1 | Note that some stars in ![]() ![]() |
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2 | Currently, there are major discussions on the details of the drive in the convection above the proto neutron star. Instabilities can be driven by the post–bounce-shock entropy profile, neutrino heating, or the standing accretion shock instability (SASI). Similarly, debate surrounds the magnitude of the entropy/lepton driven convection within the proto neutron star. | |
3 | Müller & Janka [208![]() ![]() |
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4 | The term “proto black hole” is used to describe the large (above ![]() |
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5 | Our models of these collapsing cores are also sensitive to the numerical modeling of the physics as well as uncertainties in the physics, both leading to the current variety in results between different simulations. | |
6 | In accretion, Rayleigh–Taylor instabilities occur due to entropy gradients in the envelope set up by accretion [101![]() ![]() |
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7 | These different supernova types are thought to differ primarily based on the envelope left on the star at collapse, not based on a different collapse mechanism: type II supernovae still have a hydrogen envelope, whereas type Ib/c SNe have lost their hydrogen, and for the type Ic SNe, most of its helium, envelopes. | |
8 | Fryer & Young [116![]() ![]() |
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9 | Neutrino emission is tied to electron spin, which is made anisotropic by strong magnetic fields [170, 120]. | |
10 | The possible exception is extremely massive stars above ![]() ![]() |
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11 | This “softening” of the equation of state has been studied for three decades [322]. | |
12 | Even the more pessimistic/realistic estimates of the rate of neutron-star mergers predict that such a detection will occur within a few years of operation. |
http://www.livingreviews.org/lrr-2011-1 |
Living Rev. Relativity 14, (2011), 1
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