A Jovian analogue orbiting a white dwarf star.

Autor: Blackman JW; School of Natural Sciences, University of Tasmania, Hobart, Australia. joshua.blackman@utas.edu.au.; Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France. joshua.blackman@utas.edu.au., Beaulieu JP; School of Natural Sciences, University of Tasmania, Hobart, Australia.; Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France., Bennett DP; Laboratory for Exoplanets and Stellar Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD, USA.; Department of Astronomy, University of Maryland, College Park, MD, USA., Danielski C; Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France.; Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain.; UCL Centre for Space Exochemistry Data, Didcot, UK., Alard C; Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France., Cole AA; School of Natural Sciences, University of Tasmania, Hobart, Australia., Vandorou A; School of Natural Sciences, University of Tasmania, Hobart, Australia., Ranc C; Laboratory for Exoplanets and Stellar Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD, USA., Terry SK; Department of Astronomy, University of California Berkeley, Berkeley, CA, USA., Bhattacharya A; Laboratory for Exoplanets and Stellar Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD, USA.; Department of Astronomy, University of Maryland, College Park, MD, USA., Bond I; Institute for Natural and Mathematical Sciences, Massey University, Auckland, New Zealand., Bachelet E; Las Cumbres Observatory, Goleta, CA, USA., Veras D; Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK.; Department of Physics, University of Warwick, Coventry, UK.; Centre for Space Domain Awareness, University of Warwick, Coventry, UK., Koshimoto N; Laboratory for Exoplanets and Stellar Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD, USA.; Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo, Japan., Batista V; Sorbonne Universités, UPMC Université Paris 6 et CNRS, UMR 7095, Institut d'Astrophysique de Paris, Paris, France., Marquette JB; Laboratoire d'Astrophysique de Bordeaux, University of Bordeaux, Pessac, France.
Jazyk: angličtina
Zdroj: Nature [Nature] 2021 Oct; Vol. 598 (7880), pp. 272-275. Date of Electronic Publication: 2021 Oct 13.
DOI: 10.1038/s41586-021-03869-6
Abstrakt: 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 5-8 . Simulations predict 9-11 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. 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. 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.
(© 2021. The Author(s), under exclusive licence to Springer Nature Limited.)
Databáze: MEDLINE
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