scholarly journals The r-process in the neutrino-induced relativistic jet of a gamma-ray burst

2013 ◽  
Author(s):  
Ko Nakamura
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Relativistic Jet ◽  
R Process

scholarly journals Prospects for obtaining an r process from Gamma Ray Burst Disk Winds

2005 ◽  
Vol 758 ◽  
pp. 189-196 ◽  
Author(s):  
G.C. McLaughlin ◽  
R. Surman
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
R Process

scholarly journals Origin of Ultra-High Energy Cosmic Rays: Nuclear Composition of Gamma-Ray Burst Jets

2011 ◽  
Vol 7 (S279) ◽  
pp. 389-390
Author(s):  
Sanshiro Shibata ◽  
Nozomu Tominaga
Keyword(s):  
Cosmic Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
Heavy Nuclei ◽  
Gamma Ray Burst ◽  
High Energy Cosmic Rays ◽  
Relativistic Jet ◽  
Launch Site ◽  
Nuclear Composition

AbstractUltra-high energy cosmic rays (UHECRs) are the most energetic particles flying from space and their source is not clarified yet. Recently, the Pierre Auger Observatory (PAO) suggests that UHECRs involve heavy nuclei. The PAO results require that a considerable fraction of metal nuclei must exist in the accelerating site, which can be realized only in the stellar interior. This puts strong constraints on the origin of UHECRs. In order to definitize the constraints from PAO results, we investigate the fraction of metal nuclei in a relativistic jet in gamma-ray burst associated with core-collapse supernova. If the jet is initially dominated by radiation field, quasi-statistical equilibrium (QSE) is established and heavy nuclei are dissociated to light particles such as 4He during the acceleration and expansion. On the other hand, if the jet is mainly accelerated by magnetic field heavy or intermediate mass nuclei can survive. The criterion to contain the metal nuclei is that the temperature at the launch site is below 4.5 × 109K. Therefore, if the composition of UHECRs is dominated by metal nuclei, a GRB with the magnetized jet is the most plausible candidate of the accelerating site.

Long gamma-ray burst as a production site of r-process elements

2012 ◽  
Author(s):  
Ko Nakamrua ◽  
Seiji Harikae ◽  
Toshitaka Kajino ◽  
Grant J. Mathews
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Production Site ◽  
R Process ◽  
Process Elements

scholarly journals A luminosity distribution for kilonovae based on short gamma-ray burst afterglows

2019 ◽  
Vol 486 (1) ◽  
pp. 672-690 ◽  
Author(s):  
Stefano Ascenzi ◽  
Michael W Coughlin ◽  
Tim Dietrich ◽  
Ryan J Foley ◽  
Enrico Ramirez-Ruiz ◽  
...  
Keyword(s):  
Near Infrared ◽  
Gamma Ray ◽  
Radioactive Decay ◽  
Infrared Emission ◽  
Gamma Ray Burst ◽  
Peak Magnitude ◽  
Upper Limits ◽  
R Process ◽  
Process Elements ◽  
First Time

Abstract The combined detection of a gravitational-wave signal, kilonova, and short gamma-ray burst (sGRB) from GW170817 marked a scientific breakthrough in the field of multimessenger astronomy. But even before GW170817, there have been a number of sGRBs with possible associated kilonova detections. In this work, we re-examine these ‘historical’ sGRB afterglows with a combination of state-of-the-art afterglow and kilonova models. This allows us to include optical/near-infrared synchrotron emission produced by the sGRB as well as ultraviolet/optical/near-infrared emission powered by the radioactive decay of r-process elements (i.e. the kilonova). Fitting the light curves, we derive the velocity and the mass distribution as well as the composition of the ejected material. The posteriors on kilonova parameters obtained from the fit were turned into distributions for the peak magnitude of the kilonova emission in different bands and the time at which this peak occurs. From the sGRB with an associated kilonova, we found that the peak magnitude in H bands falls in the range [−16.2, −13.1] ($95{{\ \rm per\ cent}}$ of confidence) and occurs within $0.8\!-\!3.6\, \rm d$ after the sGRB prompt emission. In g band instead we obtain a peak magnitude in range [−16.8, −12.3] occurring within the first 18 h after the sGRB prompt. From the luminosity distributions of GW170817/AT2017gfo, kilonova candidates GRB130603B, GRB050709, and GRB060614 (with the possible inclusion of GRB150101B, GRB050724A, GRB061201, GRB080905A, GRB150424A, and GRB160821B) and the upper limits from all the other sGRBs not associated with any kilonova detection we obtain for the first time a kilonova luminosity distribution in different bands.

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