dc.contributor.author | Marcy, G.W. | |
dc.contributor.author | Butler, R.P. | |
dc.contributor.author | Fischer, D.A. | |
dc.contributor.author | Vogt, S. | |
dc.contributor.author | Wright, J.T. | |
dc.contributor.author | Tinney, C.G. | |
dc.contributor.author | Jones, H.R.A. | |
dc.date.accessioned | 2007-07-08T20:14:17Z | |
dc.date.available | 2007-07-08T20:14:17Z | |
dc.date.issued | 2005 | |
dc.identifier.citation | Marcy , G W , Butler , R P , Fischer , D A , Vogt , S , Wright , J T , Tinney , C G & Jones , H R A 2005 , ' Observed Properties of Exoplanets: Masses, Orbits, and Metallicities ' , Progress of Theoretical Physics, Supplement , vol. 158 , pp. 24-42 . | |
dc.identifier.issn | 0375-9687 | |
dc.identifier.other | dspace: 2299/164 | |
dc.identifier.uri | http://hdl.handle.net/2299/164 | |
dc.description | The original publication is available at http://ptp.ipap.jp --Copyright Progress of Theoretical Physics 2005 | |
dc.description.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 MEarth, 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 MSat) has a massive rocky core, MCore ≈ 70 MEarth. 4) A super-Earth of ∼ 7 MEarth 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 MEarth 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. | en |
dc.format.extent | 749857 | |
dc.language.iso | eng | |
dc.relation.ispartof | Progress of Theoretical Physics, Supplement | |
dc.title | Observed Properties of Exoplanets: Masses, Orbits, and Metallicities | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Science & Technology Research Institute | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.description.status | Peer reviewed | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |