A giant planet orbiting the ‘extreme horizontal branch’ star V 391 Pegasi

R. Silvotti (), S. Schuh, R. Janulis, J.-E. Solheim, S. Bernabei, R. Østensen, T. D. Oswalt, I. Bruni, R. Gualandi, A. Bonanno, G. Vauclair, M. Reed, C.-W. Chen, E. Leibowitz, M. Paparo, A. Baran, S. Charpinet, N. Dolez, S. Kawaler, D. Kurtz, P. Moskalik, R. Riddle and S. Zola
Additional contact information
R. Silvotti: INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
S. Schuh: Institut für Astrophysik, Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
R. Janulis: Institute of Theoretical Physics and Astronomy, Vilnius University, 12 A. Gostauto Street, 01108 Vilnius, Lithuania
J.-E. Solheim: Institutt for Teoretisk Astrofysikk, Universitetet i Oslo, PB 1029 Blindern, 0315, Norway
S. Bernabei: INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
R. Østensen: K. U. Leuven, Institute of Astronomy, Celestijnenlaan 200D, 3001 Leuven, Belgium
T. D. Oswalt: Florida Institute of Technology, 150 West University Boulevard, Melbourne, Florida 32901, USA
I. Bruni: INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
R. Gualandi: INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
A. Bonanno: INAF-Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy
G. Vauclair: CNRS-UMR5572, Observatoire Midi-Pyrénées, Université Paul Sabatier, 14 avenue Edouard Belin, 31400 Toulouse, France
M. Reed: Astronomy and Materials Science, Missouri State University, 901 S. National, Springfield, Missouri 65897, USA
C.-W. Chen: Institute of Astronomy, National Central University, 300 Jhongda Road, Chung-Li 32054, Taiwan
E. Leibowitz: Wise Observatory, Tel Aviv University
M. Paparo: Konkoly Observatory, P O Box 67, H-1525 Budapest XII, Hungary
A. Baran: Cracow Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland
S. Charpinet: CNRS-UMR5572, Observatoire Midi-Pyrénées, Université Paul Sabatier, 14 avenue Edouard Belin, 31400 Toulouse, France
N. Dolez: CNRS-UMR5572, Observatoire Midi-Pyrénées, Université Paul Sabatier, 14 avenue Edouard Belin, 31400 Toulouse, France
S. Kawaler: 12 Physics Hall, Iowa State University, Ames, Iowa 50011, USA
D. Kurtz: Centre for Astrophysics, University of Central Lancashire
P. Moskalik: Copernicus Astronomical Centre, ul. Bartycka 18, 00-716 Warsaw, Poland
R. Riddle: Thirty Meter Telescope Project, 2632 E. Washington Blvd, Pasadena, California 91107, USA
S. Zola: Cracow Pedagogical University, ul. Podchorazych 2, 30-084 Cracow, Poland

Nature, 2007, vol. 449, issue 7159, 189-191

Abstract: Planets in the red Most of the more than 200 known extrasolar planets orbit main sequence stars similar to our Sun. When the hydrogen in their cores runs out, they will become red giants that can easily reach and engulf inner planets. This will happen to the Sun in about five billion years. After that the fate of Earth is uncertain, but the discovery of a planet orbiting a post-red-giant phase star suggests that it may survive in some form. The planet is in orbit 1.7 astronomical units (AU) from V 391 Pegasi. The maximum radius of the red giant phase was about 0.7 AU, and the distance of the planet during main sequence phase 1 AU. This shows that planets with orbital distances of less than 2 AU (which by definition includes the Sun) can survive the red giant expansion.

Date: 2007
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DOI: 10.1038/nature06143

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