The post-common-envelope binary central star of the planetary nebula ETHOS 1. Issue 4 (11th September 2020)

• Record Type: Journal Article
• Authors: Munday, James; Jones, David; García-Rojas, Jorge; Boffin, Henri M J; Miszalski, Brent; Corradi, Romano L M; Rodríguez-Gil, Pablo; Rubio-Díez, María del Mar; Santander-García, Miguel; Sowicka, Paulina
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Issue 4(2020)
• Page Start: 6005
• Page End: 6012
• Publication Date: 2020-09-11
• Subjects: stars: AGB and post-AGB -- binaries: close -- planetary nebulae: individual: PN G068.1+11.0 -- white dwarfs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2753
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present a detailed study of the binary central star of the planetary nebula ETHOS 1 (PN G068.1+11.0). Simultaneous modelling of light and radial velocity curves reveals the binary to comprise a hot and massive pre-white dwarf with an M-type main-sequence companion. A good fit to the observations was found with a companion that follows expected mass–temperature–radius relationships for low-mass stars, indicating that despite being highly irradiated, it is consistent with not being significantly hotter or larger than a typical star of the same mass. Previous modelling indicated that ETHOS 1 may comprise the first case where the orbital plane of the central binary does not lie perpendicular to the nebular symmetry axis, at odds with the expectation that the common envelope is ejected in the orbital plane. We find no evidence for such a discrepancy, deriving a binary inclination in agreement with that of the nebula as determined by spatio-kinematic modelling. This makes ETHOS 1 the ninth post-common-envelope planetary nebula in which the binary orbital and nebular symmetry axes have been shown to be aligned, with as yet no known counter-examples. The probability of finding such a correlation by chance is now less than 0.000 02 per cent.