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Article overview
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Recovery from Giant Eruptions in Very Massive Stars | | Amit Kashi
; Kris Davidson
; Roberta M. Humphreys
; | | Date: |
21 Oct 2015 | | Abstract: | We use a hydro-and-radiative-transfer code to explore the behavior of a very
massive star (VMS) after a giant eruption -- i.e., following a supernova
impostor event. Beginning with a reasonable model for an evolved VMS, we
simulate the change of state caused by a giant eruption via two methods that
explicitly conserve total energy: 1. Synthetically removing outer layers of
mass while reducing the energy of the inner layers. 2. Synthetically
transferring energy from the core to the outer layers, an operation that
automatically causes mass ejection. Our focus is on the aftermath, not the
poorly-understood eruption itself. Then, using a radiation-hydrodynamic code in
1D with realistic opacities and convection, the interior disequilibrium state
is followed for about 200 years. Typically the star develops a $sim 400
~
m{km}~
m{s}^{-1}$ wind with a mass loss rate that begins around $0.1
~M_odot~
m{yr^{-1}}$ and gradually decreases. This outflow is driven by
$kappa$-mechanism radial pulsations. In some cases a plateau in the mass loss
rate may persist about 200 years, while other cases are more like $eta$ Car’s
known history. These simulations constitute a useful preliminary reconnaissance
for 3D models which will be far more difficult. | | Source: | arXiv, 1510.6428 | | Services: | Forum | Review | PDF | Favorites | |
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