44 Andromedae

44 Andromedae
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Andromeda
Right ascension 01h 10m 18.74041s[1]
Declination +42° 04′ 53.3100″[1]
Apparent magnitude (V) 5.67[2]
Characteristics
Spectral type F8 V[3]
U−B color index +0.12[2]
B−V color index +0.59[2]
Astrometry
Radial velocity (Rv)−14.2±0.2[4] km/s
Proper motion (μ) RA: −135.569(38)[1] mas/yr
Dec.: −41.790(30)[1] mas/yr
Parallax (π)18.8145 ± 0.0376 mas[1]
Distance173.4 ± 0.3 ly
(53.2 ± 0.1 pc)
Absolute magnitude (MV)+2.07[5]
Details[3]
Mass1.64 M☉
Radius3.58±0.19 R☉
Luminosity12.9 L☉
Surface gravity (log g)3.78±0.07 cgs
Temperature6,028±32 K
Metallicity [Fe/H]−0.01±0.04 dex
Rotation15.2 d
Rotational velocity (v sin i)11.6±0.8 km/s
Age2.59 Gyr
Other designations
44 And, BD+41° 219, FK5 2075, GC 1410, GJ 53.4, HD 6920, HIP 5493, HR 340, SAO 36984, PPM 43709[6]
Database references
SIMBADdata

44 Andromedae is a single,[7] yellow-white hued star in the northern constellation of Andromeda.[6] 44 Andromedae is the Flamsteed designation. It has an apparent visual magnitude of approximately 5.67,[2] which indicates it is a dim star that is just visible to the naked eye on a dark night. The annual parallax shift as measured by the Hipparcos spacecraft is 18.8145 mas,[1] which yields a distance estimate of around 173 light years. It is moving closer to the Sun with a radial velocity of −14 km/s.[4]

This star has been assigned a stellar classification of F8 V,[3] which indicates it is an ordinary F-type main-sequence star. However, Gray et al. (2001) gave it a class of F9 IV, suggesting it is instead a subgiant star that is evolving away from the main sequence as the hydrogen fuel at its core becomes exhausted.[8] It is an estimated 2.6 billion years old and is rotating with a period of 15.2 days. The star has 1.64 times the mass of the Sun and 3.6 times the Sun's radius. It is radiating 13 times the Sun's luminosity from its photosphere at an effective temperature of 6,028 K.[3] It appears overluminous for a star of its type which may indicate the presence of a bright companion, but no radial velocity variation has been detected.[9]

  1. ^ a b c d e f Cite error: The named reference Gaia EDR3 was invoked but never defined (see the help page).
  2. ^ a b c d Guetter, H. H.; Hewitt, A. V. (June 1984), "Photoelectric UBV photometry for 317 PZT and VZT stars", Publications of the Astronomical Society of the Pacific, 96: 441–443, Bibcode:1984PASP...96..441G, doi:10.1086/131362.
  3. ^ a b c d Marsden, S. C.; et al. (November 2014), "A BCool magnetic snapshot survey of solar-type stars", Monthly Notices of the Royal Astronomical Society, 444 (4): 3517–3536, arXiv:1311.3374, Bibcode:2014MNRAS.444.3517M, doi:10.1093/mnras/stu1663, S2CID 53988884.
  4. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ HD 6920, database entry, The Geneva-Copenhagen Survey of Solar neighbourhood, J. Holmberg et al., 2007, CDS ID V/117A. Accessed on line November 19, 2008.
  6. ^ a b "44 And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-12-28.
  7. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  8. ^ Gray, R. O.; Napier, M. G.; Winkler, L. I. (April 2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars", The Astronomical Journal, 121 (4): 2148–2158, Bibcode:2001AJ....121.2148G, doi:10.1086/319956.
  9. ^ Griffin, R. F.; Suchkov, A. A. (July 2003), "The Nature of Overluminous F Stars Observed in a Radial-Velocity Survey", The Astrophysical Journal Supplement Series, 147 (1): 103–144, Bibcode:2003ApJS..147..103G, doi:10.1086/367855.