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

TL;DR

This study presents transit timing observations of the Hot Neptune exoplanet GL 436b, aiming to detect additional planets and analyze orbital dynamics through high-precision light curves.

Contribution

First detailed transit timing analysis of GL 436b, providing data for potential detection of smaller planets and orbital perturbations in this unique system.

Findings

High-precision light curves obtained from multiple telescopes.

Initial analysis discussed, with ongoing data collection planned.

Potential to detect Earth-mass planets through transit timing variations.

Abstract

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.