A planetesimal orbiting within the debris disc around a white dwarf star

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 123.4min periodic variation in the strength and shape of the CaII emiss...

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Veröffentlicht in:	arXiv.org 2019-04
Hauptverfasser:	Manser, Christopher J, Gänsicke, Boris T, Eggl, Siegfried, Hollands, Mark, Izquierdo, Paula, Koester, Detlev, Landstreet, John D, Lyra, Wladimir, Marsh, Thomas R, Meru, Farzana, Mustill, Alexander J, Rodríguez-Gil, Pablo, Toloza, Odette, Veras, Dimitri, Wilson, David J, Burleigh, Matthew R, Davies, Melvyn B, Farihi, Jay, Nicola Gentile Fusillo, de Martino, Domitilla, Parsons, Steven G, Quirrenbach, Andreas, Raddi, Roberto, Reffert, Sabine, Melania Del Santo, Schreiber, Matthias R, Silvotti, Roberto, Toonen, Silvia, Villaver, Eva, Wyatt, Mark, Xu, Siyi, Simon Portegies Zwart
Format:	Artikel
Sprache:	eng
Schlagworte:	Debris Emission Periodic variations Physics - Earth and Planetary Astrophysics Physics - Solar and Stellar Astrophysics Planetary systems White dwarf stars White dwarfs
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Beschreibung
Zusammenfassung:	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 123.4min periodic variation in the strength and shape of the CaII emission line profiles originating from the debris disc around the white dwarf SDSSJ122859.93+104032.9. We interpret this short-period signal as the signature of a solid body held together by its internal strength.
ISSN:	2331-8422
DOI:	10.48550/arxiv.1904.02163