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dc.contributor.authorFarouqi, K.
dc.contributor.authorFreiburghaus, C.
dc.contributor.authorKratz, K. L.
dc.contributor.authorPfeiffer, B.
dc.contributor.authorRauscher, T.
dc.contributor.authorThielemann, Friedrich-Karl
dc.date.accessioned2013-04-11T14:29:41Z
dc.date.available2013-04-11T14:29:41Z
dc.date.issued2005-07-25
dc.identifier.citationFarouqi , K , Freiburghaus , C , Kratz , K L , Pfeiffer , B , Rauscher , T & Thielemann , F-K 2005 , ' Astrophysical conditions for an r-process in the high-entropy wind scenario of type II supernovae ' , Nuclear Physics A , vol. 758 , pp. 631C-634C . https://doi.org/10.1016/j.nuclphysa.2005.05.187
dc.identifier.issn0375-9474
dc.identifier.otherPURE: 1628345
dc.identifier.otherPURE UUID: 5c9d5053-bc9c-4ff0-a90b-a70e9dc77573
dc.identifier.otherWOS: 000230660500136
dc.identifier.otherScopus: 20944439420
dc.identifier.urihttp://hdl.handle.net/2299/10380
dc.description.abstractWithin a full dynamical parameter study including freezeout effects, we have determined the astrophysical conditions for an r-process in the so-called "neutrino-wind" scenario of core-collapse type II supernovae (SNII). We have started our calculations after the total photo disintegration of the matter above the nascent neutron star at 9 (.) 101 Kelvin with protons and neutrons. We have used the charged-particle network of Thielemann and the r-process code of Freiburghaus, combined with the NON-SMOKER neutron-capture rates of Rauscher, nuclear masses from the ETFS1-Q mass model and recent experimental and theoretical gross beta-decay properties. Using the three parameters V-exp (expansion speed of the shock wave), S (entropy of the bubble) and the neutron-to-proton ratio Y-e, we show that the above quantities have to fulfill specific conditions in order to make a successful r-process. According to observations and hydrodynamical simulations, respectively, a realistic value for V-exp is 7500 km/s, and Y-een
dc.format.extent4
dc.language.isoeng
dc.relation.ispartofNuclear Physics A
dc.titleAstrophysical conditions for an r-process in the high-entropy wind scenario of type II supernovaeen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2005-07-25
rioxxterms.versionofrecordhttps://doi.org/10.1016/j.nuclphysa.2005.05.187
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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