A planetesimal orbiting within the debris disc around a white dwarf star
A low-mass planet around a white dwarf
Numerous exoplanets have been detected around Sun-like stars. These stars end their lives as white dwarfs, which should inherit any surviving planetary systems. Manser et al. found periodic shifts in emission lines from a disc of gas orbiting around a white dwarf (see the Perspective by Fossati). They used numerical simulations to show that the most likely explanation for the spectral shifts is a low-mass planet orbiting within the disc. The planet must be unusually small and dense to avoid being ripped apart by tidal forces. The authors speculate that it may be the leftover core of a planet whose outer layers have been removed.
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.
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Supplementary Material
Summary
Materials and Methods
Supplementary Text
Figs. S1 to S8
Tables S1 to S3
Resources
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Accepted: 26 February 2019
Acknowledgments
This work is based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in La Palma, Canary Islands. This work has made use of data from the European Space Agency (ESA) mission Gaia (www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium [(DPAC), www.cosmos.esa.int/web/gaia/dpac/consortium]. Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Based on observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under program IDs: 595.C-0650. Funding: This research has been carried out with telescope time awarded by the CCI International Time Programme. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC grant agreement 320964 (WDTracer). T.R.M. acknowledges support from STFC (ST/P000495/1). J.D.L acknowledges the funding support of the Natural Sciences and Engineering Research Council of Canada. D.V. acknowledges the support of the STFC via an Ernest Rutherford Fellowship (grant ST/P003850/1). M.R.S. is thankful for support from Fondecyt (1141269). A.J.M. and M.B.D. acknowledge the support of KAW project grant 2014.0017. A.J.M. also acknowledges the support of VR grant 2017-04945. O.T. was partially supported by a Leverhulme Trust Research Project Grant. F.M. acknowledges support from the Royal Society Dorothy Hodgkin Fellowship. P.R.-G. acknowledges support provided by the Spanish Ministry of Economy, Industry and Competitiveness through grant AYA-2017-83383-P, which is partly funded by the European Regional Development Fund of the European Union. This research was supported by the Jet Propulsion Laboratory through the California Institute of Technology postdoctoral fellowship program, under a contract with the National Aeronautics and Space Administration. Author contributions: C.J.M. led the overall project. C.J.M., B.T.G., S.E., J.D.L., W.L., A.J.M., and D.J.W. contributed to the writing of the manuscript. T.R.M., F.M., and D.V. contributed to the interpretation of the results. C.J.M., M.H., and P.I. reduced the spectra obtained from VLT/UVES and GTC/OSIRIS. D.K. and O.T. produced the white dwarf models used by J.D.L. to calculate the magnetic field strength of the white dwarf. W.L. produced the photoelectric instability simulations of the disc. P.R.-G., T.R.M., M.R.B., M.B.D., J.F., N.G.F., D.d.M., S.G.P., A.Q., R.R., S.R., M.D.S., M.R.S., R.S., S.T., E.V., M.W., S.X., and S.P.Z. contributed to the proposals that led to the data collection and discussion of the results. Competing interests: The authors declare no conflict of interests. Data and materials availability: The data used in this research are available from the ESO VLT archive (36), under proposal number 595.C-0650(G), and the GTC archive (37), under proposal numbers GTC1–16ITP and GTC25–18A. The zeeman software and the model shown in fig. S5 are available from https://sourceforge.net/projects/zeeman-f/. The pencil code software is available at https://github.com/pencil-code; we used version #f4f2f16, with the model shown in figs. S6 and S7 in the directory pencil-code/samples/2d-tests/WhiteDwarfDisk.
Authors
Funding Information
H2020 European Research Council: 677706 (WD3D)
H2020 European Research Council: 677706 (WD3D)
Space Telescope Science Institute: HST-AR-14572
Leverhulme Trust: RPG-2017-441
Royal Society: Dorothy Hodgkin Fellowship
Knut och Alice Wallenbergs Stiftelse: 2014.0017
Vetenskapsrådet: 2017-04945
European Research Council: 320964 (WDTracer)
STFC: ST/P003850/1
Ministerio de Economía y Competitividad: AYA2014-55840-P
STFC: ST/P000495/1
European Research Council: 320964 (WDTracer)
Deutsche Forschungsgemeinschaft: HE1356/71-1
Deutsche Forschungsgemeinschaft: IR190/1-1
MINECO SEV-2015-0548: BES-2016-077715
Iniciativa Cientifica Milenio: NPF - Millennium Nucleus for Planet Formation
FONDECYT: 1181404
NASA Exoplanet Research Program: 16- XRP16_2-0065
