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The electron capture rates of 55Co and 56Ni in the ultra-strong magnetic field at four typical temperature- density points have been calculated using the nuclear shell model and Landan energy levels quantized approximate correction. The results show that the electron capture rates of 55Co and 56Ni are increased greatly in the ultra-strong magnetic field, and even exceed two orders of magnitude in the range from 4.414×10^13G to 2.207×10^27 G. The change rate of electron abundance, ye, of 55Co and 56Ni under the condition of B=4.414×10^15G in the magnetar surrounding has been calculated and discussed, the proportions of ye of 55Co and 56Ni in the total Ye have been reduced by 50 percent in all more than the condition without a magnetic field. 相似文献
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Based on the p-f shell model, the effect of strong magnetic field on neutrino energy loss rates by electron capture is investigated. The calculations show that the magnetic field has only a slight effect on the neutrino energy loss rates in the range of 108—1013G on the surfaces of most neutron stars. But for some magnetars, the range of the magnetic field is 1013—1018G, and the neutrino energy loss rates are greatly reduced, even by more than four orders of magnitude due to the strong magnetic field. 相似文献
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A new improved nuclear partition function is employed to calculate
the nuclear statistical equilibrium (NSE) in core-collapse supernova
environment. The results show that the change of nucleus abundance
is slight even though the temperature is higher than 10$^{11}$\,K
when shock propagates, which indicates that the effect of the
nuclear partition function is not so important as shown in the
previous calculations, but it can also be considered in detailed
simulation if it is sensitive to weak interaction rates in
core-collapse supernova. 相似文献
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By using the new Coulomb screening model and most recent experimental results, this paper calculates the resonance reaction rates of ^21Na(p,γ)^22Mg. The derived result shows that the effect of electron screening on resonant reaction is prominent in astrophysical interesting temperature range. In conjunction with the experimental results, the recommended rates of^21Na(p,γ)^22 Mg would increase at least 10%, which undoubtedly affect the nucleosynthesis of some heavier nuclei in a variety of astrophysical sites.[第一段] 相似文献
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The current quark mass model is adopted to study the phase transition of two-flavor quark matter to more stable three-flavor quark matter in the whole core of a supernova. It shows that the timescale of the process is shorter than 10-8 seconds, that the u- and d-quark masses can be neglected completely in this model, and that the temperature and the total neutrino energies in the core after the conversion increase nearly by 40% and 20% on the average compared with former results, respectively. The last result can further enhance the probability of success for a supernova explosion significantly. 相似文献
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Based on the Weinberg-Salam theory, the pair neutrino energy loss rates for nuclei 56Fe are canvassed for the wide range of density and temperature. The results of ours (QLJ) are compared with those of Beaudet G, Petrosian V and Salpeter E. E's (QBPS), and it shows that the pair neutrino energy loss rates of QBPS are always larger than QLJ .The QBPS is 12.57%, 12.86%, 14.99%, 19.80% times higher than QLJ corresponding to the temperature T9=0.385, 1.0, 5.0, 10, respectively. 相似文献
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Improving Salpeter's method, we discuss the effect of superstrong magnetic fields (such as those of magnetars) on thermonuclear reaction rates. These most interesting reactions, including the hydrogen burning by the CNO cycle and the helium burning by the triple alpha reaction, are investigated as examples on the magnetar surfaces. The obtained result shows that the superstrong magnetic fields can increase the thermonuclear reaction rates by many orders of magnitude. The enhancement may have significant influence for further study research of the magnetars, especially for the x-ray luminosity observation and the evolution of magnetars. 相似文献