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Title:
A Third Giant Planet Orbiting HIP 14810
Authors:
Wright, J. T.; Fischer, D. A.; Ford, Eric B.; Veras, D.; Wang, J.; Henry, G. W.; Marcy, G. W.; Howard, A. W.; Johnson, John Asher
Affiliation:
AA(Department of Astronomy, 226 Space Sciences Building, Cornell University, Ithaca, NY 14853, USA ), AB(Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132, USA ), AC(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, P.O. Box 112055, Gainesville, FL 32611-2055, USA ), AD(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, P.O. Box 112055, Gainesville, FL 32611-2055, USA ), AE(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, P.O. Box 112055, Gainesville, FL 32611-2055, USA ), AF(Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209, USA ), AG(Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA ), AH(Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA ; Townes Fellow, Space Sciences Laboratory. ), AI(Institute for Astronomy, University of Hawai'i, Honolulu, HI 96822, USA ; NSF Postdoctoral Fellow.)
Publication:
The Astrophysical Journal Letters, Volume 699, Issue 2, pp. L97-L101 (2009). (ApJL Homepage)
Publication Date:
07/2009
Origin:
IOP
ApJ Keywords:
planetary systems, stars: individual: HIP 14810
DOI:
10.1088/0004-637X/699/2/L97
Bibliographic Code:
2009ApJ...699L..97W

Abstract

We present new precision radial velocities and a three-planet Keplerian orbit fit for the V = 8.5, G5 V star HIP 14810. We began observing this star at Keck Observatory as part of the N2K Planet Search Project. Wright et al. announced the inner two planets to this system, and subsequent observations have revealed the outer planet and the proper orbital solution for the middle planet. The planets have minimum masses of 3.9, 1.3, and 0.6 M Jup and orbital periods of 6.67, 147.7, and 952 day, respectively. We have numerically integrated the family of orbital solutions consistent with the data and find that they are stable for at least 106 yr. Our photometric search shows that the inner planet does not transit.
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