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Accretion simulations of Eta Carinae and implications to massive binaries

Published online by Cambridge University Press:  30 December 2019

Amit Kashi Open the ORCID record for Amit Kashi [Opens in a new window]
Amit Kashi*
Affiliation:
Department of Physics, Ariel University, Ariel, POB 3, 40700, Israel email: [email protected]
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Abstract

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Using high resolution 3D hydrodynamical simulations we quantify the amount of mass accreted onto the secondary star of the binary system η Carinae during periastron passage on its highly eccentric orbit. The accreted mass is responsible for the spectroscopic event occurring every orbit close to periastron passage, during which many lines vary and the x-ray emission associated with the destruction wind collision structure declines. The system is mainly known for its giant eruptions that occurred in the nineteenth century. The high mass model of the system, M1=170M⊙ and M2=80M⊙, gives Macc≍ 3×10−6M⊙ compatible with the amount required for explaining the reduction in secondary ionization photons during the spectroscopic event, and also matches its observed duration. As accretion occurs now, it surely occurred during the giant eruptions. This implies that mass transfer can have a huge influence on the evolution of massive stars.

Keywords

accretionaccretion disks — stars: mass loss — stars: variables: other — stars: windsoutflows — methods: numerical — (stars:) binaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 93 - 97
Copyright
© International Astronomical Union 2019 

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