Transit Timing Observations of the Extrasolar Hot-Neptune Planet GL 436b

Details Transit Timing Observations of the Extrasolar Hot-Neptune Planet GL 436b Transit Timing Observations of the Extrasolar Hot-Neptune Planet GL 436b

2009-01-03

arxiv.org/abs/0901.0343v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

4 pages, 3 figures. To appear in "Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun", 2009

Scientific paper

10.1063/1.3099153

Gliese 436 is an M dwarf with a mass of 0.45 Msun and hosts the extrasolar planet GL 436b [3, 6, 7, 2], which is currently the least massive transiting planet with a mass of ~23.17 Mearth [10], and the only planet known to transit an M dwarf. GL 436b represents the first transiting detection of the class of extrasolar planets known as "Hot Neptunes" that have masses within a few times that of Neptune's mass (~17 Mearth) and orbital semimajor axis <0.1 AU about the host star. Unlike most other known transiting extrasolar planets, GL 436b has a high eccentricity (e~0.16). This brings to light a new parameter space for habitability zones of extrasolar planets with host star masses much smaller than typical stars of roughly a solar mass. This unique system is an ideal candidate for orbital perturbation and transit-time variation (TTV) studies to detect smaller, possibly Earth-mass planets in the system. In April 2008 we began a long-term intensive campaign to obtain complete high-precision light curves using the Apache Point Observatory's 3.5-meter telescope, NMSU's 1-meter telescope (located at APO), and Sommers Bausch Observatory's 24" telescope. These light curves are being analyzed together, along with amateur and other professional astronomer observations. Results of our analysis are discussed. Continued measurements over the next few years are needed to determine if additional planets reside in the system, and to study the impact of other manifestations on the light curves, such as star spots and active regions.

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