Pulsars emit pulsed radiation at well‐defined frequencies. In the canonical model, a pulsar is assumed to be a rotating, highly magnetized sphere made mostly of neutrons that has a magnetic dipole misaligned with respect to its rotation axis, which would be responsible for the emission of the observed pulses. The measurement of the pulse frequency and its first two derivatives allows the calculation of the braking index, n. One limitation of the canonical model is that, for all pulsars, it yields n = 3, a result that does not correspond to observational values of n. In order to contribute to the solution of this problem, we proposed a model for pulsars' rotation frequency decay assuming that the star's total moment of inertia would vary with time due to mass motions inside the core. As a result, we found that the pulsar J1734‐3333 has total angular momentum practically conserved, a phenomenon that we explain by relating the motion of neutron superfluid vortices in the core to torques associated with radiation emission.

中文翻译：

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J1734-3333脉冲星的角动量守恒和核心超流体动力学

脉冲星以规定的频率发射脉冲辐射。在经典模型中，假设脉冲星是旋转的，高度磁化的球体，该球体主要由中子组成，其磁偶极子相对于其旋转轴未对准，这将导致观测到的脉冲的发射。通过测量脉冲频率及其前两个导数，可以计算出制动指数n。典范模型的一个局限性是，对于所有脉冲星，它都会产生n = 3，该结果与n的观测值不对应。为了有助于解决该问题，我们提出了一个脉冲星自转频率衰减的模型，假设恒星的总惯性矩会由于核心内​​部的质量运动而随时间变化。因此，