Speaker
Description
Since the first detected extrasolar X-ray source of Scorpius X-1 (aka Sco X-1) by Giacconi et al. in 1962, more than 7083 Type-I X-ray bursts generated by the respective 115 bursters have been observed. Reproducing the burst light curve is the key to accurately understanding thin-shell burning in Type-I X-ray bursts, nova outbursts, and Type-Ia supernovae, and to identifying important seed nuclei for superburst and neutron-star crust cooling. Up to now, there has been no theoretical model capable of producing X-ray bursts closely conformed with an observed X-ray burst profile. Here we present the first benchmark Type-I X-ray burst model that unprecedentedly reconciles the simulated periodic burst light curve properties with the observed ones. The observed periodic bursts were generated from the GS 1826−24 burster discovered by Makino et al. in 1988. It is for the first time since its discovery that a theoretical model remarkably reproduces the observed burst fluence, recurrence time, light curve profile, conforming with the observed burst peak until tail end and revealing the morphology of periodic X-ray burst.
Please select a main topic related to your abstract | Theoretical Nuclear Physics for Astrophysics |
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