期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 455, 期 4, 页码 3511-3525出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2548
关键词
hydrodynamics; methods: numerical; binaries: close; stars: evolution
资金
- Australian Research Council [DP12013337, FT120100452]
- Alexander von Humboldt Foundation
- NASA [NNX14AJ56G]
- Australian Commonwealth Government
- NSF [TG-AST130034, ACI-1053575]
- Australian Research Council [FT120100452] Funding Source: Australian Research Council
The Rotten Egg Nebula has at its core a binary composed of a Mira star and an A-type companion at a separation > 10 au. It has been hypothesized to have formed by strong binary interactions between the Mira and a companion in an eccentric orbit during periastron passage similar to 800 yr ago. We have performed hydrodynamic simulations of an asymptotic giant branch (AGB) star interacting with companions with a range of masses in orbits with a range of initial eccentricities and periastron separations. For reasonable values of the eccentricity, we find that Roche lobe overflow can take place only if the periods are << 100 yr. Moreover, mass transfer causes the system to enter a common envelope phase within several orbits. Since the central star of the Rotten Egg nebula is an AGB star, we conclude that such a common envelope phase must have lead to a merger, so the observed companion must have been a tertiary companion of a binary that merged at the time of nebula ejection. Based on the mass and time-scale of the simulated disc formed around the companion before the common envelope phase, we analytically estimate the properties of jets that could be launched. Allowing for super-Eddington accretion rates, we find that jets similar to those observed are plausible, provided that the putative lost companion was relatively massive.
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