Late Evolution of SN 1987A

1988 ◽  
Vol 7 (4) ◽  
pp. 513-519
Author(s):  
Roger A. Chevalier
Keyword(s):  
Neutron Star ◽  
Shock Waves ◽  
Interstellar Medium ◽  
Neutrino Emission ◽  
Core Collapse ◽  
Sn 1987A ◽  
Light Echoes ◽  
Late Evolution

AbstractSN 1987A has illuminated a great diversity of astrophysical processes – from neutrino emission during core collapse to the structure of the interstellar medium on a scale of hundreds of parsecs. Here I cover the evolution of SN 1987A from the outside in; the topics are interstellar light echoes, circumstellar light echoes, circumstellar shock waves, late emission and structure of the ejecta, and the effects of a central neutron star.

scholarly journals Developing an end-to-end simulation framework of supernova neutrino detection

2020 ◽  
Author(s):  
Masamitsu Mori ◽  
Yudai Suwa ◽  
Ken’ichiro Nakazato ◽  
Kohsuke Sumiyoshi ◽  
Masayuki Harada ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutrino Emission ◽  
Neutrino Detectors ◽  
Sn 1987A ◽  
Neutrino Detection ◽  
Time Simulation ◽  
Consistent Manner ◽  
Long Time ◽  
Neutron Star Cooling ◽  
Proto Neutron Star

Abstract Massive stars can explode as supernovae at the end of their life cycle, releasing neutrinos whose total energy reaches 1053erg. Moreover, neutrinos play key roles in supernovae, heating and reviving the shock wave as well as cooling the resulting proto-neutron star. Therefore, neutrino detectors are waiting to observe the next galactic supernova and several theoretical simulations of supernova neutrinos are underway. While these simulation concentrate mainly on only the first one second after the supernova bounce, the only observation of a supernova with neutrinos, SN 1987A, revealed that neutrino emission lasts for more than 10 seconds. For this reason, long-time simulation and analysis tools are needed to compare theories with the next observation. Our study is to develop an integrated supernova analysis framework to prepare an analysis pipeline for treating galactic supernovae observations in the near future. This framework deals with the core-collapse, bounce and proto-neutron star cooling processes, as well as with neutrino detection on earth in a consistent manner. We have developed a new long-time supernova simulation in one dimension that explodes successfully and computes the neutrino emission for up to 20 seconds. Using this model we estimate the resulting neutrino signal in the Super-Kamiokande detector to be about 1,800 events for an explosion at 10 kpc and discuss its implications in this paper. We compare this result with the SN 1987A observation to test its reliability.

A Three-dimensional Study Using Light Echoes of the Structure of the Interstellar Medium in Front of SN 1987A

1995 ◽  
Vol 451 ◽  
pp. 806 ◽  
Author(s):  
Jun Xu ◽  
Arlin P. S. Crotts ◽  
William E. Kunkel
Keyword(s):  
Interstellar Medium ◽  
Three Dimensional ◽  
Sn 1987A ◽  
Light Echoes

SN 1987A: the Light Curve

1991 ◽  
Vol 9 (1) ◽  
pp. 105-106 ◽  
Author(s):  
Patricia Whitelock ◽  
John Menzies ◽  
John A. R. Caldwell
Keyword(s):  
Light Curve ◽  
Radioactive Decay ◽  
Radioactive Isotopes ◽  
Core Collapse ◽  
Additional Contribution ◽  
Decay Energy ◽  
Sn 1987A ◽  
Total Luminosity ◽  
Light Echoes ◽  
Γ Ray

AbstractThe changing total luminosity of SN 1987A between 2 and 1200 days after core collapse is illustrated and discussed. From about four weeks after outburst the supernova light curve was dominated by the release of radioactive decay energy; the major contributor being 0.078M⊙ of 56Co. Recently an additional contribution probably from the decay of 57Co and 44Ti appears to be manifesting itself in the light curve. A gradually increasing fraction of the radioactive decay energy has probably been emitted at X- and γ-ray wavelengths; the fluxes are low and no recent measurements have been published. Most of the remaining radioactive decay energy appears to be emitted in the IR and is very difficult to measure. Other factors influencing the interpretation of the recent light curve are the uncertain contribution from long-lived radioactive isotopes and light-echoes. It is therefore premature to make any definitive statements on the contribution from the neutron star, although it is probably less than a few times 1037 erg s−1.

scholarly journals The evolution of dust in the local and high-redshift universe

2015 ◽  
Vol 11 (A29B) ◽  
pp. 182-183
Author(s):  
Eli Dwek ◽  
Richard G. Arendt ◽  
Johannes Staguhn ◽  
Tea Temim
Keyword(s):  
Shock Waves ◽  
Interstellar Medium ◽  
Size Distribution ◽  
High Redshift ◽  
Magellanic Clouds ◽  
Core Collapse ◽  
Agb Stars ◽  
Dust Production ◽  
Great Debate ◽  
High Redshift Universe

AbstractDust is a ubiquities component of the interstellar medium (ISM) of galaxies, and manifests itself in many different ways. Yet, its origin, composition, and size distribution are still a matter of great debate. Most of the thermally condensed dust is produced in the explosively expelled ejecta of core collapse supernovae (CCSNe) and in the quiescent winds of AGB stars. Following its injection into the ISM it is destroyed by supernova (SN) shock waves. Knowing the relative rates of these processes is crucial for understanding the nature and evolution of dust in galaxies. In the following we will review three aspects of the evolution of dust in galaxies: the evolution of dust in the ejecta of SN1987A; the rates of dust production and destruction rates in the Magellanic Clouds (MCs), and the evolution of dust in CLASH 2882, a gravitationally-lensed galaxy at z=1.

scholarly journals SUPERNOVA 1987A: CELEBRATING A SILVER JUBILEE

2013 ◽  
Vol 53 (A) ◽  
pp. 606-611
Author(s):  
Nino Panagia
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Massive Star ◽  
Core Collapse ◽  
Single Star ◽  
The Core ◽  
Sn 1987A ◽  
Supernova 1987A ◽  
Collapse Process

The story of the SN 1987A explosion is briefly reviewed. Although this supernova was somewhat peculiar, the study of SN 1987A has clarified quite a number of important aspects of the nature and the properties of supernovae, such as the confirmation of the core collapse of a massive star as the cause of the explosion, as well the confirmation that the decays 56Ni–56Co–56Fe at early times and 44Ti–44Sc at late times, are the main sources of the energy radiated by the ejecta. Still we have not been able to ascertain whether the progenitor was a single star or a binary system, nor have we been able to detect the stellar remnant, a neutron star that should be produced in the core collapse process.

A Three-dimensional Study Using Light Echoes of the Structure of the Interstellar Medium in Front of SN 1987A: Erratum

1996 ◽  
Vol 463 ◽  
pp. 391 ◽  
Author(s):  
Jun Xu ◽  
Arlin P. S. Crotts ◽  
William E. Kunkel
Keyword(s):  
Interstellar Medium ◽  
Three Dimensional ◽  
Sn 1987A ◽  
Light Echoes

Protoneutron Star Formation

1988 ◽  
Vol 7 (4) ◽  
pp. 371-381
Author(s):  
Adam Burrows
Keyword(s):  
Star Formation ◽  
Neutron Star ◽  
General Analysis ◽  
Sn 1987A ◽  
Supernova Neutrino ◽  
Neutrino Theory ◽  
Protoneutron Star

AbstractThe theory of neutron star formation is addressed in the light of the detected neutrino burst from SN 1987A. A brief review of how supernova neutrino theory has evolved over the last 30 years and a general analysis of the SN 1987A detections is presented.

scholarly journals THE PROGENITOR DEPENDENCE OF THE PRE-EXPLOSION NEUTRINO EMISSION IN CORE-COLLAPSE SUPERNOVAE

2012 ◽  
Vol 762 (2) ◽  
pp. 126 ◽  
Author(s):  
Evan O'Connor ◽  
Christian D. Ott
Keyword(s):  
Neutrino Emission ◽  
Core Collapse

scholarly journals A shallow water analogue of asymmetric core-collapse, and neutron star kick/spin

2011 ◽  
Vol 7 (S279) ◽  
pp. 134-137
Author(s):  
Thierry Foglizzo ◽  
Frédéric Masset ◽  
Jérôme Guilet ◽  
Gilles Durand
Keyword(s):  
Neutron Star ◽  
Shallow Water ◽  
Acoustic Waves ◽  
Large Scale ◽  
Massive Stars ◽  
Core Collapse ◽  
Hydraulic Jumps ◽  
Core Collapse Supernova ◽  
Accretion Shock

AbstractMassive stars end their life with the gravitational collapse of their core and the formation of a neutron star. Their explosion as a supernova depends on the revival of a spherical accretion shock, located in the inner 200km and stalled during a few hundred milliseconds. Numerical simulations suggest that the large scale asymmetry of the neutrino-driven explosion is induced by a hydrodynamical instability named SASI. Its non radial character is able to influence the kick and the spin of the resulting neutron star. The SWASI experiment is a simple shallow water analog of SASI, where the role of acoustic waves and shocks is played by surface waves and hydraulic jumps. Distances in the experiment are scaled down by a factor one million, and time is slower by a factor one hundred. This experiment is designed to illustrate the asymmetric nature of core-collapse supernova.

SN 1987A: Optical Spectrophotometry 130–900 Days After Core Collapse

Supernovae ◽  
1991 ◽  
pp. 36-48 ◽  
Author(s):  
M. M. Phillips ◽  
R. E. Williams
Keyword(s):  
Core Collapse ◽  
Sn 1987A ◽  
Optical Spectrophotometry
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