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70 Pegasi

70 Pegasi
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pegasus
Right ascension 23h 29m 09.29698s[1]
Declination +12° 45′ 37.9918″[1]
Apparent magnitude (V) 4.56[2]
Characteristics
Spectral type G8 IIIa[3]
B−V color index 0.940[2]
Astrometry
Radial velocity (Rv)−16.88±0.43[4] km/s
Proper motion (μ) RA: +61.40[1] mas/yr
Dec.: +24.82[1] mas/yr
Parallax (π)18.65 ± 0.78 mas[1]
Distance175 ± 7 ly
(54 ± 2 pc)
Absolute magnitude (MV)0.90[5]
Orbit[6]
Period (P)941.03±0.12 d
Eccentricity (e)0.713±0.006
Argument of periastron (ω)
(secondary)		57.0±1.2°
Semi-amplitude (K1)
(primary)		3.16±0.04 km/s
Details[4]
70 Peg A
Mass2.49±0.06 M☉
Radius8.44±0.37 R☉
Luminosity47.9+4.6
−4.2 L☉
Surface gravity (log g)2.92±0.05 cgs
Temperature5,032±15 K
Metallicity [Fe/H]0.05±0.03 dex
Rotational velocity (v sin i)3.6[7] km/s
Age590±40 Myr
Other designations
70 Peg, BD+11° 5009, FK5 885, HD 221115, HIP 115919, HR 8923, SAO 108638[8]
Database references
SIMBADdata

70 Pegasi is a binary star[6] system in the northern constellation Pegasus. It is a faint star, visible to the naked eye under good seeing conditions, with an apparent visual magnitude of 4.56.[2] The measured annual parallax shift measured from Earth's orbit is 18.65 mas,[1] yielding a distance estimate of around 175 light years. The visual magnitude of the star is diminished by an extinction of 0.07±0.02 due to interstellar dust. It is moving closer to the Sun with a radial velocity of −17 km/s.[4]

This is a single-lined spectroscopic binary with an orbital period of 2.58 years (941 days) and a high eccentricity of 0.713.[6] The visible component has a stellar classification of G8 IIIa,[3] indicating it is an evolved G-type giant star. It is a probable red clump star, which would mean it is generating energy through helium fusion at its core.[9] The star has 2.5 times the mass of the Sun and has expanded to more than 8 times the Sun's radius. It is radiating about 48 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 5,032 K.[4]

The secondary is most likely a low mass main sequence star with no more than 0.4 times the mass of the Sun.[6]

  1. ^ a b c d e f Cite error: The named reference vanLeeuwen2007 was invoked but never defined (see the help page).
  2. ^ a b c Cite error: The named reference Luck2015 was invoked but never defined (see the help page).
  3. ^ a b Cite error: The named reference perkins1989 was invoked but never defined (see the help page).
  4. ^ a b c d Cite error: The named reference Maldonado2013 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  6. ^ a b c d Cite error: The named reference Griffin2009 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference Massarotti2008 was invoked but never defined (see the help page).
  8. ^ "70 Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-20.
  9. ^ Cite error: The named reference Puzeras2010 was invoked but never defined (see the help page).

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