R
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{\displaystyle {\begin{aligned}2\cdot R_{*}&={\frac {(28.6\cdot 0.70\cdot 10^{-3})\ {\text{AU}}}{0.0046491\ {\text{AU}}/R_{\bigodot }}}\\&\approx 4.31\cdot R_{\bigodot }\end{aligned}}}
^ 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 . ^ [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 18, 2012, retrieved 2012-01-16 .
