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The supposed planetesimal, WD 1145+017 b, [13] with a 4.5 hour orbit, is being ripped apart by the star and is a remnant of the former planetary system that the star hosted before becoming a white dwarf. [8] [9] It is the first observation of a planetary object being shredded by a white dwarf. Several other large pieces have been seen in orbit ...
Leaving aside formation from the accretion disk surrounding the white dwarf, there are two ways a planet could end in a close orbit around stars of this kind: by surviving being engulfed by the star during its red giant phase, and then spiralling inward, or inward migration after the white dwarf has formed. The former case is implausible for ...
BZ Ursae Majoris is a dwarf nova star system in the northern circumpolar constellation of Ursa Major.It consists of a white dwarf primary in a close orbit with a red dwarf.The latter star is donating mass, which is accumulating in an accretion disk orbiting the white dwarf. [14]
The planetary object orbits a white dwarf.It has ended its main sequence lifetime and will continue to cool for billions of years to come in the future. Based on recent studies and its mass, the star was likely an early A-type main sequence star with a mass of 2.46 M ☉ and main sequence lifetime of 550 million years before it expanded and became a red giant. [5]
First white dwarf with a planet WD B1620−26: 2003 PSR B1620-26 b (planet) This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [5] [6] First singular white dwarf with a planet WD 1145+017: 2015 WD 1145+017 b: Planet is extremely small and is disintegrating. First white dwarf that is a pulsar: AR Scorpii A ...
This star system consists of a red dwarf of spectral type M6 and a white dwarf that orbit each other every seven hours; the former is 18% as massive as the Sun, while the latter has 44% of the Sun's mass. [8] The red dwarf is tidally locked with the white dwarf, meaning it displays the same side to the heavier star. [9]
The system comprises an eclipsing white dwarf and red dwarf in tight orbit (nearly 1.5 hours) and an extrasolar planet. [8] This eclipsing variable was discovered by P. Biermann and associates in 1982 as the optical counterpart to the EINSTEIN X-ray source E1114+182.
The location of T Pyxidis (circled in red). T Pyxidis (T Pyx) [4] is a recurrent nova [5] and nova remnant in the constellation Pyxis. It is a binary star system and its distance is estimated at 4,783 parsecs (15,600 light-years) from Earth. It contains a Sun-like star and a white dwarf. Because of their close proximity and the larger mass of ...