权益分类	功能权益	普通用户	{{item.name}}会员
{{category.name}}	{{benefitItem.name}}

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

磁星磁场起源及能量恢复机制研究

基本信息

批准号：
15540239
负责人：
SHIBAZAKI Moriaki
金额：
$ 1.47万
依托单位：
Rikkyo University
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
2003
资助国家：
日本
起止时间：
2003 至 2005
项目状态：
已结题

项目摘要

(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

（1）磁星的热演化我们研究了磁星的热演化，考虑了磁场的耗散。特别是磁场耗散对表面温度的影响，已引起人们的注意。将计算结果与软伽马中继站和异常X射线源的观测结果进行了比较，得出以下结论。由于磁场耗散而产生的热沉积应该发生在中子星星的外壳中。·在恒星的生命周期中，总的能量消耗应该达到10^<49>-10 ^<50>尔格。（2）SGR 1806- 20的巨型耀斑2004年12月8日，GEOTAIL卫星观测到了SGR 1806-20的巨型耀斑，并获得了大量的软γ射线。我们计算了相对论喷流发射的X射线和软γ射线，并将我们的模型与观测结果进行了比较。我们的数值模型可以很好地再现所观察到的光变曲线。我们发现喷气式飞机开着。 ...更多信息 g角小于0.2弧度。此外，与各向同性模型相比，射流模型给出6 × 10^<46>erg的总发射能量，这明显小于各向同性情况下的总发射能量。（3）4U 0142+ 61的时间观测利用1999年的ASCA资料，对4U 0142+61进行了时间分析。通过比较ASCA结果与RXTE结果的时序分析，我们发现4U 0142+61在ASCA观察之前经历了毛刺。我们还得到了脉冲频率及其时间导数跃变的Δν/ν~10^<-4>和Δν^^·/ν^·~10^<-2>。这些数值与普通中子星中观测到的数值相似，这意味着磁星的内部结构可能与普通中子星相似。我们还观察到脉冲轮廓的变化，这可能与毛刺有关。我们认为磁层的变形可能是脉冲轮廓变化的一个原因。(4)4U 0142+61的多波长同时观测我们在X射线、可见光和近红外波段进行了多波长同时观测。我们发现，在可见光和近红外波段的发射包括2个分量。我们还发现了R带的吸收特征。少