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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