Show simple item record

dc.contributor.authorSlane, P.
dc.contributor.authorLee, S.-H.
dc.contributor.authorEllison, Donald C.
dc.contributor.authorPatnaude, D. J.
dc.contributor.authorHughes, John P.
dc.contributor.authorEriksen, K. A.
dc.contributor.authorNagataki, S.
dc.contributor.authorCastro, Daniel
dc.date.accessioned2015-01-22T17:26:21Z
dc.date.available2015-01-22T17:26:21Z
dc.date.issued2014-02
dc.date.submitted2013-10
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/93132
dc.description.abstractTycho's supernova remnant (SNR) is well-established as a source of particle acceleration to very high energies. Constraints from numerous studies indicate that the observed γ-ray emission results primarily from hadronic processes, providing direct evidence of highly relativistic ions that have been accelerated by the SNR. Here we present an investigation of the dynamical and spectral evolution of Tycho's SNR by carrying out hydrodynamical simulations that include diffusive shock acceleration of particles in the amplified magnetic field at the forward shock of the SNR. Our simulations provide a consistent view of the shock positions, the nonthermal emission, the thermal X-ray emission from the forward shock, and the brightness profiles of the radio and X-ray emission. We compare these with the observed properties of Tycho to determine the density of the ambient material, the particle acceleration efficiency and maximum energy, the accelerated electron-to-proton ratio, and the properties of the shocked gas downstream of the expanding SNR shell. We find that evolution of a typical Type Ia supernova in a low ambient density (n [subscript 0] ~ 0.3 cm[superscript –3]), with an upstream magnetic field of ~5 μG, and with ~16% of the SNR kinetic energy being converted into relativistic electrons and ions through diffusive shock acceleration, reproduces the observed properties of Tycho. Under such a scenario, the bulk of observed γ-ray emission at high energies is produced by π[superscript 0]-decay resulting from the collisions of energetic hadrons, while inverse-Compton emission is significant at lower energies, comprising roughly half of the flux between 1 and 10 GeV.en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637X/783/1/33en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleA CR-HYDRO-NEI MODEL OF THE STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SUPERNOVA REMNANTen_US
dc.typeArticleen_US
dc.identifier.citationSlane, P., S.-H. Lee, D. C. Ellison, D. J. Patnaude, J. P. Hughes, K. A. Eriksen, D. Castro, and S. Nagataki. “A CR-HYDRO-NEI MODEL OF THE STRUCTURE AND BROADBAND EMISSION FROM TYCHO’S SUPERNOVA REMNANT.” The Astrophysical Journal 783, no. 1 (February 10, 2014): 33. © 2014 The American Astronomical Societyen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorCastro, Danielen_US
dc.relation.journalThe Astrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsSlane, P.; Lee, S.-H.; Ellison, D. C.; Patnaude, D. J.; Hughes, J. P.; Eriksen, K. A.; Castro, D.; Nagataki, S.en_US
dc.identifier.orcidhttps://orcid.org/0000-0002-3243-727X
mit.licensePUBLISHER_POLICYen_US


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record