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Doppler Detection of Extrasolar Planets

Published online by Cambridge University Press:  12 April 2016

G. W. Marcy ,
R. Paul Butler  and
D. A. Fischer
G. W. Marcy*
Affiliation:
Dept. of Physics and Astronomy, San Francisco State Univ., San Francisco, CA 94132
R. Paul Butler
Affiliation:
Anglo-Australian Observatory, NSW 2121, Epping, Australia
D. A. Fischer
Affiliation:
Dept. of Physics and Astronomy, San Francisco State Univ., San Francisco, CA 94132
*
1Astronomy Department, University of California, Berkeley, CA 94720

Abstract

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We have measured the radial velocities of 540 G and K main sequence stars with a precision of 3−10 ms−1 using the Lick and Keck échelle spectrometers. We had detected 6 companions that have m sin i < 7 MJup. We announce here the discovery of a new planet around Gliese 876, found in our Doppler measurements from both Lick and Keck. This is the first planet found around an M dwarf, which indicates that planets occur around low-mass stars, in addition to solar-type stars. We combine our entire stellar sample with that of Mayor et al. to derive general properties of giant planets within a few AU of these stars. Less than 1% of G and K main sequence stars harbor brown dwarf companions with masses between 5 and 70 MJup. Including Gliese 876b, 8 companions exhibit m sin i < 5 MJup which constitute the best planet candidates to date. Apparently, 4% of stars have planetary companions within the range m sin i = 0.5 to 5 MJup. Planets are distinguished from brown dwarfs by the discontinuous jump in the mass function at 5 MJup. About 2/3 of the planets orbit within just 0.3 AU due in part to their favorable detectability, but also possibly due to a real “pile up” of planets near the star. Inward orbital migration after formation may explain this, but the mechanism to stop the migration remains unclear. Five of eight planets have orbital eccentricities greater than that of our Jupiter, eJup = 0.048, and tidal circularization may explain most of the circular orbits. Thus, eccentric orbits are common and may arise from gravitational interactions with other planets, stars, or the protoplanetary disk. The planet-bearing stars are systematically metal-rich, as is the Sun, compared to the solar neighborhood.

Type
Part 3. Extrasolar Planets
Information
International Astronomical Union Colloquium , Volume 170: Precise Stellar Radial Velocities , 1999 , pp. 121 - 130
Copyright
Copyright © Astronomical Society of the Pacific 1999

References

Artymowicz, P. 1997. in Proceedings of the Workshop, Brown Dwarfs and Extrasolar Planets, held at Tenerife, Spain, March 1997, ed. Rebolo, R.,Martín, E.L., Zapatero Osorio, M.R., 152–161.Google Scholar
Butler, R.P., Marcy, G.W., Williams, E., McCarthy, C., Dosanjh, P., & Vogt, S.S. 1996, PASP, 108, 500.Google Scholar
Butler, R.P., Marcy, G.W., Williams, E., Hauser, H. & Shirts, P. 1997, ApJ, 474, L115.Google Scholar
Cochran, W.D., Hatzes, A.P., Butler, R.P. & Marcy, G.W. 1997, ApJ, 483, 457.CrossRefGoogle Scholar
Delfosse, X., Forveille, T., Perrier, C., Mayor, M. 1998, A&A, 331, 581.Google Scholar
Latham, D., Mazeh, T., Stefanik, R.P., Mayor, M., Burki, G. 1989, Nature, 339, 38 Google Scholar
Levison, H.F., Lissauer, J.J., Duncan, M.J. 1998, AJ, in press.Google Scholar
Lin, D.N.C., Bodenheimer, P. & Richardson, D.C. 1996, Nature, 380, 606.Google Scholar
Lin, D.N.C., Ida, S. 1997. Ap. J. 477, 781 Google Scholar
Lissauer, J.J. 1995. Icarus 114, 217 Google Scholar
Marcy, G.W. & Butler, R.P. 1998, ARAA, 36, 57.Google Scholar
Mayor, M., Queloz, D., Udry, S. & Halbwachs, J.-L. 1997, in Astronomical and biochemical origins and search for life in the Universe, IAU Coll. 161, ed. Cosmovici, C.B., Bowyer, S., and Werthimer, D., p.313 Google Scholar
Mayor, M., Queloz, D., Udry, S. & Halbwachs, J.-L. 1999, To appear in Precise Radial Velocities, IAU Coll. 170, to appear in ASP Conference Series.Google Scholar
Noyes, R.W., Jha, S., Korzennik, S.G., Krockenberger, M., Nisenson, P., Brown, T.M., Kennelly, E.J., Horner, S.D. 1997, Ap.J.Lett. 483, L111 Google Scholar
Perryman, M.C. et al. 1997, A&A, 323, L49. The Hipparcos CatalogGoogle Scholar
Rasio, F.A. & Ford, E.B. 1996. Science 274, 954 Google Scholar
Terquem, C., Papaloizou, J.C.B., Nelson, R.P. & Lin, D.N.C. 1998, ApJ, 502, 788 CrossRefGoogle Scholar
Trilling, D., Benz, W., Guillot, T., Lunine, J.I., Hubbard, W.B., Burrows, A., 1998, Ap.J., 500, 428 CrossRefGoogle Scholar
Vogt, S.S. 1987, PASP, 99, 1214.CrossRefGoogle Scholar
Vogt, S.S. et al. 1994, Proc. Soc. Photo-Opt. Instr. Eng., 2198, 362 Google Scholar
Weidenschilling, S.J. & Marzari, F. 1996.Nature 384, 619 Google Scholar