Effects of strong magnetic fields on the population of hyperon stars
R. O. Gomes, V. Dexheimer, C. A. Z. Vasconcellos
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Prepared for conference STARS2013 - 2nd Caibbean Symposium on Cosmology, Gravitaion, Nuclear and Astroparticle Physics / SMFNS2013 - 3rd International Symposium on Strong Electromagnetic Fields and Neutron Stars
In this contribution we study the effects of strong magnetic fields on the particle population of neutron stars with hyperon degrees of freedom in their composition. The star matter is described by a multi-component model with parameterized baryon-meson interaction couplings. We study the magnetic effects on the equation of state (EoS) due to the Landau quantization, assuming a density dependent static magnetic field that reaches about $10^{19}\,G$ in the center of the star. The Tolman-Oppenheimer-Volkoff equations are solved in order to understand the dependence of the mass-radius relation and hyperon population on the magnetic field intensity assuming different interaction coupling schemes.
Relativistic Mean-Field Treatment of Pulsar Kick from Neutrino Propagation in Magnetized Proto-Neutron
本文用微扰法计算了在强磁场作用下，热而致密的超声波中子星物质中中微子的散射和吸收。我们在完全相对论平均场论中计算了吸收截面。我们发现中微子的吸收强度存在显著的角度依赖性，即在平行于磁场的方向上减弱，而在相反的方向上增强。对于2 x 10^{17} G的内部磁场，中微子吸收的这种不对称性估计高达整个中微子动量的2.2%。与这种不对称性相关联的脉冲星反冲速度被证明是可比的观察到的速度。
Maximizing Science in the Era of LSST, Stars Study Group Report: Rotation and Magnetic Activity in the Galactic Field Population and in Open Star Clusters
Primordial magnetic fields in Population III star formation: a magnetised resolution study
第三星族恒星由于原始气体的分裂而成群形成。虽然均匀的磁场已被证明在现今的恒星形成过程中可以防止碎片化，但尚不清楚现实的k^3/2原始磁场是否具有同样的效果。当中心密度达到10-13 g cm-3时，我们通过引入与速度场均分的饱和磁场来绕过与模拟湍流发电机相关的问题。我们测试了一系列的下沉粒子创建密度从10 -10-10-8克cm-3。在测试范围内，电场并不能抑制气体的碎裂，因此无法阻止碎裂程度随着分辨率的提高而增加。形成的沉降颗粒的数量和沉降颗粒中的总质量不受所有种子场和分辨率上的磁场的影响。除了在模拟箱的最高密度区域，磁压力保持低于气体压力，在该区域磁压力等于但从未超过气体压力。我们的研究结果表明，包含磁场在数值模拟的波普III恒星形成在很大程度上是不重要的。
