Jets in Common Envelopes: a low mass main sequence star in a red giant. (arXiv:2110.02227v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Camara_D/0/1/0/all/0/1">Diego Lopez-Camara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colle_F/0/1/0/all/0/1">Fabio De Colle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendez_E/0/1/0/all/0/1">Enrique Moreno Mendez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shiber_S/0/1/0/all/0/1">Sagiv Shiber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iaconi_R/0/1/0/all/0/1">Roberto Iaconi</a>
We present small scale three dimensional hydrodynamical simulations of the
evolution of a 0.3Msun main sequence star which launches two perpendicular jets
within the envelope of a 0.88Msun red giant. Based on the large scale
simulations of Shiber et al. (2019), we study the dynamics of the jets either
when the secondary star is grazing the envelope of the red giant, or when it
has plunged-in the envelope. The dynamics of the jets through the common
envelope (CE) depend on the conditions of the environment as well as on the jet
power. Jets are successful in removing the envelope during the early grazing
envelope phase and the initial plunge-in CE phases. Deep inside the CE, the
jets are drowned. High luminosity emission going from X-rays to UV and optical
is expected when the jets break out of the CE. We find that the mass accretion
onto the MS star is 1-10% of the Bondi Hoyle Littleton rate. The amount of
angular momentum accreted on to the secondary is not large enough to form a
disk. Our study shows the benefits of coupling large scale models with small
scale as the global evolution can critically depend on the small scale
phenomena.
We present small scale three dimensional hydrodynamical simulations of the
evolution of a 0.3Msun main sequence star which launches two perpendicular jets
within the envelope of a 0.88Msun red giant. Based on the large scale
simulations of Shiber et al. (2019), we study the dynamics of the jets either
when the secondary star is grazing the envelope of the red giant, or when it
has plunged-in the envelope. The dynamics of the jets through the common
envelope (CE) depend on the conditions of the environment as well as on the jet
power. Jets are successful in removing the envelope during the early grazing
envelope phase and the initial plunge-in CE phases. Deep inside the CE, the
jets are drowned. High luminosity emission going from X-rays to UV and optical
is expected when the jets break out of the CE. We find that the mass accretion
onto the MS star is 1-10% of the Bondi Hoyle Littleton rate. The amount of
angular momentum accreted on to the secondary is not large enough to form a
disk. Our study shows the benefits of coupling large scale models with small
scale as the global evolution can critically depend on the small scale
phenomena.
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