HR 7955

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HR 7955
Observation data
Epoch J2000      Equinox J2000
Constellation Cepheus
Right ascension 20h 45m 21.12879s[1]
Declination +57° 34′ 47.0080″[1]
Apparent magnitude (V) 4.51[2]
Spectral type F8IV-V + F9IV-V[2]
Radial velocity (Rv)-32.82 ± 0.04[3] km/s
Proper motion (μ) RA: -62.32[1] mas/yr
Dec.: -236.00[1] mas/yr
Parallax (π)36.64 ± 0.48[1] mas
Distance89 ± 1 ly
(27.3 ± 0.4 pc)
Period (P)1.4331 ± 0.0003 yr
Semi-major axis (a)0.065 ± 0.001″
Eccentricity (e)0.551 ± 0.004
Inclination (i)24.53 ± 3.13°
Longitude of the node (Ω)325.21 ± 1.05°
Periastron epoch (T)B 1996.335 ± 0.0017
Argument of periastron (ω)
68.86 ± 0.76°
HR 7955 A
Mass1.071 ± 0.037 M
HR 7955 B
Mass1.047 ± 0.037 M
Other designations
BD+57° 2240, FK5 782, GJ 9706, HD 198084, HIP 102431, HR 7955, SAO 32862[4]
Database references

HR 7955 is a binary star in the constellation Cepheus. Its apparent magnitude is 4.51.[2] It is located 89 light-years (27.3 parsecs) away from the Solar System, based on parallax.[1] The two components, both late F-type main-sequence stars or subgiant stars, orbit each other every 1.4331 years.[2]


  1. 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (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 2.4 2.5 Farrington, C. D; Ten Brummelaar, T. A; Mason, B. D; Hartkopf, W. I; McAlister, H. A; Raghavan, D; Turner, N. H; Sturmann, L et al. (2010). "Separated Fringe Packet Observations with the CHARA Array. I. Methods and New Orbits for χ Draconis, HD 184467, and HD 198084". The Astronomical Journal 139 (6): 2308. Bibcode 2010AJ....139.2308F. doi:10.1088/0004-6256/139/6/2308.
  3. Pourbaix, D. et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics 424 (2): 727. arXiv:astro-ph/0406573. Bibcode 2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
  4. Lua error in Module:Citation/CS1 at line 379: attempt to call method 'match' (a nil value).

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