Journal
SCIENCE
Volume 364, Issue 6435, Pages 66-+Publisher
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.aat5330
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Funding
- CCI International Time Programme
- European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC [320964]
- STFC [ST/P000495/1]
- Natural Sciences and Engineering Research Council of Canada
- STFC via an Ernest Rutherford Fellowship [ST/P003850/1]
- Fondecyt [1141269]
- KAW project [2014.0017]
- VR grant [2017-04945]
- Leverhulme Trust Research Project Grant
- Royal Society Dorothy Hodgkin Fellowship
- Spanish Ministry of Economy, Industry and Competitiveness - European Regional Development Fund of the European Union [AYA-2017-83383-]
- Jet Propulsion Laboratory through the California Institute of Technology postdoctoral fellowship program, under National Aeronautics and Space Administration
- STFC [ST/M001377/1, ST/J003344/2, ST/J003344/1, ST/N000048/1, ST/N002695/1, ST/K003453/2, ST/P000495/1, ST/S000623/1, ST/P003850/1, ST/K003453/1, ST/J003344/3, ST/M004546/1, ST/R000476/1] Funding Source: UKRI
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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.
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