Study on the origin of the magnetic fields of magnetars and on the mechanism of the energy rekease

（1）Thermal evolution magnetarsWe have studed the thermal evolution of magnetars taking into account the dissipation of magnetic fields。我们已经支付了注意力，特别是由于磁场扩散对表面温度的影响。我们从软伽马重复器和异常X射线脉冲器的观测中得出了以下的汇编，对计算结果的比较。“热沉积”应该在中子星的外地壳中占据磁场。在星星的生命周期中，总能量被排除在10^-<49>10 ^<50>erg之外。（2）SGR 1806- 20的巨型耀斑2004年12月8日GEOTAIL卫星观测到SGR 1806-20的巨型耀斑，有大量的软伽马射线。我们已经计算了X射线和软伽马射线是从相对式喷气机发射的，并将我们的模型与观测器进行了比较。我们的数字模型可以重新制作一条相当好的光线曲线。我们找到了喷气式飞机。 ... More G角度比0.2半径少。Furthermore，与同位素模型比较，喷气模型给了6x 10^<46>erg到总发电量，在同位素情况下比它小得多。（3）Timing Observation of 4U0142 + 61 We have conducted the timing analyses for the 4U0142 +61，使用ASCA data obtained in 1999。从比较RXTE结果的ASCA结果与时间分析结果，我们找到了4U 0142+61在ASCA观察前发现的故障。We also obtained/\~10^\-4&gt; and\^\-10^\-2&gt; for the jumps in pulse f\and its time derivative。这些价值观的事实与那些在普通脉冲器中观察到的相似之处在于，磁性的内部结构可能与普通中子星相似。我们也注意到了脉搏曲线中的变化，可能与闪烁有关。我们建议磁圈的修改可能是脉冲剖面图更改的原因。（4）4U 0142+61在多波段的同步观测，我们在X射线、视觉波段和近红外波段中进行同步和多波段的观测。我们在视觉和近红外波段中发现了2个分量的发射信号。我们还在R波段找到了吸收功能。Less（低）

(1)Thermal evolution magnetarsWe have studied the thermal evolution of magnetars taking into account the dissipation of magnetic fields. We have paid attention, especially on the influence of the magnetic field dissipation on the surface temperature. We derived the following conclusions from the comparison of the computed results with the observations of the soft gamma repeaters and anomalous X-ray pulsars.・The heat deposition due to the magnetic field dissipation should occur in the outer crust of the neutron star.・The total energy dissipated during the life time of stars should amount to 10^<49>-10^<50> erg.(2)Giant flare from SGR 1806-20On December 8 2004 the GEOTAIL satellite observed the giant flare with the huge amount of soft gamma rays from SGR 1806-20. We have calculated the X-rays and soft gamma rays emitted from the relativistic jet and have compared our model with the observations. Our numerical model can reproduce the observed light curve very well. We found the jet openin … More g angle to be less than 0.2 radian. Furthermore, compared with the isotropic model, the jet model gives 6 x 10^<46> erg to the total emitted energy, which is significantly smaller than that in the isotropic case.(3)Timing observation of 4U 0142+61We have conducted the timing analyses for the 4U 0142+61, using the ASCA data obtained in 1999. From comparing the ASCA results with the RXTE results for the timing analyses, we found that 4U 0142+61 underwent the glitch before the ASCA observation. We also obtained Δν/ν~10^<-4> and Δν^^・/ν^^・~10^<-2> for the jumps in pulse frequency and its time derivative. The fact that these values are similar to those observed in ordinary pulsars implies that the internal structure of magnetars may be similar to that of ordinary neutron stars. We have also observed the change in pulse profile, which may be associated with the glitch. We suggest that the deformation of the magnetosphere may be a cause for the pulse profile change.(4) Simultaneous observation of 4U 0142+61 in multi-wavelengthsWe have conducted the simultaneous and multi-wavelength observations in X-ray, visual and near-infrared bands. We found that the emission in the visual and near-infrared bands consists of 2 components. We also found the absorption feature in the R-band. Less