X-ray Emission from the Binary Central Stars of the Planetary Nebulae HFG 1, DS 1, and LoTr 5

TL;DR

This study detects X-ray emissions from three binary central stars of planetary nebulae, supporting models that predict coronal activity in late-type companions due to binary interactions.

Contribution

First detection of X-ray emission from binary central stars in planetary nebulae, confirming models of coronal activity induced by binary interactions.

Findings

X-ray spectra characterized by two thermal plasma components (~10 MK and 15-40 MK)

X-ray luminosities around 10^30 erg/s

X-ray emission likely originates from coronae of late-type companions

Abstract

Close binary systems undergoing mass transfer or common envelope interactions can account for the morphological properties of some planetary nebulae. The search for close binary companions in planetary nebulae is hindered by the difficulty of detecting cool, late-type, main sequence companions in binary systems with hot pre-white dwarf primaries. However, models of binary PN progenitor systems predict that mass accretion or tidal interactions can induce rapid rotation in the companion, leading to X-ray-emitting coronae. To test such models, we have searched for, and detected, X-ray emission from three binary central stars within planetary nebulae: the post-common envelope close binaries in HFG 1 and DS 1 consisting of O-type subdwarfs with late-type, main sequence companions, and the binary system in LoTr 5 consisting of O-type subdwarf and rapidly rotating, late-type giant companion. The X-ray emission in each case is best characterized by spectral models consisting of two optically-thin thermal plasma components with characteristic temperatures of about 10 MK and 15-40 MK, and total X-ray luminosities about 10^30 erg/s. We consider the possible origin of the X-ray emission from these binary systems and conclude that the most likely origin is, in each case, a corona around the late-type companion, as predicted by models of interacting binaries.