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First Simulations of Core- Collapse Supernovae to Supernova Remnants with SNSPH
Solar and Stellar Astrophysics · Submitted 17 May 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These calculations demonstrate the role that supernova instabilities (the instabilities that develop as the shock drive through the star) play in defining the structure and long-term development of instabilities in supernova remnants.
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The abstract, sentence by sentence
We present the first 3-dimensional simulations following the evolution of supernova shocks from their inception in the stellar core through the development of a supernova remnant into the Sedov phase. Our set of simulations use two different progenitors and two different conditions for the structure of the circumstellar environment. These calculations demonstrate the role that supernova instabilities (the instabilities that develop as the shock drive through the star) play in defining the structure and long-term development of instabilities in supernova remnants. We also present a first investigation of the mixing between stellar and interstellar matter as the supernova evolves into a young supernova remnant.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present the first 3-dimensional simulations following the evolution of supernova shocks from their inception in the stellar core through the development of a supernova remnant into the Sedov phase. | contribution 1.00 | 0.96 | 0.16 | asserted 0.99 |
| s1 | Our set of simulations use two different progenitors and two different conditions for the structure of the circumstellar environment. | method 0.98 | 0.92 | 0.03 | asserted 0.98 |
| s2 | These calculations demonstrate the role that supernova instabilities (the instabilities that develop as the shock drive through the star) play in defining the structure and long-term development of instabilities in supernova remnants. | interpretation 0.73 | 0.90 | 0.57 | asserted 1.00 |
| s3 | We also present a first investigation of the mixing between stellar and interstellar matter as the supernova evolves into a young supernova remnant. | contribution 0.99 | 0.94 | 0.08 | asserted 0.91 |
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The paper
Original abstract
We present the first 3-dimensional simulations following the evolution of supernova shocks from their inception in the stellar core through the development of a supernova remnant into the Sedov phase. Our set of simulations use two different progenitors and two different conditions for the structure of the circumstellar environment. These calculations demonstrate the role that supernova instabilities (the instabilities that develop as the shock drive through the star) play in defining the structure and long-term development of instabilities in supernova remnants. We also present a first investigation of the mixing between stellar and interstellar matter as the supernova evolves into a young supernova remnant.
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References
How the literature uses it
9 arXiv papers cite this in 13 sentences
Papers citing it · 8 sentences without a confident label
Compares with it 2 papers
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In contrast to our explosion modeling, [ref] launched their explosions in 1D and followed the propagation of a spherical blast wave from the C-O core into the He layer.
Production and Distribution of $^{44}$Ti and $^{56}$Ni in a Three-dimensional Supernova Model Resembling Cassiopeia A · Initial model · 0.85
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The extent of the mixing falls between the few studies that have addressed stripped-envelope supernovae of Type Ib/c and IIb with consistent [ref] or artificially altered [ref] envelope structures.
Multi-D Simulations of Ultra-Stripped Supernovae to Shock Breakout · Extent of Mixing · 1.00
Cites it as background 2 papers
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Inspired by the SN 1987A event a large number of multi-D simulations studying the growth of RTIs at different composition shell interfaces (e.g. C+O/He and He/H interfaces) inside the progenitor star have been performed [ref] .
The infancy of core-collapse supernova remnants · Introduction · 0.88
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The question of mixing in Type Ib/c SNe is in fact relevant not only for ultra-stripped progenitors, but for the entire class of hydrogen-free progenitors, and has so far been explored only to a very limited extent even in parameterised 2D models [ref] — in contrast to the very extensive body of computational studies on mixing in Type II SNe such as SN 1987A [ref] and Cas A [ref] .
Multi-D Simulations of Ultra-Stripped Supernovae to Shock Breakout · Introduction · 0.88
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