Neutrinos from Supernovas and Supernova Remnants

Costantini, Maria Laura; Vissani, Francesco

doi:10.1063/1.2125656

Cited by 3 publications

(2 citation statements)

References 12 publications

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“…The drop from the 2002 paper of Alvarez-Muniz and Halzen (shortly before the construction of IceCube started) to the paper of Costantini and Vissani from 2005 is due to that fact that in the first paper oscillations have not been taken into account [Costantini & Vissani 2005], [Distefano 2006,Kistler&Beacom 2006, [Kappes 2007] and [Morlino 2009]. Courtesy of Alexander Kappes.…”

Section: Icecubementioning

confidence: 99%

Towards high-energy neutrino astronomy

Spiering

2012

EPJ H

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The search for the sources of cosmic rays is a three-fold assault, using charged cosmic rays, gamma rays and neutrinos. The first conceptual ideas to detect high energy neutrinos date back to the late fifties. The long evolution towards detectors with a realistic discovery potential started in the seventies and eighties, with the pioneering works in the Pacific Ocean close to Hawaii and in Lake Baikal in Siberia. But only now, half a century after the first concepts, such a detector is in operation: IceCube at the South Pole. We do not yet know whether with IceCube we will indeed detect extraterrestrial high energy neutrinos or whether this will remain the privilege of next generation telescopes. But whatever the answer will be: the path to the present detectors was a remarkable journey. This review sketches its main milestones. a

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Section: Icecubementioning

confidence: 99%

Towards high-energy neutrino astronomy

Spiering

2012

EPJ H

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“…It is expected that the typical distance to a supernova event in the Milky Way is 10±5 kpc, see e.g [11]. and that the number of events scales with the inverse of the square of the distance to the supernova.…”

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confidence: 99%

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Ricciardi

Vignaroli

Vissani

2022

J. High Energ. Phys.

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We discuss as accurately as possible the cross section of quasi-elastic scattering of electron (anti-)neutrinos on nucleons, also known as inverse beta decay in the case of antineutrinos. We focus on the moderate energy range from a few MeV up to hundreds of MeV, which includes neutrinos from reactors and supernovae. We assess the uncertainty on the cross section, which is relevant to experimental advances and increasingly large statistical samples. We estimate the effects of second-class currents, showing that they are small and negligible for current applications.

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TeV neutrinos from supernova remnants embedded in giant molecular clouds

Cavasinni

Grasso

Maccione

2006

Astroparticle Physics

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The recent detection of γ-rays with energy up to 10 TeV from dense regions surrounding some Supernova Remnants (SNR) provides strong, though still not conclusive, evidence that the nucleonic component of galactic Cosmic Rays is accelerated in the supernova outflows. Neutrino telescopes could further support the validity of such scenario by detecting neutrinos coming from the same regions. We re-evaluate the TeV range neutrino-photon flux ratio to be expected from pion decay, finding small differences respect to previous derivations. We apply our results and the recent HESS measurements of the very high energy γ-ray flux from the molecular cloud complex in the Galactic Centre, to estimate the neutrino flux from that region discussing the detectability perspectives for Mediterranean Neutrino Telescopes. We also discuss under which conditions neutron decay may give rise to a significant TeV antineutrino flux from a SNR embedded in Molecular Cloud complexes.

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Neutrinos from Supernovas and Supernova Remnants

Cited by 3 publications

References 12 publications

Towards high-energy neutrino astronomy

Towards high-energy neutrino astronomy

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

TeV neutrinos from supernova remnants embedded in giant molecular clouds

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