2,852 research outputs found
Status of neutrino astronomy
Astrophysical neutrinos can be produced in proton interactions of charged
cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in
balloon, satellite and air shower experiments every day, from below 1e9 eV up
to macroscopic energies of 1e21 eV. The observation of different photon fields
has been done ever since, today with detections ranging from radio wavelengths
up to very high-energy photons in the TeV range. The leading question for
neutrino astronomers is now which sources provide a combination of efficient
proton acceleration with sufficiently high photon fields or baryonic targets at
the same time in order to produce a neutrino flux that is high enough to exceed
the background of atmospheric neutrinos. There are only two confirmed
astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit
and emitted neutrinos at MeV energies. The aim of large underground Cherenkov
telescopes like IceCube and KM3NeT is the detection of neutrinos at energies
above 100 GeV. In this paper, recent developments of neutrino flux modeling for
the most promising extragalactic sources, gamma ray bursts and active galactic
nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4
figures, 1 tabl
Status of neutrino astronomy
Astrophysical neutrinos can be produced in proton interactions of charged
cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in
balloon, satellite and air shower experiments every day, from below 1e9 eV up
to macroscopic energies of 1e21 eV. The observation of different photon fields
has been done ever since, today with detections ranging from radio wavelengths
up to very high-energy photons in the TeV range. The leading question for
neutrino astronomers is now which sources provide a combination of efficient
proton acceleration with sufficiently high photon fields or baryonic targets at
the same time in order to produce a neutrino flux that is high enough to exceed
the background of atmospheric neutrinos. There are only two confirmed
astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit
and emitted neutrinos at MeV energies. The aim of large underground Cherenkov
telescopes like IceCube and KM3NeT is the detection of neutrinos at energies
above 100 GeV. In this paper, recent developments of neutrino flux modeling for
the most promising extragalactic sources, gamma ray bursts and active galactic
nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4
figures, 1 tabl
Status of neutrino astronomy
Astrophysical neutrinos can be produced in proton interactions of charged
cosmic rays with ambient photon or baryonic fields. Cosmic rays are observed in
balloon, satellite and air shower experiments every day, from below 1e9 eV up
to macroscopic energies of 1e21 eV. The observation of different photon fields
has been done ever since, today with detections ranging from radio wavelengths
up to very high-energy photons in the TeV range. The leading question for
neutrino astronomers is now which sources provide a combination of efficient
proton acceleration with sufficiently high photon fields or baryonic targets at
the same time in order to produce a neutrino flux that is high enough to exceed
the background of atmospheric neutrinos. There are only two confirmed
astrophysical neutrino sources up to today: the sun and SuperNova 1987A emit
and emitted neutrinos at MeV energies. The aim of large underground Cherenkov
telescopes like IceCube and KM3NeT is the detection of neutrinos at energies
above 100 GeV. In this paper, recent developments of neutrino flux modeling for
the most promising extragalactic sources, gamma ray bursts and active galactic
nuclei, are presented.Comment: Talk given at Neutrino 2008, Christchurch (New Zealand) 6 pages, 4
figures, 1 tabl
Introduction to neutrino astronomy
This writeup is an introduction to neutrino astronomy, addressed to
astronomers and written by astroparticle physicists. While the focus is on
achievements and goals in neutrino astronomy, rather than on the aspects
connected to particle physics, we will introduce the particle physics concepts
needed to appreciate those aspects that depend on the peculiarity of the
neutrinos. The detailed layout is as follows: In Sect.~1, we introduce the
neutrinos, examine their interactions, and present neutrino detectors and
telescopes. In Sect.~2, we discuss solar neutrinos, that have been detected and
are matter of intense (theoretical and experimental) studies. In Sect.~3, we
focus on supernova neutrinos, that inform us on a very dramatic astrophysical
event and can tell us a lot on the phenomenon of gravitational collapse. In
Sect.~4, we discuss the highest energy neutrinos, a very recent and lively
research field. In Sect.~5, we review the phenomenon of neutrino oscillations
and assess its relevance for neutrino astronomy. Finally, we offer a brief
overall assessment and a summary in Sect.~6. The material is selected - i.e.,
not all achievements are reviewed - and furthermore it is kept to an
introductory level, but efforts are made to highlight current research issues.
In order to help the beginner, we prefer to limit the list of references,
opting whenever possible for review works and books.Comment: 15 pages, 5 figures. Accepted for publication The European Physical
Journal Plus. Based on the lecture given at the "4th Azarquiel School of
Astronomy", June 2017, Porto Paolo di Capo Passero, Syracuse (Italy)
https://agenda.infn.it/conferenceDisplay.py?confId=1208
Supernova Neutrino Neutrino Astronomy
Modern neutrino facilities will be able to detect a large number of neutrinos
from the next Galactic supernova. We investigate the viability of the
triangulation method to locate a core-collapse supernova by employing the
neutrino arrival time differences at various detectors. We perform detailed
numerical fits in order to determine the uncertainties of these time
differences for the cases when the core collapses into a neutron star or a
black hole. We provide a global picture by combining all the relevant current
and future neutrino detectors. Our findings indicate that in the scenario of a
neutron star formation, supernova can be located with precision of 1.5 and 3.5
degrees in declination and right ascension, respectively. For the black hole
scenario, sub-degree precision can be reached.Comment: 18 pages, 8 figures, matches published versio
High-Energy Neutrino Astronomy
Kilometer-scale neutrino detectors such as IceCube are discovery instruments
covering nuclear and particle physics, cosmology and astronomy. Examples of
their multidisciplinary missions include the search for the particle nature of
dark matter and for additional small dimensions of space. In the end, their
conceptual design is very much anchored to the observational fact that Nature
accelerates protons and photons to energies in excess of and
eV, respectively. The cosmic ray connection sets the scale of cosmic
neutrino fluxes. In this context, we discuss the first results of the completed
AMANDA detector and the reach of its extension, IceCube. Similar experiments
are under construction in the Mediterranean. Neutrino astronomy is also
expanding in new directions with efforts to detect air showers, acoustic and
radio signals initiated by super-EeV neutrinos.Comment: 9 pages, Latex2e, uses ws-procs975x65standard.sty (included), 4
postscript figures. To appear in Proceedings of Thinking, Observing, and
Mining the Universe, Sorrento, Italy, September 200
The ANTARES Collaboration: Contributions to ICRC 2017 Part I: Neutrino astronomy (diffuse fluxes and point sources)
Papers on neutrino astronomy (diffuse fluxes and point sources, prepared for
the 35th International Cosmic Ray Conference (ICRC 2017, Busan, South Korea) by
the ANTARES Collaboratio
- …