A probable planetary companion to HD 39091 from the Anglo-Australian Planet Search

  1. Hugh R. A. Jones1,*,
  2. R. Paul Butler2,
  3. C. G. Tinney3,
  4. Geoffrey W. Marcy4,
  5. Alan J. Penny5,
  6. Chris McCarthy2,
  7. Brad D. Carter6,
  8. Dimitri Pourbaix7

Article first published online: 11 JUL 2002

DOI: 10.1046/j.1365-8711.2002.05459.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 333, Issue 4, pages 871–875, July 2002

Additional Information

How to Cite

Jones, H. R. A., Paul Butler, R., Tinney, C. G., Marcy, G. W., Penny, A. J., McCarthy, C., Carter, B. D. and Pourbaix, D. (2002), A probable planetary companion to HD 39091 from the Anglo-Australian Planet Search. Monthly Notices of the Royal Astronomical Society, 333: 871–875. doi: 10.1046/j.1365-8711.2002.05459.x

Author Information

  1. 1

    Astrophysics Research Institute, Liverpool John Moores University, Egerton Wharf, Birkenhead CH41 1LD

  2. 2

    Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015-1305, USA

  3. 3

    Anglo-Australian Observatory, PO Box 296, Epping 1710, Australia

  4. 4

    Department of Astronomy, University of California, Berkeley, CA 94720, USA

  5. 5

    Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX

  6. 6

    Faculty of Sciences, University of Southern Queensland, Toowoomba, QLD 4350, Australia

  7. 7

    Institut d'Astronomie et d'Astrophysique, Universite Libre de Bruxelles CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium

*hraj@astro.livjm.ac.uk

Publication History

  1. Issue published online: 11 JUL 2002
  2. Article first published online: 11 JUL 2002
  3. Accepted 2002 February 26. Received 2002 February 15; in original form 2001 November 29

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Keywords:

  • stars: individual: HD 39091;
  • stars: low-mass, brown dwarfs;
  • planetary systems

We report the detection of an extra-solar planet candidate orbiting the G1 V star HD 39091. The orbital period is 2049 d and the eccentricity is 0.62. With a minimum (M sin i) mass of 10.3MJUP this object falls near the high-mass end of the observed planet mass function, and may plausibly be a brown dwarf. Other characteristics of this system, including orbital eccentricity and metallicity, are typical of the well-populated class of radial velocity planets in eccentric orbits around metal-rich stars.

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