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A High Eccentricity Component in the Double Planet System Around HD 163607 and a Planet Around HD 164509 | | Matthew J. Giguere
; Debra A. Fischer
; Andrew W. Howard
; John A. Johnson
; Gregory W. Henry
; Jason T. Wright
; Geoffrey W. Marcy
; Howard T. Isaacson
; Fengji Hou
; Julien Spronck
; | | Date: |
14 Sep 2011 | | Abstract: | We report the detection of three new exoplanets from Keck Observatory. HD
163607 is a metal-rich G5IV star with two planets. The inner planet has an
observed orbital period of 75.29 $pm$ 0.02 days, a semi-amplitude of 51.1
$pm$ 1.4 ms, an eccentricity of 0.73 $pm$ 0.02 and a derived minimum mass of
msini = 0.77 $pm$ 0.02 mjup. This is the largest eccentricity of any known
planet in a multi-planet system. The argument of periastron passage is 78.7
$pm$ 2.0$^{circ}$; consequently, the planet’s closest approach to its parent
star is very near the line of sight, leading to a relatively high transit
probability of 8%. The outer planet has an orbital period of 3.60 $pm$ 0.02
years, an orbital eccentricity of 0.12 $pm$ 0.06 and a semi-amplitude of 40.4
$pm$ 1.3 ms. The minimum mass is msini = 2.29 $pm$ 0.16 mjup. HD 164509 is
a metal-rich G5V star with a planet in an orbital period of 282.4 $pm$ 3.8
days and an eccentricity of 0.26 $pm$ 0.14. The semi-amplitude of 14.2 $pm$
2.7 ms implies a minimum mass of 0.48 $pm$ 0.09 mjup. The radial velocities
of HD 164509 also exhibit a residual linear trend of -5.1 $pm$ 0.7 ms per
year, indicating the presence of an additional longer period companion in the
system. Photometric observations demonstrate that HD 163607 and HD 164509 are
constant in brightness to sub-millimag levels on their radial velocity periods.
This provides strong support for planetary reflex motion as the cause of the
radial velocity variations. | | Source: | arXiv, 1109.2955 | | Services: | Forum | Review | PDF | Favorites | |
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