Stein 2051 Explained

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.[1]

Stein 2051 is the nearest (red dwarf + white dwarf) separate binary system (40 Eridani BC is located closer at 16.26 light-years,[2] 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 these 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, which fits the expected range of a white dwarf with a carbon-oxygen core.

External links

Notes and References

  1. Web site: GCTP 986.01. The General Catalogue of Trigonometric Stellar Parallaxes . Fourth . Van Altena W. F. . Lee J. T. . Hoffleit E. D. . 1995. 2014-11-23.
  2. Web site: HIP 19849. The Hipparcos and Tycho Catalogues. Perryman. 1997. etal. 2014-11-21.