This study is devoted to dilaton generation during the propagation of magnetic dipole waves from a pulsar in the galactic magnetic field. Dilaton generation occurs at cosmological scales on the order of the coherence lengths of the galactic magnetic field L _coh, approximately 100 pc. The exact solutions of the dilaton field equation in a vacuum and in the interstellar medium with reflective index n = 1 + χ, χ ≪ 1 have been obtained, and the angular distribution of emitted dilaton energy has been determined in both cases. It has been shown that the dilaton generation intensity at first increases proportionally to r ², where r is distance from the neutron star to the observation point, then has oscillating behavior. The obtained results are applicable only for r < L _coh. For a millisecond pulsar with a magnetic field B_S ∼ 10⁹ Gauss, located at a distance from Earth on the order of the coherence length of the galactic magnetic field L _coh ∼ 100 pc, the obtained intensity of the dilaton generation can be greater in 100 times than the analogous intensity produced by rotating magnetic dipole momentum of a pulsar. Based on estimated values, the impact of pulsar and magnetar gravitational fields on magnetic dipole wave radiation is minimal and changes the amplitude of the waves by around 1 percent. For this reason, the effect of the gravitational field on the dilaton formation process can be disregarded in this study.

中文翻译：

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脉冲星磁偶极子波在银河磁场中传播的膨胀子产生


本研究致力于在银河系磁场中脉冲星的磁偶极子波传播过程中的膨胀子产生。膨胀子的产生发生在宇宙学尺度上，大约是银河系磁场 L_coh 的相干长度，大约 100 pc。已经获得了真空和反射指数 n = 1 + χ、χ ≪ 1 的真空和星际介质中膨胀子场方程的精确解，并且在这两种情况下都确定了发射的膨胀子能量的角度分布。已经表明，膨胀子生成强度首先与 r² 成比例增加，其中 r 是从中子星到观测点的距离，然后具有振荡行为。获得的结果仅适用于 r < L_coh。对于磁场 B_S ∼ 10⁹ Gauss 的毫秒脉冲星，位于距地球一定距离的星系磁场 L_coh ∼ 100 pc 的相干长度量级上，获得的膨胀子生成强度可以比脉冲星旋转磁偶极子动量产生的类似强度大 100 倍。根据估计值，脉冲星和磁力引力场对磁偶极子波辐射的影响很小，波的振幅变化了大约 1%。出于这个原因，在本研究中可以忽略引力场对膨胀子形成过程的影响。