TeV photons and Neutrinos from giant soft-gamma repeaters flares
On leave of absence from Universitá di Bari and INFN During the last 35 years three giant flares were observed from so-called Soft Gamma Repeaters (SGR’s). They are assumed to be associated with star-quakes of pulsars accelerating electrons and, possibly, protons to high energy in the huge magnetic...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.257.7319 2023-05-15T14:00:02+02:00 TeV photons and Neutrinos from giant soft-gamma repeaters flares Francis Halzen A Hagar L Sman A Teresa Montaruli A The Pennsylvania State University CiteSeerX Archives 2005 application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.7319 http://arxiv.org/pdf/astro-ph/0503348v1.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.7319 http://arxiv.org/pdf/astro-ph/0503348v1.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://arxiv.org/pdf/astro-ph/0503348v1.pdf text 2005 ftciteseerx 2016-01-07T20:01:16Z On leave of absence from Universitá di Bari and INFN During the last 35 years three giant flares were observed from so-called Soft Gamma Repeaters (SGR’s). They are assumed to be associated with star-quakes of pulsars accelerating electrons and, possibly, protons to high energy in the huge magnetic fields as inferred from the observations. Because of this and the observation of non-thermal emission it has been speculated that they may be cosmic ray accelerators producing gamma-rays up to TeV energies. Neutrino telescopes, such as AMANDA and the ANTARES now under construction, could be used as TeV-γ detectors for very short emissions by measuring underground muons produced in γ showers. We estimate signal and background rates for TeV photons from SGR giant flares in AMANDA, and we provide an estimate of the gamma shower events that Milagro could detect. Moreover, we consider that, if hadrons are accelerated in these sources, high energy neutrinos would be produced together with photons. These may be detected in neutrino telescopes using neutrino-induced cascades and upgoing muons. We argue that the Antarctic Muon and Neutrino Detector Array AMANDA may have observed the December 27, 2004 giant flare from the soft gamma-ray repeater SGR 1806-20 if the non-thermal component of the spectrum extends to TeV energies (at present the actual data is subject to blind analysis). Rates should be scaled by about two orders of magnitude in km 3 detectors, such as IceCube, making SGR flares sources of primary interest. ∗ Corresponding author. Text Antarc* Antarctic Unknown Antarctic The Antarctic |
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On leave of absence from Universitá di Bari and INFN During the last 35 years three giant flares were observed from so-called Soft Gamma Repeaters (SGR’s). They are assumed to be associated with star-quakes of pulsars accelerating electrons and, possibly, protons to high energy in the huge magnetic fields as inferred from the observations. Because of this and the observation of non-thermal emission it has been speculated that they may be cosmic ray accelerators producing gamma-rays up to TeV energies. Neutrino telescopes, such as AMANDA and the ANTARES now under construction, could be used as TeV-γ detectors for very short emissions by measuring underground muons produced in γ showers. We estimate signal and background rates for TeV photons from SGR giant flares in AMANDA, and we provide an estimate of the gamma shower events that Milagro could detect. Moreover, we consider that, if hadrons are accelerated in these sources, high energy neutrinos would be produced together with photons. These may be detected in neutrino telescopes using neutrino-induced cascades and upgoing muons. We argue that the Antarctic Muon and Neutrino Detector Array AMANDA may have observed the December 27, 2004 giant flare from the soft gamma-ray repeater SGR 1806-20 if the non-thermal component of the spectrum extends to TeV energies (at present the actual data is subject to blind analysis). Rates should be scaled by about two orders of magnitude in km 3 detectors, such as IceCube, making SGR flares sources of primary interest. ∗ Corresponding author. |
author2 |
The Pennsylvania State University CiteSeerX Archives |
format |
Text |
author |
Francis Halzen A Hagar L Sman A Teresa Montaruli A |
spellingShingle |
Francis Halzen A Hagar L Sman A Teresa Montaruli A TeV photons and Neutrinos from giant soft-gamma repeaters flares |
author_facet |
Francis Halzen A Hagar L Sman A Teresa Montaruli A |
author_sort |
Francis Halzen A |
title |
TeV photons and Neutrinos from giant soft-gamma repeaters flares |
title_short |
TeV photons and Neutrinos from giant soft-gamma repeaters flares |
title_full |
TeV photons and Neutrinos from giant soft-gamma repeaters flares |
title_fullStr |
TeV photons and Neutrinos from giant soft-gamma repeaters flares |
title_full_unstemmed |
TeV photons and Neutrinos from giant soft-gamma repeaters flares |
title_sort |
tev photons and neutrinos from giant soft-gamma repeaters flares |
publishDate |
2005 |
url |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.7319 http://arxiv.org/pdf/astro-ph/0503348v1.pdf |
geographic |
Antarctic The Antarctic |
geographic_facet |
Antarctic The Antarctic |
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Antarc* Antarctic |
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Antarc* Antarctic |
op_source |
http://arxiv.org/pdf/astro-ph/0503348v1.pdf |
op_relation |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.7319 http://arxiv.org/pdf/astro-ph/0503348v1.pdf |
op_rights |
Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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1766269009653661696 |