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 52.41522s [1]
Declination +40° 10′ 56.5783″ [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 [5]   mas/yr
Dec.: −4.56±0.67 [5]   mas/yr
Parallax (π)1.9414 ± 0.0574  mas [1]
Distance 1,680 ± 50  ly
(520 ± 20  pc)
Absolute magnitude  (MV)−2.79 [6]
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
Radius 45.78+2.89
−3.69 [1]   R☉
Luminosity 1,094±43 [1]   L☉
Surface gravity (log g)1.78 [7]   cgs
Temperature 4,907+210
−149 [1]   K
Metallicity [Fe/H]+0.04 [7]   dex
Rotational velocity (v sin i)6.2 [8]  km/s
Other designations
BD+40° 1346, HD  36891, HIP  26363, SAO  40481
Database references
SIMBAD data

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. [9] In the same year, William P. Bidelman noted that the stellar spectrum was composite indicating a companion star. [10] Confirmation of spectroscopic binary status and a preliminary orbit was published in 1998 by R. Paul Butler, [11] a much more accurate orbit was published in 2015 by Roger Griffin. [4]

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<span class="mw-page-title-main">HD 22764</span> Double star; Camelopardalis

HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.

References

  1. 1 2 3 4 5 6 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. 1 2 3 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. 1 2 3 4 5 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. 1 2 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. S2CID   18759600. Vizier catalog entry
  6. ↑ 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 .
  7. 1 2 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 .
  8. ↑ 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: 97–98. Bibcode:2002A&A...395...97D. doi: 10.1051/0004-6361:20021214 .
  9. ↑ 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.
  10. ↑ 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.
  11. ↑ 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. S2CID   119678211.
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