Rho Andromedae

Rho Andromedae
Diagram showing star positions and boundaries of the Andromeda constellation and its surroundings


Location of ρ Andromedae (circled)

Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda
Right ascension 00h 21m 07.26951s[1]
Declination +37° 58′ 06.9804″[1]
Apparent magnitude (V) +5.19[2]
Characteristics
Spectral type F5 III[3]
U−B color index +0.039[2]
B−V color index +0.424[2]
Astrometry
Radial velocity (Rv)+8.2[4] km/s
Proper motion (μ) RA: +58.93[1] mas/yr
Dec.: -38.56[1] mas/yr
Parallax (π)20.60 ± 0.21[1] mas
Distance158 ± 2 ly
(48.5 ± 0.5 pc)
Absolute magnitude (MV)+1.73[4]
Details
Radius3.3[5] R☉
Luminosity20[6] L☉
Surface gravity (log g)3.84[7] cgs
Temperature6,471[7] K
Metallicity [Fe/H]–0.09[7] dex
Rotational velocity (v sin i)44[7] km/s
Age1.3[4] Gyr
Other designations
27 Andromedae, BD+37 45, FK5 1009, HD 1671, HIP 1686, HR 82, SAO 53828.[3]

Rho Andromedae (ρ And, ρ Andromedae) is the Bayer designation for a star in the northern constellation of Andromeda. It has an apparent visual magnitude of +5.19,[2] which, according to the Bortle Dark-Sky Scale, is bright enough to be seen with the naked eye from dark suburban skies. Based upon parallax measurements, this star is at a distance of approximately 158 light-years (48 parsecs) from Earth.[1]

The stellar classification of this star is F5 III,[3] indicating that it is in the giant stage of its stellar evolution. However, some sources list a classification of F5 IV,[3][6] suggesting that it may still be in the subgiant stage. The interferometry-measured angular diameter of this star is 0.626 mas,[6] which, at its estimated distance, equates to a physical radius of around 3.3 times the radius of the Sun.[5] The outer envelope is radiating around 20[6] times the luminosity of the Sun into space at an effective temperature of 6,471 K,[7] giving it the yellow-white hue of an F-type star.[8] It is about 1.3 billion years old.[4]

X-ray emissions were detected from this star during the EXOSAT mission.[9]

Naming

In Chinese, 天廄 (Tiān Jiù), meaning Celestial Stable, refers to an asterism consisting of ρ Andromedae, θ Andromedae and σ Andromedae. Consequently, ρ Andromedae itself is known as 天廄二 (Tiān Jiù èr, English: the Second Star of Celestial Stable.)[10]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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.
  2. ↑ 2.0 2.1 2.2 2.3 Breger, M. (March 1968), "UBV and narrow-band UVBY photometry of bright stars", Astronomical Journal 73: 84–85, Bibcode:1968AJ.....73...84B, doi:10.1086/110602.
  3. ↑ 3.0 3.1 3.2 3.3 "rho And -- Star", SIMBAD Astronomical Object Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-06-24.
  4. ↑ 4.0 4.1 4.2 4.3 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.
  5. ↑ 5.0 5.1 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
    \begin{align} 2\cdot R_* & = \frac{(48.5\cdot 0.626\cdot 10^{-3})\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 6.5\cdot R_{\bigodot} \end{align}
  6. ↑ 6.0 6.1 6.2 6.3 van Belle, G. T. et al. (May 2008), "The Palomar Testbed Interferometer Calibrator Catalog", The Astrophysical Journal Supplement Series 176 (1): 276–292, arXiv:0711.4194, Bibcode:2008ApJS..176..276V, doi:10.1086/526548.
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Balachandran, Suchitra (May 1, 1990). "Lithium depletion and rotation in main-sequence stars". Astrophysical Journal, Part 1 354: 310–332. Bibcode:1990ApJ...354..310B. doi:10.1086/168691.
  8. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16.
  9. ↑ Gondoin, P.; Mangeney, A.; Praderie, F. (March 1987), "Solar-type giants - New X-ray detections from EXOSAT observations", Astronomy and Astrophysics 174 (1-2): 187–196, Bibcode:1987A&A...174..187G.
  10. ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 18 日

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