| Project/Area Number |
15540239
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | Rikkyo University |
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Principal Investigator |
SHIBAZAKI Moriaki Rikkyou University, Department of Physics, Professor, 理学部, 教授 (50206124)
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| Co-Investigator(Kenkyū-buntansha) |
MORII Mikio Japan Aerospace Exploration Agency, Research Associate, 宇宙科学研究本部, 研究員 (90392810)
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| Project Period (FY) |
2003 – 2005
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| Project Status |
Completed (Fiscal Year 2005)
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| Budget Amount *help |
¥2,300,000 (Direct Cost: ¥2,300,000)
Fiscal Year 2005: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 2004: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 2003: ¥1,100,000 (Direct Cost: ¥1,100,000)
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| Keywords | anomalous pulsars / soft gamma repeaters / magnetars / neutron stars / グリッチ / ソフトガンマバースト / 超強磁場中性子星 / クラスト / 星震 / リコネクション |
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| Research Abstract |
(1)Thermal evolution magnetars
We 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 1806-20
On 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+61
We 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-wavelengths
We 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
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