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 Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

2020 ◽  
Vol 641 ◽  
pp. L10
Author(s):  
Takashi J. Moriya ◽  
Pablo Marchant ◽  
Sergei I. Blinnikov
Keyword(s):  
Light Curve ◽  
Energy Input ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Core Collapse ◽  
Decay Energy ◽  
Slow Cooling ◽  
Gamma Ray Burst ◽  
The Core ◽  
Optical Light Curve

We show that the luminous supernovae associated with ultra-long gamma-ray bursts can be related to the slow cooling from the explosions of hydrogen-free progenitors that are extended by pulsational pair-instability. We have recently shown that some rapidly-rotating hydrogen-free gamma-ray burst progenitors that experience pulsational pair-instability can keep an extended structure caused by pulsational pair-instability until the core collapse. These types of progenitors have large radii exceeding 10 R⊙ and they sometimes reach beyond 1000 R⊙ at the time of the core collapse. They are, therefore, promising progenitors of ultra-long gamma-ray bursts. Here, we perform light-curve modeling of the explosions of one extended hydrogen-free progenitor with a radius of 1962 R⊙. The progenitor mass is 50 M⊙ and 5 M⊙ exists in the extended envelope. We use the one-dimensional radiation hydrodynamics code STELLA in which the explosions are initiated artificially by setting given explosion energy and 56Ni mass. Thanks to the large progenitor radius, the ejecta experience slow cooling after the shock breakout and they become rapidly evolving (≲10 days), luminous (≳1043 erg s−1) supernovae in the optical even without energy input from the 56Ni nuclear decay when the explosion energy is more than 1052 erg. The 56Ni decay energy input can affect the light curves after the optical light-curve peak and make the light-curve decay slowly when the 56Ni mass is around 1 M⊙. They also have a fast photospheric velocity above 10 000 km s−1 and a hot photospheric temperature above 10 000 K at around the peak luminosity. We find that the rapid rise and luminous peak found in the optical light curve of SN 2011kl, which is associated with the ultra-long gamma-ray burst GRB 111209A, can be explained as the cooling phase of the extended progenitor. The subsequent slow light-curve decline can be related to the 56Ni decay energy input. The ultra-long gamma-ray burst progenitors we proposed recently can explain both the ultra-long gamma-ray burst duration and the accompanying supernova properties. When the gamma-ray burst jet is off-axis or choked, the luminous supernovae could be observed as fast blue optical transients without accompanying gamma-ray bursts.

SN 1987a: A Progress Report

1987 ◽  
Vol 7 (2) ◽  
pp. 141-146 ◽  
Author(s):  
M. A. Dopita ◽  
N. Achilleos ◽  
J. A. Dawe ◽  
C. Flynn ◽  
S. J. Meatheringham ◽  
...  
Keyword(s):  
Light Curve ◽  
Thermal Energy ◽  
Radioactive Decay ◽  
Progress Report ◽  
Type Ii ◽  
Normal Type ◽  
Spectral Evolution ◽  
Core Mass ◽  
Sn 1987A ◽  
Residual Hydrogen

AbstractIt now appears almost certain that the precursor of SN 1987a was the brighter of the components of Sk-69 202, a blue supergiant, with a precursor mass of perhaps 12-16 solar masses. Prior to the explosion the precursor had a core mass of order six solar masses, and 0.1 to 0.2 solar masses of residual hydrogen envelope. The compact nature of this star can account for many of the odd features of the subsequent light curve and spectral evolution.An analysis of the light curve and colour evolution shows four distinct epochs, which probably relate to the initial expansion of the fireball and the escape of shock-deposited thermal energy, the hydrogen-rich layers becoming optically thin, the exposure of the helium core, and the increasing transparency of the helium core.The supernova appeared to be at its maximum on May 10, but is dimmer than a normal Type II because its light is apparently derived from recombinations and the radioactive decay of 56Ni to 56Co to 56Fe rather than by the thermal energy deposited by the passage of the shock.

scholarly journals Properties of gamma-ray decay lines in 3D core-collapse supernova models, with application to SN 1987A and Cas A

2020 ◽  
Vol 494 (2) ◽  
pp. 2471-2497 ◽  
Author(s):  
A Jerkstrand ◽  
A Wongwathanarat ◽  
H-T Janka ◽  
M Gabler ◽  
D Alp ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Radioactive Decay ◽  
Supernova Explosion ◽  
3D Models ◽  
Core Collapse ◽  
Line Profiles ◽  
Sn 1987A ◽  
And Shifts ◽  
Cas A ◽  
Explosive Burning

ABSTRACT Comparison of theoretical line profiles to observations provides important tests for supernova explosion models. We study the shapes of radioactive decay lines predicted by current 3D core-collapse explosion simulations, and compare these to observations of SN 1987A and Cas A. Both the widths and shifts of decay lines vary by several thousand kilometres per second depending on viewing angle. The line profiles can be complex with multiple peaks. By combining observational constraints from 56Co decay lines, 44Ti decay lines, and Fe IR lines, we delineate a picture of the morphology of the explosive burning ashes in SN 1987A. For MZAMS = 15−20 M⊙ progenitors exploding with ∼1.5 × 1051 erg, ejecta structures suitable to reproduce the observations involve a bulk asymmetry of the 56Ni of at least ∼400 km s−1 and a bulk velocity of at least 1500 km s−1. By adding constraints to reproduce the UVOIR bolometric light curve of SN 1987A up to 600 d, an ejecta mass around 14 M⊙ is favoured. We also investigate whether observed decay lines can constrain the neutron star (NS) kick velocity. The model grid provides a constraint VNS > Vredshift, and applying this to SN 1987A gives a NS kick of at least 500 km s−1. For Cas A, our single model provides a satisfactory fit to the NuSTAR observations and reinforces the result that current neutrino-driven core-collapse SN models achieve enough bulk asymmetry in the explosive burning material. Finally, we investigate the internal gamma-ray field and energy deposition, and compare the 3D models to 1D approximations.

scholarly journals The determination of the supernovae parameters from their light curves using the machine learning

2021 ◽  
pp. 1-11
Author(s):  
Egor Mikhailovich Urvachev
Keyword(s):  
Machine Learning ◽  
Light Curve ◽  
Learning Algorithm ◽  
Radioactive Decay ◽  
Light Curves ◽  
Radioactive Isotopes ◽  
Curve Model ◽  
Total Light ◽  
The Masses

The paper discusses the application of the machine learning library, CatBoost, to determine the masses of radioactive isotopes from the supernova light curve at a later epochs. The synthetic light curve model used for the demonstration is based on the contribution of the five major radioactive decay chains starting with <sup>56</sup>Ni, <sup>57</sup>Ni, <sup>44</sup>Ti, <sup>22</sup>Na, <sup>60</sup>Co. Separately, we considered sets of random light curves calculated for different isotope masses of both the three dominant chains (<sup>56</sup>Ni, <sup>57</sup>Ni, <sup>44</sup>Ti) and all five. It is shown that the masses of dominant isotopes are determined with acceptable accuracy in both cases, even with the standard settings of the machine learning algorithm. In the second case, the accuracy of determining the masses of the other two isotopes (<sup>22</sup>Na, <sup>60</sup>Co) turns out to be unsatisfactory, probably due to their weak contribution to the total light curve.

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.

Nuclear γ ray lines in the supernova SN 1987a

1991 ◽  
Vol 16 (4) ◽  
pp. 443-457
Author(s):  
R. Lehoucq ◽  
Ph. Durouchouxa
Keyword(s):  
Sn 1987A ◽  
Γ Ray

Self-glowing crystals–radioactive decay energy converters into optical emission

2021 ◽  
Vol 142 ◽  
pp. 111431
Author(s):  
M.V. Zamoryanskaya ◽  
E.V. Dementeva ◽  
K.N. Orekhova ◽  
V.A. Kravets ◽  
A.N. Trofimov ◽  
...  
Keyword(s):  
Radioactive Decay ◽  
Optical Emission ◽  
Decay Energy ◽  
Energy Converters

Self-Sustaining Immobilisation Processes

2003 ◽  
Author(s):  
Michael I. Ojovan ◽  
Olga K. Karlina ◽  
George A. Petrov ◽  
Igor A. Sobolev ◽  
Sergey A. Dmitriev ◽  
...  
Keyword(s):  
Chemical Reactions ◽  
Radioactive Decay ◽  
Decay Energy ◽  
Radiogenic Heat ◽  
Exothermal Chemical

As overview of self-sustaining immobilisation processes is given which describes also new thermochemical and radiogenic heat immobilising schemes based on utilization of both exothermal chemical reactions and radioactive decay energy.

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