PG 1413+01 - A white dwarf-red dwarf eclipsing binary

Details PG 1413+01 - A white dwarf-red dwarf eclipsing binary PG 1413+01 - A white dwarf-red dwarf eclipsing binary

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..892g&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 15, 1978, p. 892, 893, 895-898.

Astronomy and Astrophysics

Astrophysics

34

Dwarf Stars, Eclipsing Binary Stars, Late Stars, Hot Stars, Light Curve, M Stars, Stellar Evolution, Stellar Spectrophotometry, White Dwarf Stars

Scientific paper

The star PG 1413+01, discovered in a survey for blue stars at high galactic latitude, is an eclipsing binary with a period of 8 h 16 m. The system resembles the red dwarf-white dwarf binary BD +16 deg 516. The primary is a hot white dwarf with a mass of about 0.7 + or 0.3 solar mass. The faint secondary has been detected in the red and is probably a dwarf of spectral type M3 + or - 3. The two components are separated by around 2 solar radii. Since it is unlikely that the hot white dwarf is heated by accretion, the binary system has probably been in its present state for less than a million years. It is possible that the system is a post-common-envelope binary.

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