We determine that this system contains a 0.53 ± 0.11 M ☉ white-dwarf host orbited by a 1.4 ± 0.3 Jupiter-mass planet with a separation on the plane of the sky of 2.8 ± 0.5 astronomical units, which implies a semi-major axis larger than this. This system is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their host’s evolution, and supports the prediction that more than half of white dwarfs have Jovian planetary companions 13. Located at approximately 2.0 kiloparsecs towards the centre of our Galaxy, it is likely to represent an analogue to the end stages of the Sun and Jupiter in our own Solar System. A disintegrating minor planet transiting a white dwarf. A planetesimal orbiting within the debris disc around a white dwarf star. Can planets survive stellar evolution? Astrophys. The effects of post-main-sequence solar mass loss on the stability of our planetary system.
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