GP Comae Berenices
GP Comae Berenices, abbreviated to GP Com and also known as G 61-29, is a star system composed of a white dwarf orbited by a planetary mass object, likely the highly eroded core of another white dwarf star.[7] The white dwarf is slowly accreting material from its satellite at a rate of (3.5±0.5)×10−11 M☉/year and was proven[8] to be a low-activity AM CVn star.[7][5] The star system is showing signs of a high abundance of ionized nitrogen from the accretion disk around the primary.[9] In 1971, Brian Warner discovered that the star, then known as G61-29, is a variable star.[10][11] it was given its variable star designation, GP Comae Berenices, in 1975.[12] Planetary systemThe material emitted from the planetary mass companion is mostly helium, with a molar ratio of nitrogen up to 1.7%, very low neon levels and other elements not detectable at all.[13] Approximately half of the luminosity of the system comes from the accretion disk.[5] The planetary object is suspected to contain a strange quark matter core due to its unusually high density, which must be above 187.5 g/cm3 to prevent tidal disruption; the theoretical bound for planets composed solely of ordinary matter is on the order of 30 g/cm3. The object's orbit is expected to decay within 100 million years due to gravitational wave emission.[14]
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