HR 1884

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HR 1884
Auriga constellation map.svg
Red circle.svg
Location of HR 1884 (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Auriga
Right ascension  05h 36m 52.417s[1]
Declination +40° 10′ 56.55″[1]
Apparent magnitude (V) 6.08[2]
Characteristics
Spectral type G3 Ib[3] + B7 V?[4]
U−B color index 0.69[2]
B−V color index 1.03[2]
Astrometry
Radial velocity (Rv)−12.06±0.03[4] km/s
Proper motion (μ) RA: −2.99±1.03[1] mas/yr
Dec.: −4.56±0.67[1] mas/yr
Parallax (π)−0.75 ± 0.93[1] mas
Distance1,200[4] pc
Absolute magnitude (MV)−2.79[5]
Orbit[4]
Period (P)7829.3±1.4 days
Eccentricity (e)0.8867±0.0006
Periastron epoch (T)54417.21±0.22
Argument of periastron (ω)
(secondary)
250.61±0.20°
Semi-amplitude (K1)
(primary)
21.77±0.04 km/s
Details
Surface gravity (log g)1.78[6] cgs
Temperature5,082[5] K
Metallicity [Fe/H]+0.04[6] dex
Rotational velocity (v sin i)6.2[7] km/s
Other designations
BD+40° 1346, HD 36891, HIP 26363
Database references
SIMBADdata

HR 1884 is a spectroscopic binary star in the constellation Auriga. The primary is a G type supergiant star while the secondary is probably a B type main sequence star.[4]

The possible spectroscopic binary nature of the star was first noted in 1983 by Gilbert Burki and Michel Mayor in a paper on the rate of binaries among supergiant stars.[8] In the same year William P. Bidelman noted that the stellar spectrum was composite indicating a companion star.[9] Confirmation of spectroscopic binary status and a preliminary orbit was published in 1998 by R. Paul Butler,[10] a much more accurate orbit was published in 2015 by Roger Griffin.[4]

References[edit]

  1. ^ a b c d e 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. Vizier catalog entry
  2. ^ a b c Argue, A. N. (1966). "UBV photometry of 550 F, G and K type stars". Monthly Notices of the Royal Astronomical Society. 133 (4): 175–493. Bibcode:1966MNRAS.133..475A. doi:10.1093/mnras/133.4.475.
  3. ^ Bidelman, William P. (1957). "Spectral Classification of Stars Noted on Case Objective-Prism Plates. I". Publications of the Astronomical Society of the Pacific. 69 (407): 147–152. Bibcode:1957PASP...69..147B. doi:10.1086/127034.
  4. ^ a b c d e f Griffin, R. F. (2015). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 241: HR 1884, HD 174103, HD 182563, and HR 8442, with a note on zeta Cephei". The Observatory. 135: 71–95. Bibcode:2015Obs...135...71G.
  5. ^ a b Kovtyukh, V. V.; Chekhonadskikh, F. A.; Luck, R. E.; Soubiran, C.; Yasinskaya, M. P.; Belik, S. I. (2010). "Accurate luminosities for F-G supergiants from FeII/FeI line depth ratios". Monthly Notices of the Royal Astronomical Society. 408 (3): 1568. Bibcode:2010MNRAS.408.1568K. doi:10.1111/j.1365-2966.2010.17217.x.
  6. ^ a b Luck, R. Earle (2014). "Parameters and Abundances in Luminous Stars". The Astronomical Journal. 147 (6): 137. Bibcode:2014AJ....147..137L. doi:10.1088/0004-6256/147/6/137.
  7. ^ De Medeiros, J. R.; Udry, S.; Burki, G.; Mayor, M. (2002). "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars". Astronomy and Astrophysics. 395: 97. Bibcode:2002A&A...395...97D. doi:10.1051/0004-6361:20021214.
  8. ^ Burki, G.; Mayor, M. (1983). "Nineteen new spectroscopic binaries and the rate of binary stars among F-M supergiants". Astronomy and Astrophysics. 124 (2): 256–266. Bibcode:1983A&A...124..256B.
  9. ^ Bidelman, W. P. (1983). "Objective-prism discoveries in the northern sky. I". Astronomical Journal. 88: 1182–1186. Bibcode:1983AJ.....88.1182B. doi:10.1086/113408.
  10. ^ Butler, R. Paul (1998). "A Precision Velocity Study of Photometrically Stable Stars in the Cepheid Instability Strip". Astrophysical Journal. 494 (1): 342–365. Bibcode:1998ApJ...494..342B. CiteSeerX 10.1.1.37.7095. doi:10.1086/305195.