HD 32188

Last updated
HD 32188
Auriga constellation map.svg
Red circle.svg
Location of HD 32188 (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Auriga
Right ascension 05h 03m 18.63675s [1]
Declination +41° 26′ 29.9355″ [1]
Apparent magnitude  (V)6.08 [2]
Characteristics
Spectral type A2IIIshe [3]
U−B color index +0.22 [2]
B−V color index +0.21 [2]
Variable type Suspected [4]
Astrometry
Radial velocity (Rv)−0.7 [5]  km/s
Proper motion (μ)RA: −0.44 [6]   mas/yr
Dec.: −1.89 [6]   mas/yr
Parallax (π)1.0886 ± 0.0733  mas [1]
Distance 3,000 ± 200  ly
(920 ± 60  pc)
Absolute magnitude  (MV)−2.87 [3]
Details
Radius 30.39+1.63
−0.99 [1]   R☉
Luminosity 2,428±207 [1]   L☉
Temperature 7,350+123
−189 [1]   K
Rotational velocity (v sin i)23 [7]  km/s
Other designations
NSV  1810, BD+41°1044, HD  32188, HIP  23511, HR  1615, SAO  39979 [8]
Database references
SIMBAD data

HD 32188 is suspected variable star [4] in the northern constellation of Auriga, and is positioned roughly in between Eta and Zeta Aurigae. It has a white hue and is just barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.08. [2] The distance to this star is approximately 3,000  light years, based on parallax. [1] It has an absolute magnitude of −2.87. [3]

This object is an A-type giant star with a stellar classification of A2IIIshe. [3] The suffix notation indicates this is a shell star, [9] which means it has a peculiar spectrum indicating there is a circumstellar disk of gas around the star's equator. While the spectral luminosity class is III, analysis of its colour and brightness suggest it more closely resembles a supergiant star. [3] HD 32188 has expanded to 30 [1] times the radius of the Sun and it is spinning with a projected rotational velocity of 23 km/s. [7] It is radiating 2,428 [1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 7,350 K. [1]

Related Research Articles

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<span class="mw-page-title-main">54 Ceti</span> F-type main sequence star in the constellation Aries

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HD 35520 is a single star in the northern constellation of Auriga. It has a white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.92. The distance to this star is approximately 2,200 light years based on parallax. The radial velocity for the star is, as yet, poorly constrained.

Zeta<sup>2</sup> Antliae Star in the constellation Antlia

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HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

<span class="mw-page-title-main">Epsilon Crateris</span> Solitary star in the constellation Crater

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HD 16754 is a binary or triple-star system in the constellation Eridanus. It has the Bayer designation s Eridani; HD 16754 is the designation from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.74. It is located at a distance of approximately 132 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +18 km/s. The system is a member of the Columba association of co-moving stars.

<span class="mw-page-title-main">Nu Pegasi</span> Star in the constellation Pegasus

ν Pegasi, Latinized as Nu Pegasi is a single star in the northern constellation of Pegasus. It is an orange-hued star that is faintly visible to the naked eye with an apparent visual magnitude of 4.84. The star is located approximately 261 light years away based on parallax, but is drifting closer with a radial velocity of −19 km/s.

<span class="mw-page-title-main">HD 89890</span> Brightest member of a star system in the constellation Vela

HD 89890 is the brightest member of a multiple star system with at least four components, located in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.50. The annual parallax shift of 2.6 mas provides a distance estimate of around 1,200 light-years. It is moving further away from Earth with a heliocentric radial velocity of +10 km/s.

4 Cygni is a binary star system in the northern constellation of Cygnus. It is a faintly visible to the naked eye with an apparent visual magnitude of 5.17. The distance to 4 Cygni, as determined from its annual parallax shift of 5.8 mas, is about 560 light years.

<span class="mw-page-title-main">V4024 Sagittarii</span> Star in the constellation Sagittarius

V4024 Sagittarii is a single variable star in the southern constellation of Sagittarius. It has a blue-white hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.49. The star is located at a distance of approximately 1,700 light years based on stellar parallax, but is drifting closer with a radial velocity of −20 km/s. The position of this star near the ecliptic means it is subject to lunar occultations.

References

  1. 1 2 3 4 5 6 7 8 9 10 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 4 Guetter, H. H.; Hewitt, A. V. (June 1984), "Photoelectric UBV photometry for 317 PZT and VZT stars", Publications of the Astronomical Society of the Pacific, 96: 441–443, Bibcode:1984PASP...96..441G, doi: 10.1086/131362 .
  3. 1 2 3 4 5 Hauck, B.; Jaschek, C. (February 2000), "A-shell stars in the Geneva system", Astronomy and Astrophysics, 354: 157–162, Bibcode:2000A&A...354..157H.
  4. 1 2 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  5. ↑ Wilson, Ralph Elmer (1953), General Catalogue of Stellar Radial Velocities, Washington DC: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
  6. 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
  7. 1 2 Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, arXiv: astro-ph/0205255 , Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID   14070763.
  8. ↑ "HD 32188". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-12-18.
  9. ↑ Jaschek, M.; et al. (March 1988), "A survey of AE and A-type shell stars in the photographic region.", Astronomy and Astrophysics Supplement Series, 72: 505–513, Bibcode:1988A&AS...72..505J.
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