关于脉冲星非共转模型的研究

THE RESEARCH FOR THE NONCOROTATING MODEL OF A PULSAR

本文讨论了共轴、纯转动、force-free的脉冲星系统,在Burman理论基础上建立了一个非共转模型(其中含待定参量,共转情况是它的特例)。利用系统稳定的近似条件——系统能量最小确定特定参量,得到一个与G-J模型类似的共转模型。由于考虑了惯性效应,不存在星风,是稳定态,但没有辐射。在转轴与磁矩有小偏角时,利用非平衡系统更普遍的稳定条件——熵产生最小,确定本模型的参量,得到的辐射能量在量级上与观测值相符合。

The main point of this paper is to discuss an axisymetrical pure rotating, force-free and stable self-consistent pulsar model. There are some problems in the Golderich and Julian model (1969) due to its simple hypotheses. In order to improve it we suggest that the pulsar does not need to be corotating. We also considered the inertia effects in building a noncoro-tating pulsar model with some parameters, which can be determined according to the system's stable condition. We have obtained some interesting results: If there is no magnetic radiation, under the stable condition, the model is a corotating one. Its space charges are distributed within a definite distance from the rotating axis. The Pilipp theory is no longer correct here and it has no wind zone problem. In the case of a small angle between the rotating axis and the magnetic moment, magnetic radiation is allowed. In fact, pulsar is a nonequilibrium system with a minimum entropy production as its stable condition. From this we can obtain an exact non-corotating model with radiations which have two parts: magnetic radiation and bremsstrahlung radiation. The bremsstrahlung radiation is due to collision between electrons and protons in the pulsar crust. In the case of an arbitrary angle between the rotating axis and the magnetic moment, this result is also correct, except for different rotating velocity function.