RECORD
A Dip after the Early Emission of Super-Luminous Supernovae: A Signature of Shock Breakout within Dense Circumstellar Media
High Energy Astrophysical Phenomena · Submitted 7 Mar 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In this Letter, we suggest new diagnostics to discriminate the strong SN-CSM interaction scenario from the others: a decline in the luminosity ('dip') before the main peak of the light curve.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
The origin of super-luminous supernovae (SLSNe), especially the source of their huge luminosities, has not been clarified yet. While a strong interaction between SN ejecta and dense circumstellar media (CSM) is a leading scenario, alternative models have been proposed. In this Letter, we suggest new diagnostics to discriminate the strong SN-CSM interaction scenario from the others: a decline in the luminosity ('dip') before the main peak of the light curve. This dip is an unavoidable consequence of having a dense CSM within which the shock breakout occurs. If a dense CSM shell is located far at large radii from the progenitor inside, it takes time for the SN ejecta to reach it and the early light curve can be powered by the SN ejecta before the collision. Once the SN ejecta collides with the dense CSM, the electron density and thus the Thomson scattering opacity suddenly increase. Photons become unable to go out of the shock even if there is a source of emission inside, which results in the dip in the light curve. This dip is a solid prediction from the strong interaction scenario irrespective of a power source for the early emission. Eventually the forward shock breaks out from within the dense CSM, and the luminosity increases by the continuous strong SN-CSM interaction, resulting in an SLSN. The possible dip observed in the hydrogen-poor SLSN, 2006oz, could be the first example of this signature and give support to the SN-CSM interaction as the power source of SLSN 2006oz.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The origin of super-luminous supernovae (SLSNe), especially the source of their huge luminosities, has not been clarified yet. | gap 0.69 | 0.03 | 0.02 | asserted 0.98 |
| s1 | While a strong interaction between SN ejecta and dense circumstellar media (CSM) is a leading scenario, alternative models have been proposed. | background 1.00 | 0.04 | 0.02 | asserted 0.62 |
| s2 | In this Letter, we suggest new diagnostics to discriminate the strong SN-CSM interaction scenario from the others: a decline in the luminosity ('dip') before the main peak of the light curve. | contribution 1.00 | 0.80 | 0.57 | hedged possibility 0.87 |
| s3 | This dip is an unavoidable consequence of having a dense CSM within which the shock breakout occurs. | interpretation 0.51 | 0.41 | 0.45 | asserted 1.00 |
| s4 | If a dense CSM shell is located far at large radii from the progenitor inside, it takes time for the SN ejecta to reach it and the early light curve can be powered by the SN ejecta before the collision. | interpretation 0.56 | 0.14 | 0.04 | asserted 0.69 |
| s5 | Once the SN ejecta collides with the dense CSM, the electron density and thus the Thomson scattering opacity suddenly increase. | interpretation 0.58 | 0.14 | 0.04 | asserted 1.00 |
| s6 | Photons become unable to go out of the shock even if there is a source of emission inside, which results in the dip in the light curve. | interpretation 0.80 | 0.26 | 0.13 | asserted 1.00 |
| s7 | This dip is a solid prediction from the strong interaction scenario irrespective of a power source for the early emission. | interpretation 0.56 | 0.52 | 0.38 | asserted 1.00 |
| s8 | Eventually the forward shock breaks out from within the dense CSM, and the luminosity increases by the continuous strong SN-CSM interaction, resulting in an SLSN. | interpretation 0.47 | 0.19 | 0.22 | asserted 1.00 |
| s9 | The possible dip observed in the hydrogen-poor SLSN, 2006oz, could be the first example of this signature and give support to the SN-CSM interaction as the power source of SLSN 2006oz. | interpretation 0.87 | 0.26 | 0.20 | hedged possibility 1.00 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
The origin of super-luminous supernovae (SLSNe), especially the source of their huge luminosities, has not been clarified yet. While a strong interaction between SN ejecta and dense circumstellar media (CSM) is a leading scenario, alternative models have been proposed. In this Letter, we suggest new diagnostics to discriminate the strong SN-CSM interaction scenario from the others: a decline in the luminosity ('dip') before the main peak of the light curve. This dip is an unavoidable consequence of having a dense CSM within which the shock breakout occurs. If a dense CSM shell is located far at large radii from the progenitor inside, it takes time for the SN ejecta to reach it and the early light curve can be powered by the SN ejecta before the collision. Once the SN ejecta collides with the dense CSM, the electron density and thus the Thomson scattering opacity suddenly increase. Photons become unable to go out of the shock even if there is a source of emission inside, which results in the dip in the light curve. This dip is a solid prediction from the strong interaction scenario irrespective of a power source for the early emission. Eventually the forward shock breaks out from within the dense CSM, and the luminosity increases by the continuous strong SN-CSM interaction, resulting in an SLSN. The possible dip observed in the hydrogen-poor SLSN, 2006oz, could be the first example of this signature and give support to the SN-CSM interaction as the power source of SLSN 2006oz.
Human review
How the literature uses it
1 arXiv paper cite this in 1 sentence
What it cites · 2 sentences without a confident label
Cites as support 1 paper
-
The dip is an inevitable consequence of the shock breakout within the dense CSM ( [ref] , see also [ref] ).
Optical to X-rays supernovae light curves following shock breakout through a thick wind · Introduction · 0.98
Cites as background 3 papers
-
For these H-poor SLSNe, several mechanisms to power the LCs have been suggested, including an interaction of SN ejecta with C+O-rich dense CSM [ref] , a spin-down of a highly-magnetized neutron star [ref] , or a quark nova model [ref] .
Supernova Explosions inside Carbon-Oxygen Circumstellar Shells · Introduction · 0.85
-
For these H-poor SLSNe, several mechanisms to power the LCs have been suggested, including an interaction of SN ejecta with C+O-rich dense CSM [ref] , a spin-down of a highly-magnetized neutron star [ref] , or a quark nova model [ref] .
The peculiar case of the "double-humped" super-luminous supernova SN2006oz · Introduction · 0.85
-
Mechanisms by which WR stars experience such a huge mass loss just before the explosion have not yet been clarified, although there are some suggestions [ref] .
Wave-Driven Mass Loss in the Last Year of Stellar Evolution: Setting the Stage for the Most Luminous Core-Collapse Supernovae · Dense Circumstellar Medium around SN 2006oz · 0.84
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.