Numerical Simulations of Cosmic-Ray Acceleration at Core-Collapse Supernovae

被引：0

作者：

Giacinti, Gwenael ^{[1
]}

Dwarkadas, Vikram ^{[2
]}

Marcowith, Alexandre ^{[3
]}

Chiavassa, Andrea ^{[4
]}

机构：

[1] Max Planck Inst Kernphys, Postfach 103980, D-69029 Heidelberg, Germany

[2] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[3] Univ Montpellier, Lab Univers & Particules Montpellier LUPM, CNRS, IN2P3, CC72,Pl Eugene Bataillon, F-34095 Montpellier 5, France

[4] Univ Cote DAzur, CNRS, Observ Cote DAzur, CS 34229, Nice, France

来源：

36TH INTERNATIONAL COSMIC RAY CONFERENCE, ICRC2019 | 2021年

关键词：

DIFFUSIVE SHOCK ACCELERATION;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Core-collapse supernovae exploding in dense winds are favorable sites for cosmic-ray (CR) acceleration to very high energies. We present our CR-radiation-hydrodynamics simulations of the explosion of a red supergiant. We study the evolution of the shock wave during the first day following core collapse, and estimate the time at which CR acceleration can start. We then calculate the maximum CR energy at the forward shock as a function of time, and show that it may already exceed 100 TeV only a few hours after shock breakout from the surface of the star.

引用

页数：8

共 26 条

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[22] The first days of Type II-P core collapse supernovae in the gamma-ray range
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[26] CORE-COLLAPSE MODEL OF BROADBAND EMISSION FROM SNR RX J1713.7-3946 WITH THERMAL X-RAYS AND GAMMA RAYS FROM ESCAPING COSMIC RAYS
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