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DOI：
10.1002/9781119364856.ch3
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发表时间：
2021-12
期刊：
影响因子：
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通讯作者：
D. A. Leahy;S. Morsink;Yii-Cheng Chou
中科院分区：
文献类型：
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作者：
D. A. Leahy;S. Morsink;Yii-Cheng Chou
分析了在SAX J1808.4−3658多次爆发期间检测到的脉冲形状，以限制中子星星的质量和半径。我们使用一个热点模型与一个小的散射光组件，以联合拟合数据从两个不同的时代，下的限制，星星的质量和半径和二进制的倾角不改变从时代到时代。描述光斑位置、发射率和黑体与康普顿辐射的相对分数的所有其他参数都允许随时间变化。使用1998年数据与2002年和2005年爆发的其他时期数据的联合拟合的约束i 1.0 M，对1998年“缓慢衰减”和2002年“爆发最大结束”时期的数据进行联合拟合，也落在相同的3σ置信区域内。这个3σ置信区间允许各种各样的强子状态方程，与Leahy等人的早期分析相反，他们只考虑了1998年的爆发数据，只考虑了非常小的恒星。
The pulse shapes detected during multiple outbursts of SAX J1808.4−3658 are analyzed in order to constrain the neutron star’s mass and radius. We use a hot-spot model with a small scattered-light component to jointly fit data from two different epochs, under the restriction that the star’s mass and radius and the binary’s inclination do not change from epoch to epoch. All other parameters describing the spot location, emissivity, and relative fractions of blackbody to Comptonized radiation are allowed to vary with time. The joint fit of data from the 1998 “slow decay” and the 2002 “end of outburst maximum” epochs using the constraint i 1.0 M from joint fits of the 1998 data with data from other epochs of the 2002 and 2005 outbursts also fall within the same 3σ confidence region. This 3σ confidence region allows a wide variety of hadronic equations of state, in contrast with an earlier analysis by Leahy et al. of only the 1998 outburst data that only allowed for extremely small stars.