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Article type: Cover
1992 Volume 85 Issue 3 Pages
Cover1-
Published: June 20, 1992
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
App1-
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
C1-C3
Published: June 20, 1992
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C4-
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C5-C7
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[in Japanese], [in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C8-C9
Published: June 20, 1992
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Nobunari KASHIKAWA, Sadanori OKAMURA
Article type: Article
1992 Volume 85 Issue 3 Pages
C10-
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C11-C15
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C16-
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C17-C19
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C20-C23
Published: June 20, 1992
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We discuss the distribution and the evolution of X-ray clusters of galaxies. Hot Intra-Cluster Plasma (ICP) is the source of X-ray emission. The sample data of X-ray clusters will provide the informations of the cluster evolution which includes the clustering process and the thermal history of ICP. We calculate the number counts and the red shift distribution of the clusters emitting X-ray. We compared the computred results with the results mainly from the Extended Medium Sensitivty Survey (MSS) by Einstein Observatory. The previous analysis of a subsample of MSS presents that the observed slope is flatter than that of "Euclidean" model. This observed result suggests us that the observed deviation from the "Euclidean" model can be the evidence the evolution of clusters. We discuss the evolutionary effects comparing the observational data with the computed cluster number count and the redshift distribution of clusters.
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C24-C29
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C30-C31
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C32-C39
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C40-C43
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C44-C47
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C48-C49
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C50-C56
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Hitoshi HANAMI
Article type: Article
1992 Volume 85 Issue 3 Pages
C57-C59
Published: June 20, 1992
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We studied a planet-magnetosphere interaction model for γ-ray bursts with the picture of a current circuit which consists of the magnetosphere and the surface of a neutron star. The motion of planets or comets in the magnetosphere works as the battery in the circuit system. The physical condition on the surface of the neutron star is important to make a closed current circuit inducing good conversion from the kinetic energy of a planet to that of the magnetosphere oscillation. An old and cooled neutron star with the temperature ≃ 10eV can prepare the condition for closing the current circuit in the surface of the neutron star. The planet-magnetosphere system is unstable to feedback instability related to the variability of the γ-ray bursts.
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[in Japanese], [in Japanese], Randy R. Ross, Andy C. Fabian
Article type: Article
1992 Volume 85 Issue 3 Pages
C60-C63
Published: June 20, 1992
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C64-C67
Published: June 20, 1992
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We outline the theoretical properties of relativistic, perpendicular, magnetosonic, collisionless shock waves in electron-positron-heavy ion plasmas of relevance to astrophysical sources of synchrotron radiation. We describe a new process of preferential shock acceleration of nonthermal positrons through collective processes of plasmas. All the upstream particles which are electromagnetically reflected from the shock front dissipate their energy in the form of intense electromagnetic waves. The left handed magnetosonic waves emitted by the heavy ions are resonantly absorbed by the positrons behind the shock front. This absorption gives rise to a power law spectrum N(γ)dγ∝γ^<-s> with s ≈ 2 in energy range from γ=γ_1 to γ=(m_<ion>/Zm_<e±>)γ_1, when the upstream flow energy of the heavy ions exceeds that of the electrons and positrons.
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C68-
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C69-C74
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C75-C80
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[in Japanese], [in Japanese], A. Lanza
Article type: Article
1992 Volume 85 Issue 3 Pages
C81-C82
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C83-C84
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[in Japanese], [in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C85-C86
Published: June 20, 1992
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[in Japanese], [in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C87-C92
Published: June 20, 1992
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C93-C94
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C95-C101
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C102-C104
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[in Japanese]
Article type: Article
1992 Volume 85 Issue 3 Pages
C105-C109
Published: June 20, 1992
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Takashi Nakamura, Noriaki Shibazaki, Toshio Murakami, Atsumasa Yoshida
Article type: Article
1992 Volume 85 Issue 3 Pages
C110-C123
Published: June 20, 1992
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Recent observation of GRBs (Gamma Ray Burst) by GRO (Gamma Ray Observatory) raised puzzling questions on what GRBs are. At first look of the observational results, the galactic disk origin may be denied due to apparent isotropy and inhomogeneity of the distribution of the source. However, if one takes the lower bound for the quadrupole moment of the distribution of the sources, sources can still be anisotropic. That is, for example, a homogeneous spheroidal distribution of the sources with eccentricity of 0.7 can be compatible with the quadrupole moment and V/V_<max> test within statistical error on 2 to 3σ level. In view of this situation, three possible origins of the gamma ray bursters are discussed in this paper. They are; 1) Comets in Oort like clouds around old neutron stars in the galactic disk falling inside the tidal radius due to perturbation by passing molecular clouds of mass 〜 10^4M_⨀ and the size 〜 1Opc. 2) Comets around old neutron stars in the galactic halo of size 〜 50kpc which were ejected from globular clusters in their early phase of evolutions and/or were formed in the evolution of Population III stars. 3) Coalescing binary neutron stars at a cosmological distance. We discuss the distribution, the event rate and the energetics for each model.
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
C124-C125
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
C126-C127
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
App2-
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Article type: Appendix
1992 Volume 85 Issue 3 Pages
App3-
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Article type: Cover
1992 Volume 85 Issue 3 Pages
Cover2-
Published: June 20, 1992
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Article type: Cover
1992 Volume 85 Issue 3 Pages
Cover3-
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