| Literature DB >> 30948547 |
Christopher J Manser1, Boris T Gänsicke2,3, Siegfried Eggl4, Mark Hollands2, Paula Izquierdo5,6, Detlev Koester7, John D Landstreet8,9, Wladimir Lyra4,10, Thomas R Marsh2, Farzana Meru2, Alexander J Mustill11, Pablo Rodríguez-Gil5,6, Odette Toloza2, Dimitri Veras2,3, David J Wilson2,12, Matthew R Burleigh13, Melvyn B Davies11, Jay Farihi14, Nicola Gentile Fusillo2, Domitilla de Martino15, Steven G Parsons16, Andreas Quirrenbach17, Roberto Raddi18, Sabine Reffert17, Melania Del Santo19, Matthias R Schreiber20,21, Roberto Silvotti22, Silvia Toonen23, Eva Villaver24, Mark Wyatt25, Siyi Xu26, Simon Portegies Zwart27.
Abstract
Many white dwarf stars show signs of having accreted smaller bodies, implying that they may host planetary systems. A small number of these systems contain gaseous debris discs, visible through emission lines. We report a stable 123.4-minute periodic variation in the strength and shape of the Ca ii emission line profiles originating from the debris disc around the white dwarf SDSS J122859.93+104032.9. We interpret this short-period signal as the signature of a solid-body planetesimal held together by its internal strength.Entities:
Year: 2019 PMID： 30948547 DOI： 10.1126/science.aat5330
Source DB: PubMed Journal: Science ISSN： 0036-8075 Impact factor: 47.728