A two-dimensional electrodynamical outer gap model for γ-ray pulsars: γ-ray spectrum     

J. Takata  S. Shibata  K. Hirotani  H-K. Chang 《Monthly notices of the Royal Astronomical Society》2006,366(4):1310-1328

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MHD simulations of jets from accretion disks     

Takahiro Kudoh  Ryoji Matsumoto  Kazunari Shibata 《Astrophysics and Space Science》2003,287(1-4):99-102

We present the MHD simulation including accretion flows in disks, acceleration of outflows from disks, and collimation of the outflows self-consistently. Although it was considered that this kind of simulations only shows the transient phenomena of jets, we found that the outflow and accretion flow reached a quasi-steady state by performing a long-term calculation in a large calculation region. Though the final stage is not exactly the steady state, the acceleration and collimation mechanisms of the outflow were the same as those of the steady theory. The scale of the calculation is approaching to the scale that was observed by the VLBI technique, which provides the current highest resolution for YSO jets.  相似文献   

On the X-ray image of the Crab nebula: comparison with Chandra observations     

Shinpei Shibata  Haruhiko Tomatsuri  Makiko Shimanuki  Kazuyuki Saito  Koji Mori 《Monthly notices of the Royal Astronomical Society》2003,346(3):841-845

An axisymmetric model for the Crab nebula is constructed to examine the flow dynamics in the nebula. The model is based on that of Kennel & Coroniti, although we assume that the kinetic-energy-dominant wind is confined to an equatorial region. The evolution of the distribution function of the electron–positron plasma flowing out in the nebula is calculated. Given viewing angles, we reproduce an image of the nebula and compare it with the Chandra observation.
The reproduced image is not ring-like, but is rather 'lip-shaped'. It is found that the assumption of a toroidal field does not reproduce the Chandra image. We must assume that there is a disordered magnetic field with an amplitude as large as the mean toroidal field. In addition, the brightness contrast between the front and back sides of the ring cannot be reproduced if we assume that the magnetization parameter σ is as small as ∼10⁻³. The brightness profile along the semimajor axis of the torus is also examined. The non-dissipative, ideal-magnetohydrodynamic approximation in the nebula appears to break down.
We speculate that if the magnetic energy is released by some process that produces a turbulent field in the nebula flow and causes heating and acceleration – for example, by magnetic reconnection – then the present difficulties may be resolved (i.e. we can reproduce a ring image and a higher brightness contrast). Thus, the magnetization parameter σ can be larger than previously expected.  相似文献   

Pulsar magnetosphere with conspicuous trans-field flow     

Shinpel Shibata 《Astrophysics and Space Science》1986,119(1):105-107

It is shown that (1) in the pulsar magnetosphere the violation of the ideal-MHD condition,E+v×B0, (i.e., conspicuous trans-field motion and non-zero field aligned electric field (E 0) appears owing to relativistic large inertia, and (2) an axisymmetric numerical model with tenuous plasma suggests that in the region of the trans-field flow a vacuum-like electric field and a closed current circuit develop.Paper presented at the IAU Third Asian-Pacific Regional Meeting, held in Kyoto, Japan, between 30 September–6 October, 1984.  相似文献   

Rotating eruption of an untwisting filament triggered by the 3B flare of 25 April, 1984     

Hiroki Kurokawa  Yoichiro Hanaoka  Kazunari Shibata  Yutaka Uchida 《Solar physics》1987,108(2):251-264

A great 3B flare, whose X-ray class was X13, occurred over a delta-sunspot at 00: 01 UT on April 25, 1984. Before the flare, a strong magnetic shear was found to be formed along the neutral line in the delta-sunspot with shear motions of umbrae. The shear motions of the umbrae were caused by the successive emergence of a magnetic flux rope.Before the flare, several groups of sheared H threads and filaments were found to merge into an elongated filament along the neutral line through the delta-sunspot. In the merging process the helical twists were formed in the filament by the reconnection as in the Pneuman's (1983) model.At the post-maximum phase of the flare, the helically twisted filament spouted out with an untwisting rotation. Examining the morphological and dynamical features of the filament eruption, we concluded that it has some typical features of the flare spray and that it seems to be accelerated by the sweeping-magnetictwist mechanism proposed by Shibata and Uchida (1986).Contributions from the Kwasan and Hida Observatories, University of Kyoto, No. 276.  相似文献   

Two types of jets and origin of macrospicules     

Kazunari Shibata 《Solar physics》1982,81(1):9-17

Comparison between observations of macrospicules and numerical jet models obtained in our previous one-dimensional hydrodynamic simulations suggests that H macrospicules and EUV macrospicules unseen in H have different physical origins. H macrospicules are produced by pressure gradient force at the bright point in the middle or in the upper chromosphere. On the other hand, EUV macrospicules unseen in H are produced by shock waves which originate from network bright-points in the photosphere or in the low chromosphere and have propagated through the chromosphere. An essential difference between the two types of macrospicules is the density ratio between macrospicules and the corona. The critical parameter causing this difference is the height of bright points. The general relation between the density in jets (including also regular spicules) and the height of bright points is discussed.  相似文献   

Numerical analysis of shipping water impact on a deck using a particle method     

Kazuya Shibata  Seiichi Koshizuka   《Ocean Engineering》2007,34(3-4):585-593

The objective of this study is to simulate three-dimensional behavior of shipping water and to predict the impact pressure on the deck using a particle method. An experiment carried out in a two-dimensional wave tank with a fixed deck model was numerically analyzed in three dimensions. The fluid motion, the surface elevation, and the impact pressure on the deck were compared between the experiment and the calculation and good agreement was obtained.  相似文献   

Analysis of the global relationship of biennial variation of sea surface temperature and air-sea heat flux using satellite data     

Masanori Konda  Norihisa Imasato  Akira Shibata 《Journal of Oceanography》1996,52(6):717-746

We investigated the phase difference and the cross correlation coefficient between the band-pass filtered biennial variations of sea surface temperature (SST) and air-sea heat flux estimated by the monthly mean 2°×2° satellite data of Advanced Very High Resolution Radiometer (AVHRR) and Special Sensor Microwave/Imager (SSM/I) from July 1987 to June 1991. Judging from the phase difference, it can be determined whether the biennial variation of SST is controlled by local thermal air-sea interaction or oceanic processes of horizontal transport. When the local air-sea heat flux controls the biennial variation of SST, the phase of SST advances /2 (6 months) against that of the air-sea heat flux. In contrast, when the biennial variation of SST is controlled by the oceanic process, the phase difference between the SST and the air-sea heat flux becomes 0 or (12 months). In this case, two types of the phase differences are determined, depending on which variability of SST and air-sea heat flux is larger. The close thermal air-sea interaction is noticeable in the tropics and in the western boundary current region. The phase difference of /2 appears mainly in the north Pacific, the southeast Indian Ocean, and the western tropical Pacific; zero in the eastern tropical Pacific and the northeast and equatorial Atlantic; and that of in the central equatorial Pacific and north of the intertropical convergence zone (ITCZ) of the Atlantic. Phase differences of 0, , or /2 are possible in the western boundary current regions. This fact indicates that each current plays a different role to the biennial variation of SST. It is inferred that SST anomalies in the tropics are mutually correlated, and the process in which marked SST anomalies in the tropics are transferred to the remote area was probed. In the equatorial Pacific, the SST anomaly is transferred by the long planetary wave. On the other hand, it is found from the phase relationship and the horizontal correlation of SST that the SST anomaly in the central and western equatorial Pacific is connected through atmospheric mediation. It is suggested that the biennial variation of SST in the eastern Indian Ocean is affected by heat transport due to the Indonesian throughflow from the western tropical Pacific. It is found that the mentioned pattern of the interannual variation of SST in the tropical Atlantic as a dipole is not tenable.  相似文献   

Pigeonite-bearing basalts dredged from the Puerto Rico Trench: A microprobe study     

Tsugio Shibata 《Marine Geology》1979,30(3-4):285-297

A microprobe study was carried out on zoned clinopyroxene, composed of a pigeonite core mantled by augite, and plagioclase in six tholeiitic basalts dredged from the Puerto Rico Trench (20° 06.8′N, 65° 06.5′W). The pigeonite cores are characterized by high magnesium contents [Fe/Fe + Mg = 0.19 on the average]; their crystallization temperatures based on the three-pyroxene geothermometer are thus estimated to be higher than those of the well-studied tholeiitic pyroxene assemblages (Hakone, Weiselberg, Mull, Skaergaard, and Bushveld). It is suggested from textural and chemical relationships that pyroxene crystallization started first with precipitation of pigeonite followed by simultaneous precipitation of pigeonite and augite and finally by crystallization of augite alone in the groundmass.  相似文献   

A wind speed retrieval algorithm by combining 6 and 10 GHz data from Advanced Microwave Scanning Radiometer: Wind speed inside hurricanes     

Akira Shibata 《Journal of Oceanography》2006,62(3):351-359

A wind speed retrieval algorithm was developed using 6 and 10 GHz h-pol (6H and 10H) data of the Advanced Microwave Scanning Radiometer (AMSR) aboard the Advanced Earth Observation Satellite-II (ADEOS-II) and AMSR-E aboard AQUA, for the purpose of retrieving wind speed inside rainstorms, primarily hurricanes and typhoons. The h-pol was used rather than the v-pol, because the brightness temperature sensitivity to the ocean wind at h-pol is larger than v-pol. The microwave emission change of 6H and 10H corresponding to ocean wind was evaluated in no-rain areas by combining AMSR and SeaWinds data aboard the ADEOS-II (SeaWinds was NASA’s scatterometer), and it was found that the ratio of the two 6H to 10H increments due to ocean wind is 0.9. Assuming that this result also holds with higher wind speeds and under rainy conditions, the brightness temperatures at 6H and 10H were simulated using a microwave radiative transfer model. A parameter W6 (unit; Kelvin) was then defined, representing an increment at 6H due to ocean wind. W6 is applicable to rainy areas, and to all ranges of sea surface temperature. W6 was compared with wind speed reported by the National Hurricanes Center for several hurricanes in the Western Atlantic Ocean during three years (2002 to 2004). W6 averaged around centers of hurricanes was found to exhibit a sensitivity to wind speed, such as increasing from 22 K to 65 K as the wind speed rose from 65 to 140 knots (33 to 72 m/s), and an empirical relationship relating the averaged W6 to wind speed in hurricanes was derived.  相似文献