High-energy cosmic rays: Puzzles, models, and giga-ton neutrino telescopes

Waxman, Eli

doi:10.1007/bf02705103

Cited by 23 publications

(35 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…AGN are disfavoured as sources of UHECRs, since no AGN powerful enough to allow acceleration to greater than 10 20 eV is present out to a distance of approximately wd GZK from Earth. The suggested association between GRB and UHECR sources is based on two arguments (Waxman 1995a(Waxman , 2004b: (i) the constraints that UHECR sources must satisfy to allow proton acceleration to greater than 10 20 eV are similar to those inferred for GRB sources from gamma-ray observations and (ii) the average energy generation rate of UHECR's is similar to the gamma-ray generation rate of GRBs (associations based on different arguments were suggested in Milgrom &Usov 1995 andin Vietri 1995).…”

Section: Cosmic Accelerators and The Neutrino Backgroundmentioning

confidence: 98%

“…The identity of the UHECR sources as well as the acceleration mechanism is not yet known. The stringent constraints, which are imposed on the properties of possible UHECR sources by the high energies observed, rule out almost all source candidates, and suggest that GRBs and active galactic nuclei (AGN) are the most plausible sources (Bhattacharjee & Sigl 2000;Waxman 2004a). AGN are disfavoured as sources of UHECRs, since no AGN powerful enough to allow acceleration to greater than 10 20 eV is present out to a distance of approximately wd GZK from Earth.…”

Section: Cosmic Accelerators and The Neutrino Backgroundmentioning

confidence: 99%

“…The origin of the highest energy, greater than 10 19 eV, cosmic rays (UHECRs) is a mystery: the identity of the UHECR sources and the mechanism(s) by which particles are accelerated to such extreme energies are unknown. Identifying the sources and understanding the acceleration mechanism are among the most interesting and important challenges of high-energy astrophysics (Bhattacharjee & Sigl 2000;Waxman 2004a). Identifying the UHECR sources and probing the physical mechanisms driving them are among the main science targets of highenergy neutrino detectors (Waxman 2005).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Neutrino astronomy and gamma-ray bursts

Waxman

2007

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

The construction of large-volume detectors of high energy, greater than 1 TeV, neutrinos is mainly driven by the search for extragalactic neutrino sources. The existence of such sources is implied by the observations of ultra-high-energy, greater than or equal to 10 19 eV, cosmic rays, the origin of which is a mystery. In this lecture, I briefly discuss the expected extragalactic neutrino signal and the current state of the experimental efforts. Neutrino emission from gamma-ray bursts (GRBs), which are probably sources of both high-energy protons and neutrinos, is discussed in some detail. The detection of the predicted GRB neutrino signal, which may become possible in the coming few years, will allow one to identify the sources of ultra-high-energy cosmic rays and to resolve open questions related to the underlying physics of GRB models. Moreover, detection of GRB neutrinos will allow one to test for neutrino properties (e.g. flavour oscillations and coupling to gravity) with an accuracy many orders of magnitude better than is currently possible.

show abstract

Section: Cosmic Accelerators and The Neutrino Backgroundmentioning

confidence: 98%

Section: Cosmic Accelerators and The Neutrino Backgroundmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Neutrino astronomy and gamma-ray bursts

Waxman

2007

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

show abstract

“…In addition to this, the observed energy-release rate (per unit volume) in GRB γ rays proves to be comparable with the high-energy-proton energy, which is necessary for explaining the observable UHECR flux. The energy-release rate was estimated in [112] (see also [109]). It was assumed that the extragalactic protons in the energy range from 10 19 to 10 21 eV are produced in cosmologically distributed sources with the following density and spectrum:…”

Section: Grb and Origin Of Ultrahigh-energy Cosmic Rays (Uhecrs)mentioning

confidence: 99%

Cosmic γ-ray bursts: Observations and modeling

Бисноватый-Коган

2006

Phys. Part. Nuclei

View full text Add to dashboard Cite

It is now commonly accepted that cosmic γ -ray bursts (GRBs) are of cosmological origin. This conclusion is based on the statistical analysis of GRBs and the measurements of line redshifts in GRB optical afterglows, i.e., in the so-called long GRBs. In this review, the models of radiation and models of GRB sources are considered. In most of these models, if not in all of them, the isotropic radiation cannot provide the energy release necessary for the appearance of a cosmological GRB. No correlation is noted between the redshift, the GRB-spectrum shape, and the total detected energy. The comparison between data obtained in the Soviet experiment KONUS and the American experiment BATSE shows that they substantially differ in statistical properties and the detection of hard x-ray lines. The investigation of hard gamma (0.110 GeV) afterglows, the measurement of prompt optical spectra during the GRB detection, and the further investigation of hard x-ray lines is of obvious importance for gaining insight into the GRB origin. Observations of two bright optical GRB afterglows point to the fact that an initially bright optical flare is directly related to the GRB itself, and the subsequent weak and much more continuous optical radiation is of a different nature. The results of observations of optical GRB afterglows are discussed. They point to the fact that the GRBs originate in distant galaxies with a high matter density, where intense star formation takes place. The interaction of the cosmological GRB radiation with a dense surrounding molecular cloud results in the appearance of long-duration (up to 10 years) weak optical afterglows associated with the heating and reradiation of gas. Results of 2D numerical simulation of the heating and reradiation of gas in various variants of the relative disposition of GRB and molecular clouds are presented. In conclusion, the possible relation between

show abstract

“…The isotropic-equivalent magnetic luminosity that is required to accelerate cosmic rays with energy E is (Blandford 2000;Waxman 2004)…”

Section: Relativistic Jets and Cosmic Raysmentioning

confidence: 99%

Ultrafast Outflows From Black Hole Mergers With a Minidisk

Murase

Kashiyama

Mészáros

et al. 2016

ApJL

108

View full text Add to dashboard Cite

Recently, the direct detection of gravitational waves from black hole (BH) mergers was announced by the Advanced LIGO Collaboration. Multi-messenger counterparts of stellar-mass BH mergers are of interest, and it had been suggested that a small disk or celestial body may be involved in the binary of two BHs. To test such possibilities, we consider the fate of a wind powered by an active mini-disk in a relatively short, super-Eddington accretion episode onto a BH with ∼ 10 − 100 solar masses. We show that its thermal emission could be seen as a fast optical transient with the duration from hours to days. We also find that the coasting outflow forms external shocks due to interaction with the interstellar medium, whose synchrotron emission might be expected in the radio band on a time scale of years. Finally, we also discuss a possible jet component and the associated high-energy neutrino emission as well as ultra-high-energy cosmic-ray acceleration.

show abstract

High-energy cosmic rays: Puzzles, models, and giga-ton neutrino telescopes

Cited by 23 publications

References 35 publications

Neutrino astronomy and gamma-ray bursts

Neutrino astronomy and gamma-ray bursts

Cosmic γ-ray bursts: Observations and modeling

Ultrafast Outflows From Black Hole Mergers With a Minidisk

Contact Info

Product

Resources

About