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arXiv · 1807.11388

The short orbital period binary star at the heart of the planetary nebula M 3-1

David Jones·Henri M. J. Boffin·Paulina Sowicka·Brent Miszalski·Pablo Rodríguez-Gil·Miguel Santander-García·Romano L. M. Corradi
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Abstract

We present the discovery of a 3h5m orbital-period binary star at the heart of the planetary nebula M 3-1 - the shortest period photometrically-variable central star known and second only to V458 Vul, in general. Combined modelling of light and radial velocity curves reveals both components to be close to Roche-lobe-filling, strongly indicating that the central star will rapidly evolve to become a cataclysmic variable, perhaps experiencing a similar evolution to V458 Vul resulting in a nova eruption before the planetary nebula has fully dissipated. While the short orbital period and near Roche-lobe filling natures of both components make the central binary of M 3-1 an important test case with which to constrain the formation processes of cataclysmic variables, novae and perhaps even supernovae type Ia.

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David Jones, Henri M. J. Boffin, Paulina Sowicka, Brent Miszalski, Pablo Rodríguez-Gil, Miguel Santander-García, Romano L. M. Corradi. 2018-07-30. The short orbital period binary star at the heart of the planetary nebula M 3-1. https://doi.org/10.1093/mnrasl/sly142

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