变化吸积率下中子星的壳冷却研究（英文）

刘荷蕾; 吕国梁; 陆向阳; 李琳; 王兆军

doi:10.13568/j.cnki.651094.651316.2022.05.12.0004

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变化吸积率下中子星的壳冷却研究（英文）

更新时间：2026-01-21

- 变化吸积率下中子星的壳冷却研究（英文）
- Journal of Xinjiang University (Natural Science Edition in Chinese and English) Vol. 40, Issue 1, Pages: 10-16(2023)
- 作者机构：
  
  新疆大学物理科学与技术学院
- 作者简介：
- 基金信息：
- DOI：10.13568/j.cnki.651094.651316.2022.05.12.0004
  CLC： P145.6
- Published：2023
- 稿件说明：
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[1]刘荷蕾,吕国梁,陆向阳,等.变化吸积率下中子星的壳冷却研究（英文）[J].新疆大学学报(自然科学版)(中英文),2023,40(01):10-16.
[1]刘荷蕾,吕国梁,陆向阳,等.变化吸积率下中子星的壳冷却研究（英文）[J].新疆大学学报(自然科学版)(中英文),2023,40(01):10-16. DOI： 10.13568/j.cnki.651094.651316.2022.05.12.0004.

DOI：10.13568/j.cnki.651094.651316.2022.05.12.0004.

摘要

暂现源中子星（NS）低质量X射线双星为研究NS壳加热和冷却提供了一个宝贵的机会．模拟其宁静期的光变曲线需要在中子星的浅壳层加一个额外的未知热源．通过开源的d Star程序，探究时间依赖吸积率对中子星壳冷却以及浅壳层加热参数的影响．研究表明：爆发初期变化吸积率对壳冷却影响较小，爆发期最后阶段吸积率的变化对壳冷却有较大的影响．变化吸积率导致爆发结束后中子星表面的温度比常数吸积率下中子星表面温度低，因此变化吸积率下需要提供更多的浅壳层加热来拟合爆发结束后的壳冷却观测．研究了MXB 1659-29和MAXI J0556-332这两颗源，它们对应不同的吸积时间以及浅壳层加热，时间变化吸积率对这两颗源的壳冷却以及浅壳层加热参数的影响是一致的．

Abstract

The transient neutron star(NS) low-mass X-ray binary provides a rare opportunity to study NS crust heating and cooling. Models of the quiescent light curve require additional heat in the shallow outer crust from an unknown source. Here we examine the crust cooling of NS with varying accretion rate to understand the effect of time-dependent accretion rate on crust cooling and shallow heating parameters with use of the open source code d Star. Our modeling indicates that variations of accretion rate during the early stage of outburst have a small effect on the theoretical crust cooling light curve

while variations in the final stage(days to months) of the outburst strongly affect the theoretical crust cooling light curve. The surface temperature of NS at the end of outburst with a time-dependent accretion rate is lower than that with constant accretion rate. As a result

more shallow heating is needed to fit the observational quiescent crust cooling light curve with time-dependent accretion rate. Our research focuses on MXB 1659-29 and MAXI J0556-332 which have different accretion time and shallow heating. We find that the results are consistent from these two sources.

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references

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