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Gamma-Ray Emission from the Shell of Supernova Remnant W44 Revealed by the Fermi LAT
KTH, Skolan för teknikvetenskap (SCI), Fysik, Partikel- och astropartikelfysik.
Vise andre og tillknytning
2010 (engelsk)Inngår i: Science, ISSN 0036-8075, E-ISSN 1095-9203, Vol. 327, nr 5969, s. 1103-1106Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

Recent observations of supernova remnants (SNRs) hint that they accelerate cosmic rays to energies close to similar to 10(15) electron volts. However, the nature of the particles that produce the emission remains ambiguous. We report observations of SNR W44 with the Fermi Large Area Telescope at energies between 2 x 10(8) electron volts and 3 x 10(11) electron volts. The detection of a source with a morphology corresponding to the SNR shell implies that the emission is produced by particles accelerated there. The gamma-ray spectrum is well modeled with emission from protons and nuclei. Its steepening above similar to 10(9) electron volts provides a probe with which to study how particle acceleration responds to environmental effects such as shock propagation in dense clouds and how accelerated particles are released into interstellar space.

sted, utgiver, år, opplag, sider
2010. Vol. 327, nr 5969, s. 1103-1106
Emneord [en]
shocked molecular gas, pulsar wind nebula, very-high-energy, particle-acceleration, streaming instability, wave dissipation, rx, j1713.7-3946, area telescope, galactic plane, cosmic-rays
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Identifikatorer
URN: urn:nbn:se:kth:diva-19250DOI: 10.1126/science.1182787ISI: 000274901100028Scopus ID: 2-s2.0-77649202347OAI: oai:DiVA.org:kth-19250DiVA, id: diva2:337297
Forskningsfinansiär
Knut and Alice Wallenberg FoundationSwedish Research Council
Merknad
QC 20100525Tilgjengelig fra: 2010-08-05 Laget: 2010-08-05 Sist oppdatert: 2017-12-12bibliografisk kontrollert

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