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.
A planetesimal orbiting within the debris disc around a white dwarf star / Manser, C.J., Gansicke, B.T., Eggl, S., Hollands, M., Izquierdo, P., Koester, D., Landstreet, J.D., Lyra, W., Marsh, T.R., Meru, F., Mustill, A.J., Rodriguez-Gil, P., Toloza, O., Veras, D., Wilson, D.J., Burleigh, M.R., Davies, M.B., Farihi, J., Gentile Fusillo, N., de Martino, D., et al.. - In: SCIENCE. - ISSN 0036-8075. - 364/2019:6435(2019), pp. 66-69. [10.1126/science.aat5330]
A planetesimal orbiting within the debris disc around a white dwarf star
Gentile Fusillo N.Writing – Review & Editing
;de Martino D.;
2019-01-01
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.| File | Dimensione | Formato | |
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