Circumbinary Planets Orbiting the sdB Binary NY Virginis: An Updated Two Planet Solution. (arXiv:1812.01726v1 [astro-ph.EP])

Circumbinary Planets Orbiting the sdB Binary NY Virginis: An Updated Two Planet Solution. (arXiv:1812.01726v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Song_S/0/1/0/all/0/1">Shuo Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mai_X/0/1/0/all/0/1">Xinyu Mai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mutel_R/0/1/0/all/0/1">Robert L. Mutel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pulley_D/0/1/0/all/0/1">Dvaid Pulley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faillace_G/0/1/0/all/0/1">George Faillace</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Watkins_A/0/1/0/all/0/1">Americo Watkins</a>

We report 18 new primary minima timing observations of the short-period
eclipsing binary system NY Virginis. We combined these minima with previously
published primary minima to update circumbinary exoplanet models in this system
based on O-C timing variations. We performed a non-linear least-squares
minimization search using a quadratic ephemeris and either one or two
exoplanets. The only model with an acceptable fit includes a period derivative
($dot{P} = -2.09times10^{-12}$) and two planets in eccentric orbits with
minimum masses 2.9 and 4.9 Jovian masses. However, a number of model parameters
are highly degenerate, so additional observations are required to determine
planetary parameters with high statistical confidence.

We report 18 new primary minima timing observations of the short-period
eclipsing binary system NY Virginis. We combined these minima with previously
published primary minima to update circumbinary exoplanet models in this system
based on O-C timing variations. We performed a non-linear least-squares
minimization search using a quadratic ephemeris and either one or two
exoplanets. The only model with an acceptable fit includes a period derivative
($dot{P} = -2.09times10^{-12}$) and two planets in eccentric orbits with
minimum masses 2.9 and 4.9 Jovian masses. However, a number of model parameters
are highly degenerate, so additional observations are required to determine
planetary parameters with high statistical confidence.

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