Consistent Modeling of GS 1826-24 X-Ray Bursts for Multiple Accretion Rates Demonstrates the Possibility of Constraining rp-process Reaction Rates
Consistent Modeling of GS 1826-24 X-Ray Bursts for Multiple Accretion Rates Demonstrates the Possibility of Constraining rp-process Reaction Rates
复制标题
多个吸积速率的 GS 1826-24 X 射线爆发的一致建模证明了限制 rp 过程反应速率的可能性
作者：
Z. Meisel
I型X射线暴的光变曲线编码了关于吸积中子星结构和驱动暴的rp过程的核反应速率的独特信息。使用第一个模型计算的氢/氦燃烧爆发的大范围的天体物理条件下进行的代码梅萨，这项工作表明，同时模型观测比较爆发从几个吸积率需要删除简并在天体物理条件下，否则再现爆发的一个单一的，这种一致的多历元建模可能会限制15 O（α，γ）19 Ne反应率。与1998年、2000年和2007年中子星星GS 1826-24爆发时期的比较表明，它必须比以前推断的要大，而且这个源的浅层加热必须低于0.5 MeV/u，这提供了一种新的方法来限制吸积中子星外层的浅层加热机制。光变曲线上升的特征被用来证明15 O（α，γ）反应速率可能会有一个下限，这表明了用X射线暴光变曲线限制核反应速率的可能性。
Type-I X-ray burst light curves encode unique information about the structure of accreting neutron stars and the nuclear reaction rates of the rp-process that powers bursts. Using the first model calculations of hydrogen/helium-burning bursts for a large range of astrophysical conditions performed with the code MESA, this work shows that simultaneous model–observation comparisons for bursts from several accretion rates are required to remove degeneracies in astrophysical conditions that otherwise reproduce bursts for a single and that such consistent multi-epoch modeling could possibly limit the 15O(α, γ)19Ne reaction rate. Comparisons to the 1998, 2000, and 2007 bursting epochs of the neutron star GS 1826-24 show that must be larger than previously inferred and that the shallow heating in this source must be below 0.5 MeV/u, providing a new method to constrain the shallow heating mechanism in the outer layers of accreting neutron stars. Features of the light curve rise are used to demonstrate that a lower limit could likely be placed on the 15O(α, γ) reaction rate, demonstrating the possibility of constraining nuclear reaction rates with X-ray burst light curves.