| Date |
Author + Title |
Description |
| 2005/04/08 |
T. HADA,
Introductions of solar wind and space plasma
|
|
| 2005/04/15 |
K. BEPPU,
under graduate research
|
Estimation of equivalent electrical circuit of fuel cell via fractal integration |
| 2005/04/22 |
S. MATSUKIYO,
Introduction of decay instability of finite amplitude circularly polarized
Alfven wave
|
Review of "An instability of finite amplitude circularly polarized
Alfven wave" (M.L.Goldsteint, Astrophys. Journal.,1978), which dirived
the linear dispersion relation of the decay instability of finite amplitude
circularly polarized Alfven wave, as a double three wave interaction.
|
| 2005/05/06 |
M. OHNISHI,
Structure of perpendicular shocks in collisionless plasma
|
Review of "Structure of perpendicular shocks in collisionless plasma"
(M.M.Leroy, Phys. Fluid.,1983). |
| 2005/05/13,20 |
M2 students |
Practices and discussions of presentation in SGEPPS meeting 2005, Chiba. |
| 2005/05/27 |
Y. KURAMITSU,
"Chaos" and Gyroresonant surfing acceleration |
A new acceleration or energization mechanism of charged particles in space
and astrophysical plasmas. In the presence of an electrostatic potential
gradient and a circularly polarized electromagnetic monochromatic wave,
particles are accelerated efficiently by keeping cyclotron resonance with
the wave due to the electrostatic dragging force. In addition, particles
can propagate against the electrostatic potential even if they have smaller
parallel energy. |
| 2005/06/03 |
Y. KURAMITSU,
Nonlinear interaction between a charged particle and an MHD pulse |
When the particle velocity is small (adiabatic regime), the probability
that the particle be reflected by the MHD pulse is essentially determined
by the pitch angle only, and is thus independent of the velocity. On the
other hand, in the non-adiabatic regime, the reflection probability is
shown to be inversely proportional to the square root of the normalized
velocity. |
| 2005/06/10 |
Y. NARIYUKI,
An introduction of wave-wave interaction in parallel Alfven turbulence |
The relationship between the basic nonlinear process (the decay instability
and the modulational instability) in parallel propagating MHD waves and
phase coherence is discussed. When the wave modes exchange the energy,
the phases are "locked", and when there is no exchange energy,
the phases can slip freely. |
| 2005/06/24 |
T. HADA,
Introductions of solar wind physics (1): isothermal model
|
|
| 2005/07/01 |
B. LEMBEGE,
Physics of collisionless shocks from macro to micro scales
|
|
| 2005/07/08 |
Y. IKEDA,
Numerical simulation of plasma behavior under the external electromagnetic
field |
|
| 2005/07/15 |
T. UNOKI,
Numerical simulations of instabilities in transition regions of colissionless
shocks |
|
| 2005/07/22 |
Y.KATSUKI,
Numerical methods for computational Fluid Dynamics via finite difference
method: from advection equation to MHD equation |
|
| 2005/07/29 |
T.HASEGAWA,
Numerical experiment of electron-positron shocks |
|
| 2005/09/09 |
V.MUNOZ,
Longitudinal oscillations in a nonextensive relativestic plasma |
The dispersion relation of longitudinal ocsillations in a relativestic
plasmas in the context of the nonextensive statistics formalism proposed
by Tsallis. |
| 2005/09/26-29 |
SGEPSS Fall Meeting |
Society of Geomagnetism and Earth, Planetary and Space Sciences fall meeting, Kyoto. Univ
|
| 2005/10/31 |
B. Pandey ,
Magnetorotational instability in a proroplanetary disk |
One of the important differences between protoplanetary disks and otherastrophysical
accretion disks is the coupling level of gas and the magnetic field.The
protoplanetary disks are very cold and dnese, so the degree of ionization
is verylow. This leads to the inertia of the disk fluid being carried by
the neutrals and thecurrent being carried by the electrons or ions. This
gives rise to novelmagnetohydrodynamic features in a WIP disk and magnetorotational
instability mayoperate on on very short scale-lengths and will play important
role in the transportof mass and angular momentum. This talk revisits the
magnetorotaional instabilityin a WIP disk and examines the role of various
constituents of the ionizedcomponent on the instability. |