| Project/Area Number |
05640315
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| Research Category |
Grant-in-Aid for General Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | RIKKYO UNIVERSITY |
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Principal Investigator |
HOSHI Reiun RIKKYO UNIV., DEPT.of physics.PROF, 理学部, 教授 (70062601)
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| Co-Investigator(Kenkyū-buntansha) |
YABE Takashi Gunma UNIV., DEPT.of EngineeringPROF, 工学部, 教授 (60016665)
SHIBAZAKI Noriaki Rikkyo UNIV., DEPT.of Physics.ASSIST, 理学部, 助教授 (50206124)
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| Project Period (FY) |
1993 – 1994
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| Project Status |
Completed (Fiscal Year 1994)
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| Budget Amount *help |
¥2,100,000 (Direct Cost: ¥2,100,000)
Fiscal Year 1994: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 1993: ¥1,500,000 (Direct Cost: ¥1,500,000)
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| Keywords | pulsar wind / jet / supernova remnant / shock wave / particle acceleration / synchrotron radiation |
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| Research Abstract |
We have developed simulation programs to study the interaction of a pulsar wind with stellar and interstellar matters. When the pulsar wind ejected from a moving neutron star collides with the interstellar matter, the bow shock is expected to be formed at the place where the ram pressures of pulsar and interstellar matter winds balance. Our simulation code developed can calculate the behavior of the bow shock stably when the Mach number is not so high. We are now improving the programs so as to conduct simulations stably even when the Mach number is cosiderably high.
We have studied the interaction of a jet with a supernova remnant. We derived an analytical solution to the propagation of forward and reverse shocks after the jet collides with the remnant. When applied to the SS 433/W50 system, we found that our model can explain the radio and X-ray morphology of the system relatively well. Comparing our model with the observations of the SS 433/W 50 system, we could determine the densities of jet and interstellar matters and a jet velocity to be - 0.01cm^<-3>, - 0.001cm^<-3>, and - 2x10^9cms^<-1>, respectivery. We also found that X-rays from the lobes can be explained in terms of synchrotron emission by electrons accelerated at the reverse shock.
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