See Also
 |
Table: Properties of Nearby Exoplanets. Includes both orbital and physical characteristics. | |
 |
Table: Properties of Exoplanet Host Stars. With stellar coordinates and distance, as well as physical parameters. |
Planets and Their Orbital Properties
Minimum Mass Distribution
Minimum mass distribution of the 167 known nearby exoplanets with M sin i < 15
MJup. The mass distribution shows a dramatic decrease in the number of planets at high
masses, a decrease that is roughly characterized by a power law, dN/dM ~ M-1.16. Lower mass
planets have smaller Doppler amplitudes, so the relevent selection effects enhance this
effect. This distribution represents results from many surveys, and so is drawn from an
inhomogeneous sample.
Orbital Distance Distribution
Orbital distance distribution of the 167 known nearby exoplanets with 0.03 <
a < 10 in logarithmic distance bins. Planets with a > 3AU have periods comparable to or
longer than the length of most Doppler surveys, so the distribution is incomplete beyond
that distance. This distribution represents results from many surveys, and so is drawn from
an inhomogeneous sample.
Distribution of Periods
Distribution of periods among the known nearby “hot Jupiters”. There is a
clear “pile-up” of planets with orbital periods near 3 days. Doppler surveys generally have
uniform sensitivity to hot Jupiters, so for massive planets, there is no important selection
effect contributing to the 3-day pile-up. This distribution represents results from many
surveys, and so is drawn from an inhomogeneous sample.
Minimum mass vs. semimajor axis
Minimum mass as a function of semimajor axis for the 164 known nearby exoplanets
with 0.03 < a < 6.5 AU. Doppler surveys are generally incomplete for exoplanets with
a > 3 AU, low-mass planets (M sin i < 1MJup) beyond 1 AU, and very low-mass planets
(M sin i < 0.1MJup) everywhere. This plot represents results from many surveys, and so is
drawn from an inhomogeneous sample.
Orbital eccentricity vs. semimajor axis
Orbital eccentricity as a function of semimajor axis for the 168 known nearby
exoplanets. Planets within 0.1 AU are presumably tidally circularized. Beyond 0.1 AU,
the distribution of eccentricities appears essentially uniform between 0 and 0.8. For most
Doppler surveys, sensitivity is not a strong function of eccentricity for 0 < e < 0.8 and a < 3
AU. This plot represents results from many surveys, and so is drawn from an inhomogeneous
sample.
Orbital eccentricities vs. minimum mass
Distribution of orbital eccentricities as a function of minimum mass for the
130 known nearby exoplanets with M sin i < 13MJup, excluding those for which a < 0.1
AU, i.e., those planets which may have been tidally circularized. High-mass exoplanets
(M sin i > 5MJup) have a slightly higher median eccentricity than lower-mass exoplanets.
The completeness of Doppler surveys increases with M sin i and is generally insensitive to
eccentricity. This distribution represents results from many surveys, and so is drawn from
an inhomogeneous sample.
Planets Announced June 2006
A Planet Around HD 11964
Best-fit orbit to the radial velocities measured at Keck Observatory for HD 11964,
with P = 5.8yr, e ~ 0, and M sin i = 0.6MJup.
A Planet Around HD 66428
Best-fit orbit to the radial velocities measured at Keck Observatory for HD 66428,
with P = 5.4yr, e = 0.5, and M sin i = 3MJup.
A Planet Around HD 99109
Best-fit orbit to the radial velocities measured at Keck Observatory for HD 99109,
with P = 1.2yr, e ~ 0, and M sin i = 0.5MJup.
A Planet Around HD 107148
Best-fit orbit to the radial velocities measured at Keck Observatory for HD 107148,
with P = 48d, e ~ 0, and M sin i = 0.2MJup.
A Planet Around HD 164922
Best-fit orbit to the radial velocities measured at Keck Observatory for HD 164922,
with P = 3.2yr, e ~ 0, and M sin i = 0.4MJup.