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Published October 22, 2015 | Supplemental Material + Submitted
Journal Article Open

A disintegrating minor planet transiting a white dwarf


Most stars become white dwarfs after they have exhausted their nuclear fuel (the Sun will be one such). Between one-quarter and one-half of white dwarfs have elements heavier than helium in their atmospheres, even though these elements ought to sink rapidly into the stellar interiors (unless they are occasionally replenished). The abundance ratios of heavy elements in the atmospheres of white dwarfs are similar to the ratios in rocky bodies in the Solar System. This fact, together with the existence of warm, dusty debris disks surrounding about four per cent of white dwarfs, suggests that rocky debris from the planetary systems of white-dwarf progenitors occasionally pollutes the atmospheres of the stars. The total accreted mass of this debris is sometimes comparable to the mass of large asteroids in the Solar System. However, rocky, disintegrating bodies around a white dwarf have not yet been observed. Here we report observations of a white dwarf—WD 1145+017—being transited by at least one, and probably several, disintegrating planetesimals, with periods ranging from 4.5 hours to 4.9 hours. The strongest transit signals occur every 4.5 hours and exhibit varying depths (blocking up to 40 per cent of the star's brightness) and asymmetric profiles, indicative of a small object with a cometary tail of dusty effluent material. The star has a dusty debris disk, and the star's spectrum shows prominent lines from heavy elements such as magnesium, aluminium, silicon, calcium, iron, and nickel. This system provides further evidence that the pollution of white dwarfs by heavy elements might originate from disrupted rocky bodies such as asteroids and minor planets.

Additional Information

© 2015 Macmillan Publishers Limited. Received 11 June 2015. Accepted 26 August 2015. Published online 21 October 2015. We thank B. Croll, D. Veras, M. Holman, R. Loomis, J. Becker, K. Deck, H. Schlichting, H. Lin, A. Loeb, and D. Osip for discussions and assistance. We thank C. Allinson, S. Dillet, D. Frostig, A. Johnson, D. Hellstrom, S. Johnson, B. Peak, and T. Reneau for conducting MINERVA observations. We thank M. Wyatt for suggesting how to present Supplementary Fig. 8. A.V. is supported by a National Science Foundation Graduate Research Fellowship (grant DGE 1144152). J.A.J. is supported by grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. The Center for Exoplanets and Habitable Worlds is supported by Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. The MEarth Team acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (to D.C.), the National Science Foundation under grants AST-0807690, AST-1109468, and AST-1004488 (Alan T. Waterman Award), and a grant from the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This research has made use of NASA's Astrophysics Data System, the SIMBAD database and VizieR catalog access tool operated at the Centre de Données astronomiques de Strasbourg, France. Some of the data presented here were obtained from the Mikulski Archive for Space Telescopes (MAST). This paper includes data from the Kepler/K2 mission, the Wide-field Infrared Survey Explorer, the MMT Observatory, the Sloan Digital Sky Survey (SDSS-III), the National Geographic Society—Palomar Observatory Sky Atlas (POSS-I) and the W.M. Keck Observatory. MINERVA is made possible by contributions from its collaborating institutions and Mt Cuba Astronomical Foundation, the David and Lucile Packard Foundation, the National Aeronautics and Space Administration, and the Australian Research Council. We acknowledge the cultural significance of the summit of Maunakea within the indigenous Hawai'ian community. We are grateful for the opportunity to conduct observations from this mountain. Contributions: A.V. processed and searched the K2 data, identified this system, analysed the K2 data for WD 1145+017 (with help from S.R., D.K., and J.T.W.), processed the MINERVA data, measured radial velocities (with help from W.R.B. and D.W.L.), and was the primary author of the manuscript. S.R. performed the dynamical calculations and dust simulations. W.R.B. obtained and reduced the MMT spectra. P.D. analysed the MMT spectra and SDSS photometry to measure spectroscopic properties. J.A.L. analysed archival photometric measurements and modelled the excess infrared emission. A.B. and D.W.L. obtained and processed the FLWO data. J.I. and D.C. obtained and processed the MEarth data. D.R.C. and C.B. obtained and processed the Keck data. R.A. calculated the systematics insensitive periodogram. L.S. calculated vapour pressures for some minerals with MAGMA. J.A.J., J.E., N.M., R.A.W., and J.T.W. made it possible to use MINERVA. J.A.J. provided scientific leadership. The authors declare no competing financial interests. The raw K2 data are available at http://archive.stsci.edu/k2/data_search/search.php under the identification number 201563164. The processed K2 data are available at https://archive.stsci.edu/missions/hlsp/k2sff/html/c01/ep201563164.html. We have opted not to make the code used in this work available.

Attached Files

Submitted - 1510.06387.pdf

Supplemental Material - nature15527-s1.pdf

Supplemental Material - nature15527-s2.txt

Supplemental Material - nature15527-s3.txt

Supplemental Material - nature15527-s4.txt


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