KPD 0005+5106 is a helium-rich white dwarf [4] located 1,350 light-years from Earth. [2] As a "pre-white dwarf", it is believed to still be in the helium-burning phase, just before nuclear fusion finally stops. It is one of the hottest known white dwarfs, with a temperature of 200,000 K. [3]

KPD 1930+2752 is a binary star system including a subdwarf B star and a probable white dwarf with relatively high mass. [4]

Nov 26, 2021 · There's a dead star behaving very oddly 1,300 light-years away. It's a white dwarf named KPD 0005+5106, and X-ray data from the Chandra space telescope have revealed that it's enacting extreme violence on an orbiting companion.

Astronomers have observed that the white dwarf KPD 0005+5106, located about 1,300 light years from Earth, emits high-energy X-ray emission that regularly increases and decreases in X-ray brightness every 4.7 hours. This recurring ebb and flow of X-rays indicates that KPD 0005+5106 has an object in orbit around it — either a very low mass star or a planet — depicted in the illustration by ...

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Mar 14, 2011 · KPD 1930+2752 is a short-period pulsating subdwarf B (sdB) star. It is also an ellipsoidal variable with a known binary period of 2.3 h. The companion is most likely a white dwarf and the total mass of the system is close to the Chandresekhar limit.

Nov 1, 2010 · KPD 1930+2752 is a short-period pulsating subdwarf B (sdB) star. It is also an ellipsoidal variable with a known binary period just over two hours. The companion is most likely a white dwarf and the total mass of the system is close to the Chandresakhar limit.

KPD 1930+2752 is the first star to be discovered that is a good candidate for the progenitor of a Type Ia supernova of this type, which will merge on an astrophysically interesting time-scale. We present spectra of the pulsating sdB star KPD 1930+2752 which confirm that this star is a binary.

KPD 1930+2752 is a short-period pulsating subdwarf B (sdB) star. It is also an ellipsoidal variable with a known binary period of 2.3 h. The companion is most likely a white dwarf and the total mass of the system is close to the Chandresekhar limit.