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dc.contributor.authorThielemann, Friedrich-Karl
dc.contributor.authorSchatz, H.
dc.contributor.authorRauscher, T.
dc.contributor.authorRembges, J.F.
dc.contributor.authorGorres, J.
dc.contributor.authorWiescher, Michael
dc.contributor.authorBildsten, L.
dc.contributor.editorMezzacappa, A.
dc.date.accessioned2014-11-27T09:59:33Z
dc.date.available2014-11-27T09:59:33Z
dc.date.issued1998
dc.identifier.citationThielemann , F-K , Schatz , H , Rauscher , T , Rembges , J F , Gorres , J , Wiescher , M & Bildsten , L 1998 , Explosive H-burning, the rp-process, and X-ray bursts . in A Mezzacappa (ed.) , Stellar Evolution, Stellar Explosions and Galactic Chemical Evolution . IOP PUBLISHING LTD , Bristol , pp. 483-494 , 2nd Oak Ridge Symposium on Atomic and Nuclear Astrophysics , OAK RIDGE , Tunisia , 2/12/97 .
dc.identifier.citationconference
dc.identifier.isbn0-7503-0555-X
dc.identifier.isbn978-0750305556
dc.identifier.otherPURE: 1635720
dc.identifier.otherPURE UUID: c8d1c1fb-e4b6-497d-88e5-6c4d3cbccb37
dc.identifier.otherWOS: 000077110500057
dc.identifier.urihttp://hdl.handle.net/2299/14832
dc.description.abstractThe major astrophysical events which involve explosive H-burning are novae and type I X-ray bursts. Both are related to binary stellar systems with hydrogen accretion from a binary companion onto a compact object, and the explosive ignition of the accreted H-layer. High densities cause the pressure to be dominated by the degenerate electron gas, preventing a stable and controlled burning. In the case of novae the compact object is a white dwarf, in the case of X-ray bursts it is a neutron star. Explosive II-burning in novae has been discussed in many recent articles [1, 2, 3, 4, 5]. Its processing is limited due to maximum temperatures of similar to 3X10(8)K. Only in X-ray bursts temperatures larger than 4x10(8)K are possible, which permit a break-out from the hot CNO-cycle, leading to a further temperature increase beyond 10(9)K, the onset of an rp-process (a sequence of proton captures and beta-decays) and burning of H and He to Fe/Ni and beyond. Here we investigate the rp-process by making use of a complete and updated nuclear reaction network from H to Sn. In particular we consider 2p-capture reactions that can bridge proton unbound nuclei and therefore accelerate the reaction flow. In a simplified one dimensional, one-cone X-ray burst model we find that for a 25 s burst the reaction flow reaches Cd. The consequences for energy production, final composition of the ashes, and fuel consumption are discussed.en
dc.format.extent12
dc.language.isoeng
dc.publisherIOP PUBLISHING LTD
dc.relation.ispartofStellar Evolution, Stellar Explosions and Galactic Chemical Evolution
dc.titleExplosive H-burning, the rp-process, and X-ray burstsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted1998
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue


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