Stein 2051

Stein 2051 (Gliese 169.1, G 175-034, LHS 26/27) is a nearby binary star system, containing a red dwarf (component A) and a degenerate star (white dwarf) (component B), located in constellation Camelopardalis at about 18 ly from Earth.[8]

Stein 2051

Stein 2051 taken by Hubble Space Telescope.[1]
Credit: NASA, ESA, and K. Sahu (STScI)
Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Stein 2051 A
Right ascension  04h 31m 11.5181s[2]
Declination +58° 58′ 37.461″[2]
Apparent magnitude (V) 10.977[2]
Stein 2051 B
Right ascension  04h 31m 12.570s[3]
Declination +58° 58′ 41.15″[3]
Apparent magnitude (V) 11.19[3]
Characteristics
Stein 2051 A
Spectral type M4.0Ve[2]
U−B color index +1.21[4]
B−V color index +1.65[4]
Stein 2051 B
Spectral type DC5[3]
U−B color index -0.53[4]
B−V color index +0.31[4]
Astrometry
Stein 2051 A
Radial velocity (Rv)29 km/s
Proper motion (μ) RA: 1300.2[5] mas/yr
Dec.: -2049.0[5] mas/yr
Parallax (π)180 ± 0.8[2] mas
Distance18.12 ± 0.08 ly
(5.56 ± 0.02 pc)
Stein 2051 B
Radial velocity (Rv)2.0 km/s
Proper motion (μ) RA: 1335.6[5] mas/yr
Dec.: -1962.6[5] mas/yr
Parallax (π)179 ± 3[3] mas
Distance18.2 ± 0.3 ly
(5.59 ± 0.09 pc)
Other designations
Stein 2051, G 175-34, HIP 21088,[6] WDS J04312+5858AB, GJ 169.1,[7] PLX 986.01[8]
Stein 2051 A: LHS 26, NLTT 13373, TYC 3744-412-1, 2MASS J04311147+585837, WISE J043113.20+585816.7[2]
Stein 2051 B: EGGR 180, LHS 27, NLTT 13375, TYC 3744-2062-1, 2MASS J04311201+5858476, WD 0426+58, WD2 0426+585, WD3 0426+588[3]
Database references
SIMBADThe system
A
B

Stein 2051 is the nearest (red dwarf + white dwarf) separate binary system (40 Eridani BC is located closer at 16.26 light-years,[9] but it is a part of a triple star system).

Stein 2051 B is the 6th nearest white dwarf after Sirius B, Procyon B, van Maanen's star, LP 145-141 and 40 Eridani B.

Properties

The brighter of this two stars is A (a red dwarf), but the more massive is component B (a white dwarf).

In 2017, Stein 2051 B was observed passing in front of a more distant star. The bending of starlight by the gravitational field of the nearer star allowed its mass to be directly measured. The estimated mass of Stein 2051 B is 0.675±0.051 M☉, which fits the expected range of a white dwarf with a carbon-oxygen core.[10]

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References
  1. "Einstein revisited". www.spacetelescope.org. Retrieved 12 June 2017.
  2. "NAME Stein 2051 A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 December 2016.
  3. "NAME Stein 2051 B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 December 2016.
  4. Hardie, R. H. (1966). "UBV Photometry of the Lowell Proper Motion Object G175-34". Publications of the Astronomical Society of the Pacific. 78 (462): 171. Bibcode:1966PASP...78..171H. doi:10.1086/128321.
  5. Zacharias, N. (2012). "The fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". VizieR On-line Data Catalog. Bibcode:2012yCat.1322....0Z.
  6. Perryman; et al. (1997). "HIP 21088". The Hipparcos and Tycho Catalogues. Retrieved 2014-11-23.
  7. Gliese, W. & Jahreiß, H. (1991). "Gl 169.1". Preliminary Version of the Third Catalogue of Nearby Stars. Retrieved 2014-11-23.
  8. Van Altena W. F.; Lee J. T.; Hoffleit E. D. (1995). "GCTP 986.01". The General Catalogue of Trigonometric Stellar Parallaxes (Fourth ed.). Retrieved 2014-11-23.
  9. Perryman; et al. (1997). "HIP 19849". The Hipparcos and Tycho Catalogues. Retrieved 2014-11-21.
  10. Sahu, Kailash C.; et al. (June 2017), "Relativistic deflection of background starlight measures the mass of a nearby white dwarf star", Science, 356 (6342): 1046–1050, arXiv:1706.02037, Bibcode:2017Sci...356.1046S, doi:10.1126/science.aal2879.


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