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Prog. Theor. Phys. Supplement No.158 (2005) pp. 24-42

[ Full Text PDF : FREE ACCESS (732K) ]

Observed Properties of Exoplanets: Masses, Orbits, and Metallicities

Geoffrey Marcy,1,* R. Paul Butler,2 Debra Fischer,3 Steven Vogt,4 Jason T. Wright,1 Chris G. Tinney5 and Hugh R. A. Jones6

1Astronomy Department, University of California, Berkeley, CA 94720, USA
2Department of Terrestrial Magnetism, Carnegie Institution of Washington,
5241 Broad Branch Rd NW, Washington DC 20015-1305, USA
3Department of Physics and Astronomy, San Francisco State University,
San Francisco, CA 94132, USA
4UCO/Lick Observatory, University of California at Santa Cruz,
Santa Cruz, CA 95064, USA
5Anglo-Australian Observatory, PO Box 296, Epping 1710, Australia
6Centre for Astrophysics Research, University of Hertfordshire,
Hatfield, AL10 9AB, UK

Abstract:

We review the observed properties of exoplanets found by the Doppler technique that has revealed 152 planets to date. We focus on the ongoing 18-year survey of 1330 FGKM type stars at Lick, Keck, and the Anglo-Australian Telescopes that offers both uniform Doppler precision (3 m s-1) and long duration. The 104 planets detected in this survey have minimum masses (M sin i) as low as 6 M Earth, orbiting between 0.02 and 6 AU. The core-accretion model of planet formation is supported by four observations: 1) The mass distribution rises toward the lowest detectable masses, dN/dM ∝M -1.0. 2) Stellar metallicity correlates strongly with the presence of planets. 3) One planet (1.3 M Sat) has a massive rocky core, M Core ≈ 70 M Earth. 4) A super-Earth of ∼ 7 M Earth has been discovered. The distribution of semi-major axes rises from 0.3 – 3.0 AU (dN/d log a) and extrapolation suggests that ∼12% of the FGK stars harbor gas-giant exoplanets within 20 AU. The median orbital eccentricity is <e >= 0.25, and even planets beyond 3 AU reside in eccentric orbits, suggesting that the circular orbits in our Solar System are unusual. The occurrence “hot Jupiters” within 0.1 AU of FGK stars is 1.2 ± 0.2%. Among stars with one planet, 14% have at least one additional planet, occasionally locked in resonances. Kepler and COROT will measure the occurrence of earth-sized planets. The Space Interferometry Mission (SIM) will detect planets with masses as low as 3 M Earth orbiting within 2 AU of stars within 10 pc, and it will measure masses, orbits, and multiplicity. The candidate rocky planets will be amenable to follow-up spectroscopy by the “Terrestrial Planet Finder” and Darwin.


URL : http://ptp.ipap.jp/link?PTPS/158/24/
DOI : 10.1143/PTPS.158.24


*E-mail: gmarcy@berkeley.edu

[ Full Text PDF : FREE ACCESS (732K) ] Citation:

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