A planetesimal orbiting within the debris disc around a white dwarf star
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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 123.4-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.
1989 ◽
Vol 114
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pp. 296-299
1989 ◽
Vol 114
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pp. 384-387
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2011 ◽
Vol 77
(5)
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pp. 571-575
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1987 ◽
Vol 93
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pp. 785-794
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2020 ◽
Vol 497
(1)
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pp. L24-L29
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2017 ◽
Vol 598
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pp. A109
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