SUPERNOVAE, PROTONEUTRON STARS AND RELATED HIGH ENERGY PHENOMENA

We present a brief review of the present status of the standard model of core collapse supernovae and neutron star formation outlining the basic concepts and paying attention to the possibility of a transition to quark matter. We evaluate the consequences of this transition on the whole explosion mechanism, analyze the possible generation of beamed gamma ray bursts, and discuss the nature of the compact star born as a result of the supernova explosion.

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Abstracts

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312013701 ◽

2011 ◽

Vol 7 (S279) ◽

pp. 433-446

Keyword(s):

Gamma Ray ◽

Cosmological Parameters ◽

Supernova Explosion ◽

Wide Band ◽

High Energy ◽

Gamma Ray Bursts ◽

Core Collapse ◽

Host Galaxies ◽

Unique Type ◽

X Ray

Measuring cosmological parameters with GRBs: status and perspectivesNew interpretation of the Amati relationThe SED Machine - a dedicated transient spectrographPTF10iue - evidence for an internal engine in a unique Type Ic SNDirect evidence for the collapsar model of long gamma-ray burstsOn pair instability supernovae and gamma-ray burstsPan-STARRS1 observations of ultraluminous SNeThe influence of rotation on the critical neutrino luminosity in core-collapse supernovaeGeneral relativistic magnetospheres of slowly rotating and oscillating neutron starsHost galaxies of short GRBsGRB 100418A: a bridge between GRB-associated hypernovae and SNeTwo super-luminous SNe at z ~ 1.5 from the SNLSProspects for very-high-energy gamma-ray bursts with the Cherenkov Telescope ArrayThe dynamics and radiation of relativistic flows from massive starsThe search for light echoes from the supernova explosion of 1181 ADThe proto-magnetar model for gamma-ray burstsStellar black holes at the dawn of the universeMAXI J0158-744: the discovery of a supersoft X-ray transientWide-band spectra of magnetar burst emissionDust formation and evolution in envelope-stripped core-collapse supernovaeThe host galaxies of dark gamma-ray burstsKeck observations of 150 GRB host galaxiesSearch for properties of GRBs at large redshiftThe early emission from SNeSpectral properties of SN shock breakoutMAXI observation of GRBs and short X-ray transientsA three-dimensional view of SN 1987A using light echo spectroscopyX-ray study of the southern extension of the SNR Puppis AAll-sky survey of short X-ray transients by MAXI GSCDevelopment of the CALET gamma-ray burst monitor (CGBM)

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NEUTRINO CAPTURE INDUCED SUPERNOVA EXPLOSIONS

International Journal of Modern Physics D ◽

10.1142/s0218271810017895 ◽

2010 ◽

Vol 19 (08n10) ◽

pp. 1483-1490 ◽

Cited By ~ 2

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.

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No supernovae detected in two long-duration gamma-ray bursts

Philosophical Transactions of The Royal Society A Mathematical Physical and Engineering Sciences ◽

10.1098/rsta.2006.1994 ◽

2007 ◽

Vol 365 (1854) ◽

pp. 1269-1275 ◽

Cited By ~ 8

Author(s):

D Watson ◽

J.P.U Fynbo ◽

C.C Thöne ◽

J Sollerman

Keyword(s):

Massive Star ◽

Gamma Ray ◽

Compact Star ◽

Gamma Ray Bursts ◽

Host Galaxy ◽

Core Collapse ◽

Host Galaxies ◽

Star Forming ◽

Long Duration ◽

Spiral Arm

There is strong evidence that long-duration gamma-ray bursts (GRBs) are produced during the collapse of a massive star. In the standard version of the collapsar model, a broad-lined and luminous Type Ic core-collapse supernova (SN) accompanies the GRB. This association has been confirmed in observations of several nearby GRBs. Recent observations show that some long-duration GRBs are different. No SN emission accompanied the long-duration GRBs 060505 and 060614 down to limits fainter than any known Type Ic SN and hundreds of times fainter than the archetypal SN 1998bw that accompanied GRB 980425. Multi-band observations of the early afterglows, as well as spectroscopy of the host galaxies, exclude the possibility of significant dust obscuration. Furthermore, the bursts originated in star-forming galaxies, and in the case of GRB 060505, the burst was localized to a compact star-forming knot in a spiral arm of its host galaxy. We find that the properties of the host galaxies, the long duration of the bursts and, in the case of GRB 060505, the location of the burst within its host, all imply a massive stellar origin. The absence of an SN to such deep limits therefore suggests a new phenomenological type of massive stellar death.

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Time-dependent high-energy gamma-ray signal from accelerated particles in core-collapse supernovae: the case of SN 1993J

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa984 ◽

2020 ◽

Vol 494 (2) ◽

pp. 2760-2765 ◽

Cited By ~ 3

Author(s):

P Cristofari ◽

M Renaud ◽

A Marcowith ◽

V V Dwarkadas ◽

V Tatischeff

Keyword(s):

Gamma Ray ◽

Supernova Explosion ◽

Cosmic Ray ◽

High Energy ◽

Probability Of Detection ◽

Core Collapse ◽

Annihilation Process ◽

High Energy Gamma ◽

Energy Gamma ◽

Gamma Ray Attenuation

ABSTRACT Some core-collapse supernovae are likely to be efficient cosmic ray accelerators up to the PeV range, and therefore, to potentially play an important role in the overall Galactic cosmic ray population. The TeV gamma-ray domain can be used to study particle acceleration in the multi-TeV and PeV range. This motivates the study of the detectability of such supernovae by current and future gamma-ray facilities. The gamma-ray emission of core-collapse supernovae strongly depends on the level of the two-photon annihilation process: high-energy gamma-ray photons emitted at the expanding shock wave following the supernova explosion can interact with soft photons from the supernova photosphere through the pair production channel, thereby strongly suppressing the flux of gamma-rays leaving the system. In the case of SN 1993J, whose photospheric and shock-related parameters are well measured, we calculate the temporal evolution of the expected gamma-ray attenuation by accounting for the temporal and geometrical effects. We find the attenuation to be of about 10 orders of magnitude in the first few days after the supernova explosion. The probability of detection of a supernova similar to SN 1993J with the Cherenkov Telescope Array is highest if observations are performed either earlier than 1 d, or later than 10 d after the explosion, when the gamma-ray attenuation decreases to about two orders of magnitude.

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Supernovae, Gamma-Ray Bursts and Stellar Rotation

Symposium - International Astronomical Union ◽

10.1017/s0074180900196275 ◽

2004 ◽

Vol 215 ◽

pp. 601-612 ◽

Cited By ~ 13

Author(s):

S. E. Woosley ◽

A. Heger

Keyword(s):

Angular Momentum ◽

Neutron Star ◽

Gamma Ray ◽

Massive Stars ◽

Supernova Explosion ◽

Gamma Ray Bursts ◽

Iron Core ◽

Stellar Rotation ◽

Explosion Mechanism ◽

Stellar Mergers

One of the most dramatic possible consequences of stellar rotation is its influence on stellar death, particularly of massive stars. If the angular momentum of the iron core when it collapses is such as to produce a neutron star with a period of 5 ms or less, rotation will have important consequences for the supernova explosion mechanism. Still shorter periods, corresponding to a neutron star rotating at break up, are required for the progenitors of gamma-ray bursts (GRBs). Current stellar models, while providing an excess of angular momentum to pulsars, still fall short of what is needed to make GRBs. The possibility of slowing young neutron stars in ordinary supernovae by a combination of neutrino-powered winds and the propeller mechanism is discussed. The fall back of slowly moving ejecta during the first day of the supernova may be critical. GRBs, on the other hand, probably require stellar mergers for their production and perhaps less efficient mass loss and magnetic torques than estimated thus far.

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Constraining the fraction of core-collapse supernovae harbouring choked jets with high-energy neutrinos

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3245 ◽

2020 ◽

Vol 492 (1) ◽

pp. 843-847

Author(s):

Dafne Guetta ◽

Roi Rahin ◽

Imre Bartos ◽

Massimo Della Valle

Keyword(s):

Black Hole ◽

Gamma Ray ◽

High Energy ◽

Gamma Ray Bursts ◽

Core Collapse ◽

Stellar Envelope ◽

Jet Production ◽

Stellar Core ◽

High Fraction ◽

High Energy Neutrinos

ABSTRACT The joint observation of core-collapse supernovae with gamma-ray bursts shows that jets can be launched in the aftermath of stellar core collapse, likely by a newly formed black hole that accretes matter from the star. Such gamma-ray bursts have only been observed accompanying Type Ibc supernovae, indicating a stellar progenitor that lost its hydrogen envelope before collapse. According to recent hypothesis, it is possible that jets are launched in core-collapse events even when the progenitors still retain their hydrogen envelopes; however, such jets are not able to burrow through the star and will be stalled into the interior of the progenitor star before escaping. These jets are called choked jets. High-energy neutrinos produced by such choked jets could escape the stellar envelope and could be observed. Here, we examine how multimessenger searches for high-energy neutrinos and core-collapse supernovae can detect or limit the fraction of stellar collapses that produce jets. We find that a high fraction of jet production is already limited by previous observational campaigns. We explore possibilities with future observations using Large Synoptic Survey Telescope, IceCube, and Km3NET.

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