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#White dwarf magazine 298.pdf drivers#
Unstable low-mass planetary systems as drivers of white dwarf pollution.
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The effect of tides on the population of PN from interacting binaries. Accretion of a giant planet onto a white dwarf. Discovery of a candidate for the coolest known brown dwarf. A giant planet candidate transiting a white dwarf. A young white dwarf companion to pulsar B1620-26: evidence for early planet formation. The effects of post-main-sequence solar mass loss on the stability of our planetary system. Can planets survive stellar evolution? Astrophys. A planetesimal orbiting within the debris disc around a white dwarf star. A disintegrating minor planet transiting a white dwarf. 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. 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. 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. Here we report the non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb 12 using near-infrared observations from the Keck Observatory.
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Simulations predict 9, 10, 11 that planets in Jupiter-like orbits around stars of ≲8 M ☉ (solar mass) avoid being destroyed by the strong tidal forces of their stellar host, but as yet, there has been no observational confirmation of such a survivor. Studies 1, 2 have shown that the remnants of destroyed planets and debris-disk planetesimals can survive the volatile evolution of their host stars into white dwarfs 3, 4, but few intact planetary bodies around white dwarfs have been detected 5, 6, 7, 8.