Nucleosynthesis of proton rich nuclei on accreting neutron stars related to type I X-ray burst

Osamu Koike; Reiko Kuromizu; Masa-Aki Hashimoto; Shin Ichirou Fujimoto

doi:10.1016/S0375-9474(03)00871-6

Nucleosynthesis of proton rich nuclei on accreting neutron stars related to type I X-ray burst

Osamu Koike, Reiko Kuromizu, Masa-Aki Hashimoto, Shin Ichirou Fujimoto

Experimental Particle Physics

Research output: Contribution to journal › Article

Abstract

Using a shell flash model, we have investigated the relation between the endpoint of the rp-process and the ignition pressure. We have found a striking feature of the rp-process during the burst: nuclear fuel is almost burned out after the flash; the mass number of synthesized nuclei reaches to ∼ 100 for the typical pressure from 10²³ to 10^23.5 [dyn cm^-2]. These results will severely constrain the model of type I X-ray bursts in reproducing the observational properties such as the shape of the light curve, the total radiated energy and the recurrence time.

Original language	English
Journal	Nuclear Physics A
Volume	723
Issue number	1-2
DOIs	https://doi.org/10.1016/S0375-9474(03)00871-6
Publication status	Published - Jul 28 2003

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All Science Journal Classification (ASJC) codes

Nuclear and High Energy Physics

Cite this

Koike, O., Kuromizu, R., Hashimoto, M-A., & Fujimoto, S. I. (2003). Nucleosynthesis of proton rich nuclei on accreting neutron stars related to type I X-ray burst. Nuclear Physics A, 723(1-2). https://doi.org/10.1016/S0375-9474(03)00871-6

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AB - Using a shell flash model, we have investigated the relation between the endpoint of the rp-process and the ignition pressure. We have found a striking feature of the rp-process during the burst: nuclear fuel is almost burned out after the flash; the mass number of synthesized nuclei reaches to ∼ 100 for the typical pressure from 1023 to 1023.5 [dyn cm-2]. These results will severely constrain the model of type I X-ray bursts in reproducing the observational properties such as the shape of the light curve, the total radiated energy and the recurrence time.

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10.1016/S0375-9474(03)00871-6