Matter radii of [superscript 32–35]Mg

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dc.creator Kanungo, Rituparna
dc.creator Prochazka, A.
dc.creator Horiuchi, W.
dc.creator Nociforo, C.
dc.creator Aumann, T.
dc.creator Boutin, D.
dc.creator Cortina-Gil, D.
dc.creator Davids, B.
dc.creator Diakaki, M.
dc.creator Farinon, F.
dc.creator Perro, C.
dc.date.accessioned 2017-01-13T13:40:08Z
dc.date.available 2017-01-13T13:40:08Z
dc.date.issued 2011-02-09
dc.identifier.issn 0556-2813
dc.identifier.uri http://library2.smu.ca/handle/01/26730
dc.description Publisher's version/PDF en_CA
dc.description.abstract The interaction cross sections of [superscript 32–35]Mg at 900A MeV have been measured using the fragment separator at GSI. The deviation from the r[subscript 0]A[superscript 1/3] trend is slightly larger for [superscript 35]Mg, signaling the possible formation of a longer tail in the neutron distribution for [superscript 35]Mg. The radii extracted from a Glauber model analysis with Fermi densities are consistent with models predicting the development of neutron skins. en_CA
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dc.description.provenance Made available in DSpace on 2017-01-13T13:40:08Z (GMT). No. of bitstreams: 1 Kanungo_Rituparna_article_2011_a.pdf: 465077 bytes, checksum: a3110ecf99aef30efdeab9a6980a7c23 (MD5) Previous issue date: 2011-02-09 en
dc.language.iso en en_CA
dc.publisher American Physical Society en_CA
dc.relation.uri https://doi.org/10.1103/PhysRevC.83.021302
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Neutrons
dc.subject.lcsh Matter
dc.subject.lcsh Cross sections (Nuclear physics)
dc.subject.lcsh Magnesium -- Isotopes
dc.title Matter radii of [superscript 32–35]Mg en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Physical Review C 83, 021302(R). (2011) en_CA
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Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: https://doi.org/10.1103/PhysRevC.83.021302
 
 

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