Core-Collapse Supernova Explosion Simulations: The Path to and Necessity for 3D Models

2009 ◽  
Author(s):  
Adam Burrows ◽  
Jason Nordhaus ◽  
Ivan Hubeny ◽  
James M. Stone ◽  
Keith MacGregor ◽  
...  
Keyword(s):  
Supernova Explosion ◽  
3D Models ◽  
Core Collapse ◽  
Core Collapse Supernova

scholarly journals A successful 3D core-collapse supernova explosion model

2018 ◽  
Vol 482 (1) ◽  
pp. 351-369 ◽  
Author(s):  
David Vartanyan ◽  
Adam Burrows ◽  
David Radice ◽  
M Aaron Skinner ◽  
Joshua Dolence
Keyword(s):  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova

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 DENSE IRON EJECTA AND CORE-COLLAPSE SUPERNOVA EXPLOSION IN THE YOUNG SUPERNOVA REMNANT G11.2-0.3

2009 ◽  
Vol 703 (1) ◽  
pp. L81-L85 ◽  
Author(s):  
Dae-Sik Moon ◽  
Bon-Chul Koo ◽  
Ho-Gyu Lee ◽  
Keith Matthews ◽  
Jae-Joon Lee ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Young Supernova Remnant

scholarly journals Gravitational wave signatures ofab initiotwo-dimensional core collapse supernova explosion models for12–25  M⊙stars

2015 ◽  
Vol 92 (8) ◽  
Author(s):  
Konstantin N. Yakunin ◽  
Anthony Mezzacappa ◽  
Pedro Marronetti ◽  
Shin’ichirou Yoshida ◽  
Stephen W. Bruenn ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
M Stars

scholarly journals The KM3NeT potential for the next core-collapse supernova observation with neutrinos

2021 ◽  
Vol 81 (5) ◽  
Author(s):  
S. Aiello ◽  
A. Albert ◽  
S. Alves Garre ◽  
Z. Aly ◽  
A. Ambrosone ◽  
...  
Keyword(s):  
Sea Water ◽  
Neutrino Flux ◽  
Supernova Explosion ◽  
Time Profile ◽  
Core Collapse ◽  
Spectral Parameters ◽  
Core Collapse Supernova ◽  
Neutrino Astrophysics ◽  
Under Construction ◽  
Accretion Shock

AbstractThe KM3NeT research infrastructure is under construction in the Mediterranean Sea. It consists of two water Cherenkov neutrino detectors, ARCA and ORCA, aimed at neutrino astrophysics and oscillation research, respectively. Instrumenting a large volume of sea water with $$\sim {6200}$$ ∼ 6200 optical modules comprising a total of $$\sim {200{,}000}$$ ∼ 200 , 000 photomultiplier tubes, KM3NeT will achieve sensitivity to $$\sim {10} \ \mathrm{MeV}$$ ∼ 10 MeV neutrinos from Galactic and near-Galactic core-collapse supernovae through the observation of coincident hits in photomultipliers above the background. In this paper, the sensitivity of KM3NeT to a supernova explosion is estimated from detailed analyses of background data from the first KM3NeT detection units and simulations of the neutrino signal. The KM3NeT observational horizon (for a $$5\,\sigma $$ 5 σ discovery) covers essentially the Milky-Way and for the most optimistic model, extends to the Small Magellanic Cloud ($$\sim {60} \ \mathrm{kpc}$$ ∼ 60 kpc ). Detailed studies of the time profile of the neutrino signal allow assessment of the KM3NeT capability to determine the arrival time of the neutrino burst with a few milliseconds precision for sources up to 5–8 kpc away, and detecting the peculiar signature of the standing accretion shock instability if the core-collapse supernova explosion happens closer than 3–5 kpc, depending on the progenitor mass. KM3NeT’s capability to measure the neutrino flux spectral parameters is also presented.

The Three Dimensional MHD Effects For Core Collapse Supernova Explosion

2008 ◽  
Author(s):  
Hayato Mikami ◽  
Yuji Sato ◽  
Tomoaki Matsumoto ◽  
Tomoyuki Hanawa ◽  
Ye-Fei Yuan ◽  
...  
Keyword(s):  
Three Dimensional ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova

scholarly journals Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations

2019 ◽  
Vol 489 (2) ◽  
pp. 2227-2246 ◽  
Author(s):  
David Vartanyan ◽  
Adam Burrows ◽  
David Radice
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
3D Models ◽  
Temporal Variations ◽  
Neutrino Energy ◽  
Mode Frequency ◽  
Core Collapse ◽  
Time Dynamics ◽  
Core Collapse Supernova ◽  
Proto Neutron Star

Abstract We provide the time series and angular distributions of the neutrino and gravitational wave emissions of 11 state-of-the-art 3D non-rotating core-collapse supernova models and explore correlations between these signatures and the real-time dynamics of the shock and the proto-neutron star (PNS) core. The neutrino emissions are roughly isotropic on average, with instantaneous excursions about the mean inferred luminosity of as much as ±20 per cent. The deviation from isotropy is least for the ‘νμ’-type neutrinos and the lowest mass progenitors. Instantaneous temporal luminosity variations along a given direction for exploding models average ∼2–4 per cent, but can be as high as ∼10 per cent. For non-exploding models, they can achieve ∼25 per cent. The temporal variations in the neutrino emissions correlate with the temporal and angular variations in the mass accretion rate. We witness the lepton-number emission self-sustained asymmetry (LESA) phenomenon in all our models and find that the vector direction of the LESA dipole and that of the inner Ye distribution are highly correlated. For our entire set of 3D models, we find strong connections between the cumulative neutrino energy losses, the radius of the proto-neutron star, and the f-mode frequency of the gravitational wave emissions. When physically normalized, the progenitor-to-progenitor variation in any of these quantities is no more than ∼10 per cent. Moreover, the reduced f-mode frequency is independent of time after bounce to better than ∼10 per cent. Therefore, simultaneous measurement of gravitational waves and neutrinos from a given supernova event can be used synergistically to extract real physical quantities of the supernova core.

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