scholarly journals Neutrino flavor as a test of the explosion mechanism of core-collapse supernovae

2019 ◽  
Vol 99 (12) ◽  
Author(s):  
Nitsan Bar ◽  
Kfir Blum ◽  
Guido D’Amico
Keyword(s):  
Core Collapse ◽  
Neutrino Flavor ◽  
Explosion Mechanism

scholarly journals Stripped-envelope core-collapse supernova 56Ni masses

2020 ◽  
Vol 641 ◽  
pp. A177 ◽  
Author(s):  
N. Meza ◽  
J. P. Anderson
Keyword(s):  
Systematic Errors ◽  
Power Source ◽  
Radioactive Material ◽  
Estimation Methods ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Explosion Mechanism ◽  
The Difference ◽  
Uniform Manner ◽  
Lower Limits

Context. The mass of synthesised radioactive material is an important power source for all supernova (SN) types. In addition, the difference of 56Ni yields statistics are relevant to constrain progenitor paths and explosion mechanisms. Aims. Here, we re-estimate the nucleosynthetic yields of 56Ni for a well-observed and well-defined sample of stripped-envelope SNe (SE-SNe) in a uniform manner. This allows us to investigate whether the observed hydrogen-rich–stripped-envelope (SN II–SE SN) 56Ni separation is due to real differences between these SN types or because of systematic errors in the estimation methods. Methods. We compiled a sample of well-observed SE-SNe and measured 56Ni masses through three different methods proposed in the literature: first, the classic “Arnett rule”; second the more recent prescription of Khatami & Kasen (2019, ApJ, 878, 56) and third using the tail luminostiy to provide lower limit 56Ni masses. These SE-SN distributions were then compared to those compiled in this article. Results. Arnett’s rule, as previously shown, gives 56Ni masses for SE-SNe that are considerably higher than SNe II. While for the distributions calculated using both the Khatami & Kasen (2019, ApJ, 878, 56) prescription and Tail 56Ni masses are offset to lower values than “Arnett values”, their 56Ni distributions are still statistically higher than that of SNe II. Our results are strongly driven by a lack of SE-SN with low 56Ni masses, that are, in addition, strictly lower limits. The lowest SE-SN 56Ni mass in our sample is of 0.015 M⊙, below which are more than 25% of SNe II. Conclusions. We conclude that there exist real, intrinsic differences in the mass of synthesised radioactive material between SNe II and SE-SNe (types IIb, Ib, and Ic). Any proposed current or future CC SN progenitor scenario and explosion mechanism must be able to explain why and how such differences arise or outline a bias in current SN samples yet to be fully explored.

scholarly journals Enhanced mass-loss rate evolution of stars with ≳18 M⊙ and missing optically observed type II core-collapse supernovae

2020 ◽  
Vol 494 (4) ◽  
pp. 5230-5238
Author(s):  
Roni Anna Gofman ◽  
Naomi Gluck ◽  
Noam Soker
Keyword(s):  
Mass Loss ◽  
Loss Rate ◽  
Main Sequence ◽  
Mass Loss Rate ◽  
Core Collapse ◽  
Type Ii ◽  
Instability Strip ◽  
Stellar Envelope ◽  
Explosion Mechanism ◽  
Hydrogen Mass

ABSTRACT We evolve stellar models with zero-age main-sequence (ZAMS) mass of MZAMS ≳ 18 M⊙ under the assumption that they experience an enhanced mass-loss rate when crossing the instability strip at high luminosities and conclude that most of them end as type Ibc supernovae (SNe Ibc) or dust-obscured SNe II. We explore what level of enhanced mass-loss rate during the instability strip would be necessary to explain the ‘red supergiant problem’. This problem refers to the dearth of observed core-collapse supernovae progenitors with MZAMS ≳ 18 M⊙. Namely, we examine what enhanced mass-loss rate could make it possible for all these stars actually to explode as core-collapse supernovae (CCSNe). We find that the mass-loss rate should increase by a factor of at least about 10. We reach this conclusion by analysing the hydrogen mass in the stellar envelope and the optical depth of the dusty wind at the explosion, and crudely estimate that under our assumptions only about a fifth of these stars explode as unobscured SNe II and SNe IIb. About 10–15 per cent end as obscured SNe II that are infrared-bright but visibly very faint, and the rest, about 65–70 per cent, end as SNe Ibc. However, the statistical uncertainties are still too significant to decide whether many stars with MZAMS ≳ 18 M⊙ do not explode as expected in the neutrino driven explosion mechanism, or whether all of them explode as CCSNe, as expected by the jittering jets explosion mechanism.

scholarly journals Utilizing Supernova Remnants as Probes of Explosion Mechanisms and Progenitor Systems

2015 ◽  
Vol 11 (A29B) ◽  
pp. 225-226
Author(s):  
Dan Milisavljevic
Keyword(s):  
Supernova Remnants ◽  
Core Collapse ◽  
Interior Structure ◽  
Explosion Mechanism

AbstractTheory and observation strongly favor the notion that asymmetric explosions drive core-collapse supernovae, but where and how this asymmetry becomes introduced is uncertain. The most likely places of origin are in the explosion mechanism itself or the interior structure of the star into which the explosion proceeds. Investigating the recently uncovered bubble-like interiors of young, nearby supernova remnants may provide a way to unravel which of these competing processes dominate.

NEUTRINO CAPTURE INDUCED SUPERNOVA EXPLOSIONS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1483-1490 ◽  
Author(s):  
T. STROTHER ◽  
W. BAUER
Keyword(s):  
Kinetic Theory ◽  
Heavy Ion Collisions ◽  
Supernova Explosion ◽  
Heavy Ion ◽  
High Energy ◽  
Transport Equations ◽  
Core Collapse ◽  
Ion Collisions ◽  
Supernova Explosions ◽  
Explosion Mechanism

Motivated by the success of kinetic theory in the description of observables in intermediate and high energy heavy-ion collisions, we use kinetic theory to model the dynamics of core collapse supernovae. The specific way that we employ kinetic theory to solve the relevant transport equations allows us to explicitly model the propagation of neutrinos and a full ensemble of nuclei and treat neutrino–matter interactions in a very general way. With these abilities, our simulations have observed dynamics that may prove to be an entirely new neutrino capture induced supernova explosion mechanism.

scholarly journals The aspherical explosion of the Type IIP SN 2017gmr†

2019 ◽  
Vol 489 (1) ◽  
pp. L69-L74 ◽  
Author(s):  
T Nagao ◽  
A Cikota ◽  
F Patat ◽  
S Taubenberger ◽  
M Bulla ◽  
...  
Keyword(s):  
Spherical Symmetry ◽  
Significant Part ◽  
Core Collapse ◽  
Explosion Mechanism ◽  
Intrinsic Diversity ◽  
Early Rise

ABSTRACT Type IIP supernovae (SNe IIP), which represent the most common class of core-collapse (CC) SNe, show a rapid increase in continuum polarization just after entering the tail phase. This feature can be explained by a highly asymmetric helium core, which is exposed when the hydrogen envelope becomes transparent. Here we report the case of an SN IIP (SN 2017gmr) that shows an unusually early rise of the polarization, ≳30 d before the start of the tail phase. This implies that SN 2017gmr is an SN IIP that has very extended asphericity. The asymmetries are not confined to the helium core, but reach out to a significant part of the outer hydrogen envelope, hence clearly indicating a marked intrinsic diversity in the aspherical structure of CC explosions. These observations provide new constraints on the explosion mechanism, where viable models must be able to produce such extended deviations from spherical symmetry, and account for the observed geometrical diversity.

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