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Omega Andromedae

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Binary star system in the constellation Andromeda
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ω Andromedae
Location of χ Andromedae (circled)
Observation data
Epoch J2000Equinox ICRS
Constellation Andromeda
Right ascension 01h 27m 39.38072s[1]
Declination +45°24′24.0651′′[1]
Apparentmagnitude(V) +4.83[2] [3]
Characteristics
Spectraltype F5IVe[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:357.564(127)[1] mas/yr
Dec.:−110.039(118)[1] mas/yr
Parallax (π)34.7332±0.1341mas [1]
Distance 93.9 ± 0.4ly
(28.8 ± 0.1pc)
Absolutemagnitude(MV)+2.57[2]
Orbit [5]
Period (P)254.9 days
Semi-major axis (a)0.038±0.001′′
Eccentricity (e)0.142±0.012
Inclination (i)62.49±2.10°
Semi-amplitude (K1)
(primary)		17.54±0.30km/s
Semi-amplitude (K2)
(secondary)		19.62±0.30km/s
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 (vsini)57.1[8] km/s
Age 2.1[2] Gyr
ω And B
Mass 0.860±0.051[5] M☉
Other designations
48Andromedae, BD+44°307, FK51040, HD8799, HIP6813, HR417, SAO37228, PPM44006[4]
Database references
SIMBAD data

Omega Andromedae (ω And, ω Andromedae) is a binary star system[9] in the northern constellation of Andromeda. Parallax measurements made during the Gaia mission make this system to be approximately 93.9 light-years (28.8 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 6,628K .[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 arcsecond.[9] Abt (1985) lists the class as F5 V.[5]

References

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  1. 1 2 3 4 5 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.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 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.
  4. 1 2 3 "ome And", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2012年06月26日.
  5. 1 2 3 4 5 6 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.
  6. 1 2 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:
    2 ⋅ R ∗ = ( 28.6 ⋅ 0.70 ⋅ 10 − 3 ) AU 0.0046491 AU / R ⨀ ≈ 4.31 ⋅ R ⨀ {\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}}} {\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}}}
  7. 1 2 3 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.
  8. ↑ Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo", Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377 .
  9. 1 2 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.
  10. ↑ 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 .
  11. ↑ "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年01月16日.
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