scholarly journals Astrophysical explosions: from solar flares to cosmic gamma-ray bursts

2012 ◽  
Vol 370 (1960) ◽  
pp. 774-799 ◽  
Author(s):  
J. Craig Wheeler
Keyword(s):  
Neutron Stars ◽  
Energy Release ◽  
Solar Flares ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Accretion Discs ◽  
Stellar Flares ◽  
Crossing Time ◽  
Dynamical Time ◽  
New Research

Astrophysical explosions result from the release of magnetic, gravitational or thermonuclear energy on dynamical time scales, typically the sound-crossing time for the system. These explosions include solar and stellar flares, eruptive phenomena in accretion discs, thermonuclear combustion on the surfaces of white dwarfs and neutron stars, violent magnetic reconnection in neutron stars, thermonuclear and gravitational collapse supernovae and cosmic gamma-ray bursts, each representing a different type and amount of energy release. This paper summarizes the properties of these explosions and describes new research on thermonuclear explosions and explosions in extended circumstellar media. Parallels are drawn between studies of terrestrial and astrophysical explosions, especially the physics of the transition from deflagration-to-detonation.

Giant flares in soft γ -ray repeaters and short GRBs

2007 ◽  
Vol 365 (1854) ◽  
pp. 1307-1313 ◽  
Author(s):  
S Zane
Keyword(s):  
Neutron Stars ◽  
Energy Release ◽  
Gamma Ray ◽  
Rare Events ◽  
Gamma Ray Bursts ◽  
Current Scenario ◽  
Γ Ray ◽  
Short Grbs

Soft gamma-ray repeaters (SGRs) are a peculiar family of bursting neutron stars that, occasionally, have been observed to emit extremely energetic giant flares (GFs), with energy release up to approximately 10 47  erg s −1 . These are exceptional and rare events. It has been recently proposed that GFs, if emitted by extragalactic SGRs, may appear at Earth as short gamma-ray bursts. Here, I will discuss the properties of the GFs observed in SGRs, with particular emphasis on the spectacular event registered from SGR 1806-20 in December 2004. I will review the current scenario for the production of the flare, within the magnetar model, and the observational implications.

The melting of neutron stars' crystalline cores and gamma-ray bursts

1976 ◽  
Vol 39 (1) ◽  
pp. 243-249 ◽  
Author(s):  
Ju. M. Bruk ◽  
K. I. Kugel
Keyword(s):  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts

Gamma-ray bursts from galactic neutron stars?

1989 ◽  
Vol 10 (2) ◽  
pp. 27-37
Author(s):  
D. Hartmann ◽  
R.I. Epstein ◽  
S.E. Woosley
Keyword(s):  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts

scholarly journals Variabilities of gamma-ray bursts from black hole hyper-accretion discs

2016 ◽  
Vol 463 (1) ◽  
pp. 245-250 ◽  
Author(s):  
Da-Bin Lin ◽  
Zu-Jia Lu ◽  
Hui-Jun Mu ◽  
Tong Liu ◽  
Shu-Jin Hou ◽  
...  
Keyword(s):  
Black Hole ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Accretion Discs

scholarly journals Gamma-rays from Solar Flares

2000 ◽  
Vol 195 ◽  
pp. 123-132 ◽  
Author(s):  
R. Ramaty ◽  
N. Mandzhavidze
Keyword(s):  
Energy Release ◽  
Gamma Rays ◽  
Solar Flares ◽  
Gamma Ray ◽  
Particle Interaction ◽  
Mass Motion ◽  
Relativistic Electrons ◽  
Total Energy Release ◽  
Flare Energy ◽  
Accelerated Particles

Gamma-ray emission is the most direct diagnostic of energetic ions and relativistic electrons in solar flares. Analysis of solar flare gamma-ray data has shown: (i) ion acceleration is a major consequence of flare energy release, as the total flare energy in accelerated particles appears to be equipartitioned between ≳ 1 MeV/nucleon ions and ≳ 20 keV electrons, and amounts to an important fraction of the total energy release; (ii) there are flares for which over 50% of the energy is in a particles and heavier ions; (iii) in both impulsive and gradual flares, the particles that interact at the Sun and produce gamma rays are essentially always accelerated by the same mechanism that operates in impulsive flares, probably stochastic acceleration through gyroresonant wave particle interaction; and (iv) gamma-ray spectroscopy can provide new information on solar abundances, for example the site of the FIP-bias onset and the photospheric 3He abundance. We propose a new technique for the investigation of mass motion and mixing in the solar atmosphere: the observations of gamma-ray lines from long-term radioactivity produced by flare accelerated particles.

Study of Solar Flares and Gamma-Ray Bursts in the Helicon Experiment

2013 ◽  
pp. 393-403 ◽  
Author(s):  
E. P. Mazets ◽  
R. L. Aptekar ◽  
S. V. Golenetskii ◽  
V. N. Il’inskii ◽  
V. D. Pal’shin ◽  
...  
Keyword(s):  
Solar Flares ◽  
Gamma Ray ◽  
Gamma Ray Bursts

scholarly journals Acceleration Processes for Gamma-Ray Bursts

1994 ◽  
Vol 142 ◽  
pp. 869-876 ◽  
Author(s):  
Igor G. Mitrofanov
Keyword(s):  
Particle Acceleration ◽  
Electric Field ◽  
Neutron Stars ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Initial Energy ◽  
Gamma Ray Bursts ◽  
Acceleration Of Particles ◽  
Radiation Mechanisms ◽  
Radiative Pressure

AbstractIs it shown that for those astronomical models of cosmic gamma-ray bursts (GRBs) which are associated with galactic neutron stars (NSs), the initial energy of the outburst could be converted to gamma-rays through processes of particle acceleration. The main emission mechanisms are considered for two basic alternatives, when particles are accelerated either by radiative pressure or by an electric field.Subject headings: acceleration of particles — gamma rays: bursts — radiation mechanisms: nonthermal

scholarly journals Astrophysical implications of neutron star inspiral and coalescence

2020 ◽  
Vol 29 (11) ◽  
pp. 2041015
Author(s):  
John L. Friedman ◽  
Nikolaos Stergioulas
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Maximum Mass ◽  
X Ray ◽  
Spectral Bands ◽  
Heaviest Elements ◽  
X Ray Binaries

The first inspiral of two neutron stars observed in gravitational waves was remarkably close, allowing the kind of simultaneous gravitational wave and electromagnetic observation that had not been expected for several years. Their merger, followed by a gamma-ray burst and a kilonova, was observed across the spectral bands of electromagnetic telescopes. These GW and electromagnetic observations have led to dramatic advances in understanding short gamma-ray bursts; determining the origin of the heaviest elements; and determining the maximum mass of neutron stars. From the imprint of tides on the gravitational waveforms and from observations of X-ray binaries, one can extract the radius and deformability of inspiraling neutron stars. Together, the radius, maximum mass, and causality constrain the neutron-star equation of state, and future constraints can come from observations of post-merger oscillations. We selectively review these results, filling in some of the physics with derivations and estimates.

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