Pulsars are stars whose electromagnetic radiation is observed to pulsate in well‐defined time intervals while they rotate as long as the electromagnetic signal is not emitted in the direction of the rotation axis. The frequencies of the pulses decay with time as quantified by the braking index (n). In the canonical model, n = 3 for all pulsars, but observational data yield n < 3. In this work, this model is modified to allow time change in the moment of inertia. According to that model, as the neutron star loses energy by the emission of electromagnetic radiation, its rotation decelerates under constant moment of inertia. Here, we propose that, as the rotation decelerates, the shape of the star changes due to an increasingly weaker centrifugal force that reduces its moment of inertia, a change that, under normal circumstances, would accelerate the star's rotation. In the case of pulsars, as the rotation decreases in view of electromagnetic energy loss, the rotation would decelerate less than in the canonical model, yielding a braking index less than three. This is a good result from our model, especially regarding stars with indices close to three. For lower indices, our model requires refinements as a complete explanation of braking index values probably demands that a series of phenomena be incorporated into the process.

中文翻译：

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旋转减速对脉冲星形状的影响可能反映在恒星的制动指数上

脉冲星是恒星，只要不向旋转轴方向发射电磁信号，就可以观察到电磁辐射在确定的时间间隔内脉动。脉冲的频率随时间衰减，如制动指数（n）所量化。在典范模型中，所有脉冲星的n  = 3，但观测数据得出n  <3。在这项工作中，修改了该模型以允许惯性矩中的时间发生变化。根据该模型，由于中子星由于电磁辐射的发射而失去能量，因此它的旋转在恒定的惯性矩下减速。在此，我们建议，随着旋转的减速，恒星的形状会由于逐渐减弱的离心力而减小，从而减小了其惯性矩，这种变化在正常情况下会加速恒星的旋转。在脉冲星的情况下，由于电磁能量损失而导致旋转减少，因此旋转将比标准模型中的减速少，从而产生小于3的制动指数。这是从我们的模型得出的良好结果，尤其是对于折射率接近三的恒星。对于较低的索引，