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Neutrinos from Fallback onto Newly Formed Neutron Stars
Astrophysics · Submitted 4 Nov 2007
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim But, as we shall show in this paper, in most supernova explosions, a tenth of a solar mass or more of the ejecta is decelerated enough that it does not escape the potential well of that compact object.
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The abstract, sentence by sentence
In the standard supernova picture, type Ib/c and type II supernovae are powered by the potential energy released in the collapse of the core of a massive star. In studying supernovae, we primarily focus on the ejecta that makes it beyond the potential well of the collapsed core. But, as we shall show in this paper, in most supernova explosions, a tenth of a solar mass or more of the ejecta is decelerated enough that it does not escape the potential well of that compact object. This material falls back onto the proto-neutron star within the first 10-15 seconds after the launch of the explosion, releasing more than 1e52erg of additional potential energy. Most of this energy is emitted in the form of neutrinos and we must understand this fallback neutrino emission if we are to use neutrino observations to study the behavior of matter at high densities. Here we present both a 1-dimensional study of fallback using energy-injected, supernova explosions and a first study of neutrino emission from fallback using a suite of 2-dimensional simulations.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In the standard supernova picture, type Ib/c and type II supernovae are powered by the potential energy released in the collapse of the core of a massive star. | background 1.00 | 0.04 | 0.02 | asserted 1.00 |
| s1 | In studying supernovae, we primarily focus on the ejecta that makes it beyond the potential well of the collapsed core. | background 0.98 | 0.14 | 0.02 | asserted 0.97 |
| s2 | But, as we shall show in this paper, in most supernova explosions, a tenth of a solar mass or more of the ejecta is decelerated enough that it does not escape the potential well of that compact object. | result 0.89 | 0.65 | 0.52 | asserted 0.97 |
| s3 | This material falls back onto the proto-neutron star within the first 10-15 seconds after the launch of the explosion, releasing more than 1e52erg of additional potential energy. | result 1.00 | 0.71 | 0.26 | asserted 1.00 |
| s4 | Most of this energy is emitted in the form of neutrinos and we must understand this fallback neutrino emission if we are to use neutrino observations to study the behavior of matter at high densities. | interpretation 0.45 | 0.16 | 0.19 | asserted 0.99 |
| s5 | Here we present both a 1-dimensional study of fallback using energy-injected, supernova explosions and a first study of neutrino emission from fallback using a suite of 2-dimensional simulations. | contribution 0.94 | 0.96 | 0.08 | asserted 0.99 |
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Original abstract
In the standard supernova picture, type Ib/c and type II supernovae are powered by the potential energy released in the collapse of the core of a massive star. In studying supernovae, we primarily focus on the ejecta that makes it beyond the potential well of the collapsed core. But, as we shall show in this paper, in most supernova explosions, a tenth of a solar mass or more of the ejecta is decelerated enough that it does not escape the potential well of that compact object. This material falls back onto the proto-neutron star within the first 10-15 seconds after the launch of the explosion, releasing more than 1e52erg of additional potential energy. Most of this energy is emitted in the form of neutrinos and we must understand this fallback neutrino emission if we are to use neutrino observations to study the behavior of matter at high densities. Here we present both a 1-dimensional study of fallback using energy-injected, supernova explosions and a first study of neutrino emission from fallback using a suite of 2-dimensional simulations.
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4 arXiv papers cite this in 4 sentences
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Cites it as background 1 paper
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The hydrodynamics of the matter infalling and accreting onto a NS at hypercritical rates has been extensively studied in different astrophysics contexts taking into account details on the neutrino emission, e.g., fallback accretion in SN [ref] , accreting NS in X-ray binaries [ref] , and for the case of BdHNe, we refer to [ref] for details.
The first minutes of a binary-driven hypernova · Simulation of the BdHN early evolution · 0.99
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