Hydrodynamic interaction between the be star and the pulsar in the TeV binary PSR B1259-63/LS 2883
Hydrodynamic interaction between the be star and the pulsar in the TeV binary PSR B1259-63/LS 2883
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DOI：
10.1093/pasj/63.4.893
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发表时间：
2011-05
影响因子：
2.3
通讯作者：
A. Okazaki;S. Nagataki;T. Naito;A. Kawachi;K. Hayasaki;S. Owocki;J. Takata
中科院分区：
文献类型：
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作者：
A. Okazaki;S. Nagataki;T. Naito;A. Kawachi;K. Hayasaki;S. Owocki;J. Takata
我们利用3-D SPH方法模拟了TeV双星PSR B1259−63/LS 2883中Be-脉冲星系统的潮汐和风相互作用，研究了Be星星与脉冲星之间的相互作用.我们首先运行一个没有脉冲星风和Be风的模拟，只考虑脉冲星对Be盘的引力效应。在这个模拟中，气体粒子以恒定的速率从Be星星的赤道表面喷出，该表面的倾斜方向与多波段观测一致。我们运行模拟，直到Be盘完全发育并开始重复与脉冲星的定期潮汐相互作用。然后，我们打开脉冲星风和Be风。我们运行两个模拟不同的风质量损失率的Be星星，一个为B2 V型和其他显着较早的光谱类型。虽然脉冲星风和Be风相互作用面的整体形状与解析解一致，但脉冲星风对Be盘的影响是深远的。脉冲星风剥离了Be盘的外部，将盘截断在一个半径明显小于脉冲星轨道的地方。因此，我们的结果排除了脉冲星穿过近星点Be盘的想法，这在以前的研究中一直假设。它还证明，接触不连续的位置可以显着不同的相位时，脉冲星风直接击中的Be盘和那些当脉冲星风与Be风碰撞。因此，重要的是要充分考虑到的Be星星的拱星环境，以构建一个令人满意的模型，这个原型TeV的二进制。
We study the interaction between the Be star and the pulsar in the TeV binary PSR B1259−63/LS 2883, using 3-D SPH simulations of the tidal and wind interactions in this Be-pulsar system. We first run a simulation without pulsar wind nor Be wind, taking into account only the gravitational effect of the pulsar on the Be disk. In this simulation, the gas particles are ejected at a constant rate from the equatorial surface of the Be star, which is tilted in a direction consistent with multi-waveband observations. We run the simulation until the Be disk is fully developed and starts to repeat a regular tidal interaction with the pulsar. Then, we turn on the pulsar wind and the Be wind. We run two simulations with different wind mass-loss rates for the Be star, one for a B2V type and the other for a significantly earlier spectral type. Although the global shape of the interaction surface between the pulsar wind and the Be wind agrees with the analytical solution, the effect of the pulsar wind on the Be disk is profound. The pulsar wind strips off an outer part of the Be disk, truncating the disk at a radius significantly smaller than the pulsar orbit. Our results, therefore, rule out the idea that the pulsar passes through the Be disk around periastron, which has been assumed in the previous studies. It also turns out that the location of the contact discontinuity can be significantly different between phases when the pulsar wind directly hits the Be disk and those when the pulsar wind collides with the Be wind. It is thus important to adequately take into account the circumstellar environment of the Be star, in order to construct a satisfactory model for this prototypical TeV binary.