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The origin of the iron-rich knot in Tycho's supernova remnant

Yamaguchi, Hiroya; Hughes, John P.; Badenes, Carles; Bravo, Eduardo; Seitenzahl, Ivo R.; Martínez-Rodríguez, Héctor; Park, Sangwook; Petre, Robert

Description

X-ray observations of supernova remnants (SNRs) allow us to investigate the chemical inhomogeneity of ejecta, offering unique insight into the nucleosynthesis in supernova explosions. Here we present detailed imaging and spectroscopic studies of the “Fe knot” located along the eastern rim of the Type Ia SNR Tycho (SN 1572) using Suzaku and Chandra long-exposure data. Surprisingly, the Suzaku spectrum of this knot shows no emission from Cr, Mn, or Ni, which is unusual for the Fe-rich regions...[Show more]

dc.contributor.authorYamaguchi, Hiroya
dc.contributor.authorHughes, John P.
dc.contributor.authorBadenes, Carles
dc.contributor.authorBravo, Eduardo
dc.contributor.authorSeitenzahl, Ivo R.
dc.contributor.authorMartínez-Rodríguez, Héctor
dc.contributor.authorPark, Sangwook
dc.contributor.authorPetre, Robert
dc.date.accessioned2017-03-17T01:05:35Z
dc.date.available2017-03-17T01:05:35Z
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1885/113383
dc.description.abstractX-ray observations of supernova remnants (SNRs) allow us to investigate the chemical inhomogeneity of ejecta, offering unique insight into the nucleosynthesis in supernova explosions. Here we present detailed imaging and spectroscopic studies of the “Fe knot” located along the eastern rim of the Type Ia SNR Tycho (SN 1572) using Suzaku and Chandra long-exposure data. Surprisingly, the Suzaku spectrum of this knot shows no emission from Cr, Mn, or Ni, which is unusual for the Fe-rich regions in this SNR. Within the framework of the canonical delayed-detonation models for SN Ia, the observed mass ratios MCr/MFe < 0.023, MMn/MFe < 0.012, and MNi/MFe < 0.029 (at 90% confidence) can only be achieved for a peak temperature of (5.3–5.7)x10⁹ K and a neutron excess of 2.0x10⁻³. These constraints rule out the deep, dense core of a Chandrasekhar-mass white dwarf as the origin of the Fe knot and favor either incomplete Si burning or an α-rich freeze-out regime, probably close to the boundary. An explosive He burning regime is a possible alternative, although this hypothesis is in conflict with the main properties of this SNR.
dc.description.sponsorshipH.Y. is supported by the Chandra GO Program grant GO5- 16072A. C.B., H.Y., H.M.-R., and S.P. are supported by the NASA ADAP grant NNX15AM03G. E.B. was supported by MINECO-FEDER grants AYA2013-40545 and AYA2015- 63588-P.
dc.format.mimetypeapplication/pdf
dc.publisherAmerican Astronomical Society
dc.rights© 2017. The American Astronomical Society. http://www.sherpa.ac.uk/romeo/issn/0004-637X/..."Publisher's version/PDF may be used on any website or authors' institutional repository" from SHERPA/RoMEO site (as at 17/03/17).
dc.sourceThe Astrophysical Journal
dc.titleThe origin of the iron-rich knot in Tycho's supernova remnant
dc.typeJournal article
local.identifier.citationvolume834
dc.date.issued2017
local.publisher.urlhttps://aas.org/
local.type.statusPublished Version
local.contributor.affiliationSeitenzahl, I. R., Research School of Astronomy and Astrophysics, The Australian National University
local.bibliographicCitation.issue2
local.bibliographicCitation.startpage124
local.identifier.doi10.3847/1538-4357/834/2/124
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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