HD 2421

HD 2421 is a double-lined spectroscopic binary with a class A main-sequence primary and a class F main-sequence secondary[4] in the constellation Andromeda. Its apparent magnitude is 5.18 and it is approximately 290 light years away based on parallax.[1]

HD 2421
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda
Right ascension  0h 28m 13.6588s[1]
Declination +44° 23′ 40.1085″[1]
Apparent magnitude (V) 5.173[2]
Characteristics
Spectral type A2V[3]/F2V[4]
Astrometry
Radial velocity (Rv)2.0±0.9[5] km/s
Proper motion (μ) RA: 82.361±0.197[1] mas/yr
Dec.: −16.244±0.119[1] mas/yr
Parallax (π)11.2634 ± 0.1621[1] mas
Distance290 ± 4 ly
(89 ± 1 pc)
Orbit[6]
PrimaryHD 2421A
CompanionHD 2421B
Period (P)3.95529±0.00003 d
Eccentricity (e)0.135±0.011
Periastron epoch (T)2448523.14±0.04
Argument of periastron (ω)
(secondary)		280±4°
Argument of periastron (ω)
(primary)		91±8°
Semi-amplitude (K1)
(primary)		49.1±0.6 km/s
Semi-amplitude (K2)
(secondary)		81.1±1.0 km/s
Other designations
BD+43° 92, HD 2421, HIP 2225, HR 104, SAO 36390[7]
Database references
SIMBADdata

Binary system

The binary has a period of 3.96 days and an eccentricity of 0.135. The variable radial velocity was first reported by Robert Horace Baker in 1909 and the first orbit computed by Stella Udick in 1912.[8] A refined orbit was published in 1993 resulting in updated orbital parameters, and in the assessment of a period shift with respect to the 1912 observations.[6]

gollark: ++help
gollark: ++deploy apiosystem 1¹¹3\\4
gollark: ++exec```pythonfrom itertools import chainÜ = ["apioforms", "are", "apioforms", "and", "apiohazards"]def þ(ŧ): ø = [""] for Ö in ŧ: ŋ = [] for Ä in Ö: for Ø in ø: ŋ.append(Ø + Ä) ø = ŋ return øprint(" ".join(þ(Ü)))```
gollark: ++exec```pythonfrom itertools import chainÜ = ["ðdDÐ", "ÆÄAaæä", "włWŁ", "nN", "ØOÖøoö", "§sßs"]def þ(ŧ): ø = [""] for Ö in ŧ: ŋ = [] for Ä in Ö: for Ø in ø: ŋ.append(Ø + Ä) ø = ŋ return øprint(" ".join(þ(Ü)))```
gollark: ++exec```pythonfrom itertools import chainÜ = ["ðdDÐ", "ÆÄAaæä", "włWŁ", "nN", "ØOÖøoö", "§sßs"]def þ(ŧ): ø = [""] for Ö in ŧ: ŋ = [] for Ä in Ö: for Ø in ø: ŋ.append(Ø + Ä) ø = ŋ return øprint("".join(þ(Ü)))```

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy & Astrophysics, 355: L27–L30, Bibcode:2000A&A...355L..27H.
  3. Cowley, A.; et al. (1969). "A study of the bright stars. I. A catalogue of spectral classifications". The Astronomical Journal. 74: 375–406. Bibcode:1969AJ.....74..375C. doi:10.1086/110819.
  4. Adelman, Saul J.; et al. (2015). "Elemental Abundance Analyses with DAO Spectrograms. XXXVIII. The SB2 Stars HR 104 (A2 V) and θ Aql (B9.5 III)". Publications of the Astronomical Society of the Pacific. 127 (952): 509–515. Bibcode:2015PASP..127..509A. doi:10.1086/682075.
  5. Database entry, General catalogue of stellar radial velocities. (Wilson, 1953), R.E. Wilson, CDS ID III/21 Accessed on line 2018-12-03.
  6. Hill, Graham; et al. (1993). "The double-lined spectroscopic binary HR 104". Publications of the Astronomical Society of the Pacific. 105: 748–750. Bibcode:1993PASP..105..748H. doi:10.1086/133225.
  7. "HD 2421". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-03.
  8. Udick, Stella (1912). "The orbit of B. D. + 43° 92". Publications of the Allegheny Observatory of the University of Pittsburgh. 2 (18): 191–196. Bibcode:1912PAllO...2..191U.
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