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arxiv: 1904.02163 · v1 · pith:3X3NPPDRnew · submitted 2019-04-03 · 🌌 astro-ph.EP · astro-ph.SR

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

Christopher J. Manser , Boris T. G\"ansicke , Siegfried Eggl , Mark Hollands , Paula Izquierdo , Detlev Koester , John D. Landstreet , Wladimir Lyra
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Thomas R. Marsh Farzana Meru Alexander J. Mustill Pablo Rodr\'iguez-Gil Odette Toloza Dimitri Veras David J. Wilson Matthew R. Burleigh Melvyn B. Davies Jay Farihi Nicola Gentile Fusillo Domitilla de Martino Steven G. Parsons Andreas Quirrenbach Roberto Raddi Sabine Reffert Melania Del Santo Matthias R. Schreiber Roberto Silvotti Silvia Toonen Eva Villaver Mark Wyatt Siyi Xu Simon Portegies Zwart
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classification 🌌 astro-ph.EP astro-ph.SR
keywords debrisdwarfwhitearounddiscemissionstrengthsystems
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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.

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  1. Size limits on tidal debris around white dwarfs: the km-size barrier

    astro-ph.EP 2026-06 unverdicted novelty 5.0

    Tidal breakup of cohesive rubble piles around white dwarfs imposes a 0.1-1 km maximum fragment size that sets the initial debris distribution and requires collisional grinding before Poynting-Robertson drag acts.