Affiliation:
1. Department of Physics, Technion - Israel Institute of Technology, Haifa 3200003, Israel
2. Guangdong Technion Israel Institute of Technology, Guangdong Province, Shantou 515069, China
Abstract
ABSTRACT
We study the evolution of six exoplanetary systems with the stellar evolutionary code Modules for Experiments in Stellar Astrophysics(mesa) and conclude that they will likely spin-up the envelope of their parent stars on the red giant branch (RGB) or later on the asymptotic giant branch (AGB) to the degree that the mass-loss process might become non-spherical. We choose six observed exoplanetary systems where the semimajor axis is $a_i \simeq 1\small{-}2 {~\rm au}$, and use the binary mode of mesa to follow the evolution of the systems. In four systems, the star engulfs the planet on the RGB, and in two systems on the AGB, and the systems enter a common envelope evolution (CEE). In two systems where the exoplanet masses are Mp ≃ 10MJ, where MJ is Jupiter mass, the planet spins up the envelope to about $10{{\ \rm per\ cent}}$ of the break-up velocity. Such envelopes are likely to have significant non-spherical mass-loss geometry. In the other four systems where Mp ≃ MJ the planet spins up the envelope to values of $1{-}2 {{\ \rm per\ cent}}$ of break-up velocity. Magnetic activity in the envelope that influences dust formation might lead to a small departure from spherical mass-loss even in these cases. In the two cases of CEE on the AGB, the planet deposits energy to the envelope that amounts to ${\gt}10{{\ \rm per\ cent}}$ of the envelope binding energy. We expect this to cause a non-spherical mass-loss that will shape an elliptical planetary nebula in each case.
Funder
Israel Science Foundation
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
7 articles.
订阅此论文施引文献
订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献