A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host.
| Title: | A giant planet undergoing extreme-ultraviolet irradiation by its hot massive-star host. |
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| Authors: | Gaudi BS; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Stassun KG; Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, Tennessee 37235, USA.; Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, Tennessee 37208, USA.; Collins KA; Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, Tennessee 37235, USA.; Beatty TG; Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, 525 Davey Laboratory, University Park, Pennsylvania 16802, USA.; Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, Pennsylvania 16802, USA.; Zhou G; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Latham DW; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Bieryla A; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Eastman JD; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Siverd RJ; Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, California 93117, USA.; Crepp JR; Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, Indiana 46556, USA.; Gonzales EJ; Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, Indiana 46556, USA.; Stevens DJ; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Buchhave LA; Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 21S00 Copenhagen, Denmark.; Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, 1350 Copenhagen, Denmark.; Pepper J; Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, Pennsylvania 18015, USA.; Johnson MC; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Colon KD; NASA Ames Research Center, M/S 244-30, Moffett Field, California 94035, USA.; Bay Area Environmental Research Institute, 625 2nd Street Ste. 209, Petaluma, California 94952, USA.; Jensen ELN; Department of Physics and Astronomy, Swarthmore College, Swarthmore, Pennsylvania 19081, USA.; Rodriguez JE; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Bozza V; Dipartimento di Fisica 'E. R. Caianiello', Università di Salerno, Via Giovanni Paolo II 132, 84084 Fisciano (SA), Italy.; Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, 80126 Napoli, Italy.; Novati SC; Dipartimento di Fisica 'E. R. Caianiello', Università di Salerno, Via Giovanni Paolo II 132, 84084 Fisciano (SA), Italy.; IPAC, Mail Code 100-22, Caltech, 1200 East California Boulevard, Pasadena, California 91125, USA.; D'Ago G; Istituto Internazionale per gli Alti Studi Scientifici (IIASS), Via G. Pellegrino 19, 84019 Vietri sul Mare (SA), Italy.; INAF-Observatory of Capodimonte, Salita Moiariello 16, 80131 Naples, Italy.; Dumont MT; Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA.; Department of Astronomy and Astrophysics, University of California Santa Cruz, Santa Cruz, California 95064, USA.; Ellis T; Department of Physics and Astronomy, University of Wyoming, 1000 East University, Laramie, Wyoming 82071, USA.; Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA.; Gaillard C; Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA.; Jang-Condell H; Department of Physics and Astronomy, University of Wyoming, 1000 East University, Laramie, Wyoming 82071, USA.; Kasper DH; Department of Physics and Astronomy, University of Wyoming, 1000 East University, Laramie, Wyoming 82071, USA.; Fukui A; Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, NINS, Asakuchi, Okayama 719-0232, Japan.; Gregorio J; Atalaia Group and Crow Observatory, Portalegre, Portugal.; Ito A; National Astronomical Observatory of Japan, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.; Graduate School of Science and Engineering, Hosei University, 3-7-2 Kajino-cho, Koganeishi, Tokyo 184-8584, Japan.; Kielkopf JF; Department of Physics and Astronomy, University of Louisville, Louisville, Kentucky 40292, USA.; Manner M; Spot Observatory, Nashville, Tennessee 37206, USA.; Matt K; Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA.; Narita N; National Astronomical Observatory of Japan, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.; Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan.; Astrobiology Center, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan.; Oberst TE; Department of Physics, Westminster College, New Wilmington, Pennsylvania 16172, USA.; Reed PA; Department of Physical Sciences, Kutztown University, Kutztown, Pennsylvania 19530, USA.; Scarpetta G; Dipartimento di Fisica 'E. R. Caianiello', Università di Salerno, Via Giovanni Paolo II 132, 84084 Fisciano (SA), Italy.; IPAC, Mail Code 100-22, Caltech, 1200 East California Boulevard, Pasadena, California 91125, USA.; Stephens DC; Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA.; Yeigh RR; Department of Physics and Astronomy, University of Wyoming, 1000 East University, Laramie, Wyoming 82071, USA.; Zambelli R; Società Astronomica Lunae, Castelnuovo Magra 19030, Italy.; Fulton BJ; Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822-1839, USA.; Howard AW; Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, Hawaii 96822-1839, USA.; James DJ; Astronomy Department, University of Washington, Box 351580, Seattle, Washington 98195, USA.; Penny M; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Bayliss D; Observatoire Astronomique de l'Université de Genève, 51 Chemin des Maillettes, 1290 Versoix, Switzerland.; Curtis IA; ICO, Adelaide, South Australia, Australia.; DePoy DL; George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A &M University, College Station, Texas 77843-4242, USA.; Esquerdo GA; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Gould A; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany.; Joner MD; Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA.; Kuhn RB; South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa.; Labadie-Bartz J; Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, Pennsylvania 18015, USA.; Lund MB; Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, Tennessee 37235, USA.; Marshall JL; George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A &M University, College Station, Texas 77843-4242, USA.; McLeod KK; Wellesley College, 106 Central Street, Wellesley, Massachusetts 02481, USA.; Pogge RW; Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA.; Relles H; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA.; Stockdale C; Hazelwood Observatory, Churchill, Victoria, Australia.; Tan TG; Perth Exoplanet Survey Telescope, Perth, Western Australia, Australia.; Trueblood M; Winer Observatory, Sonoita, Arizona 85637, USA.; Trueblood P; Winer Observatory, Sonoita, Arizona 85637, USA. |
| Source: | Nature [Nature] 2017 Jun 22; Vol. 546 (7659), pp. 514-518. Date of Electronic Publication: 2017 Jun 05. |
| Publication Type: | Journal Article; Research Support, U.S. Gov't, Non-P.H.S.; Research Support, Non-U.S. Gov't |
| Language: | English |
| Journal Info: | Publisher: Nature Publishing Group Country of Publication: England NLM ID: 0410462 Publication Model: Print-Electronic Cited Medium: Internet ISSN: 1476-4687 (Electronic) Linking ISSN: 00280836 NLM ISO Abbreviation: Nature Subsets: PubMed not MEDLINE |
| Imprint Name(s): | Publication: Basingstoke : Nature Publishing Group; Original Publication: London, Macmillan Journals ltd. |
| Abstract: | The amount of ultraviolet irradiation and ablation experienced by a planet depends strongly on the temperature of its host star. Of the thousands of extrasolar planets now known, only six have been found that transit hot, A-type stars (with temperatures of 7,300-10,000 kelvin), and no planets are known to transit the even hotter B-type stars. For example, WASP-33 is an A-type star with a temperature of about 7,430 kelvin, which hosts the hottest known transiting planet, WASP-33b (ref. 1); the planet is itself as hot as a red dwarf star of type M (ref. 2). WASP-33b displays a large heat differential between its dayside and nightside, and is highly inflated-traits that have been linked to high insolation. However, even at the temperature of its dayside, its atmosphere probably resembles the molecule-dominated atmospheres of other planets and, given the level of ultraviolet irradiation it experiences, its atmosphere is unlikely to be substantially ablated over the lifetime of its star. Here we report observations of the bright star HD 195689 (also known as KELT-9), which reveal a close-in (orbital period of about 1.48 days) transiting giant planet, KELT-9b. At approximately 10,170 kelvin, the host star is at the dividing line between stars of type A and B, and we measure the dayside temperature of KELT-9b to be about 4,600 kelvin. This is as hot as stars of stellar type K4 (ref. 5). The molecules in K stars are entirely dissociated, and so the primary sources of opacity in the dayside atmosphere of KELT-9b are probably atomic metals. Furthermore, KELT-9b receives 700 times more extreme-ultraviolet radiation (that is, with wavelengths shorter than 91.2 nanometres) than WASP-33b, leading to a predicted range of mass-loss rates that could leave the planet largely stripped of its envelope during the main-sequence lifetime of the host star. |
| References: | Astrophys J. 2000 Jan 20;529(1):L41-L44. (PMID: 10615032); Astrophys J. 2000 Jan 20;529(1):L45-L48. (PMID: 10615033); Science. 2010 Feb 19;327(5968):977-80. (PMID: 20056856); Nature. 2017 Feb 22;542(7642):456-460. (PMID: 28230125) |
| Entry Date(s): | Date Created: 20170606 Date Completed: 20171006 Latest Revision: 20181113 |
| Update Code: | 20260130 |
| DOI: | 10.1038/nature22392 |
| PMID: | 28582774 |
| Database: | MEDLINE |
Journal Article; Research Support, U.S. Gov't, Non-P.H.S.; Research Support, Non-U.S. Gov't