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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.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.otherPURE: 1635720
dc.identifier.otherPURE UUID: c8d1c1fb-e4b6-497d-88e5-6c4d3cbccb37
dc.identifier.otherWOS: 000077110500057
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.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

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