PSTEP Models

SUSANOO

Developer: Shiota, D.; Miyoshi, Y.; Kataoka, R.

A three-dinmeisional MHD simulation of propagation of solar wind and coronal mass ejections in the inner heliosphere (r < 2AU) on the basis of photospheric magnetic field observations. The modeled time profile of solar wind at the Earth’s position is utilized for a prediction of high energy electron flux at the geosynchronous orbit.

URL: http://cidas.isee.nagoya-u.ac.jp/susanoo/

Reference: Shiota, D., R. Kataoka, Y. Miyoshi, T. Hara, C. Tao, K. Masunaga, Y. Futaana, and N. Terada (2014), Inner heliosphere MHD modeling system applicable to space weather forecasting for the other planets, Space Weather, 12, 187–204, doi:10.1002/2013SW000989. etc.

Link to the reference: http://onlinelibrary.wiley.com/doi/10.1002/2013SW000989/abstract

Related PSTEP groups: A01, A02, A03

GAIA

Developer: Jin, H.; Miyoshi, Y.; Fujiwara, H.; Shinagawa, H.

GAIA (Ground-to-Topside Model of Atmosphere and Ionosphere for Aeronomy) is a whole atmosphere GCM which solves physical and chemical processes from the ground to upper atmosphere under interaction with the ionosphere.

URL: http://seg-web.nict.go.jp/GAIA/index_e.html

Reference: Jin, H., Y. Miyoshi, H. Fujiwara, H. Shinagawa, K. Terada, N. Terada, M. Ishii, Y. Otsuka, and A. Saito, Vertical Connection from the Tropospheric Activities to the Ionospheric Longitudinal Structure Simulated by a New Earth’s Whole Atmosphere-Ionosphere Coupled Model, J. Geophys. Res., 116, A01316, doi:10.1029/2010JA015925, 2011. etc.

Link to the reference: http://onlinelibrary.wiley.com/doi/10.1029/2010JA015925/abstract

Related PSTEP groups: A03, A04

Plasma Bubble Model

Developer: Yokoyama, T.

Equatorial plasma bubbles are known to cause severe degradation of satellite-based communication and navigation. This model is able to reproduce nonlinear growth of equatorial plasma bubbles by solving the electrodynamics of equatorial ionosphere with very high spatial resolution (<1km). It is expected to reveal generation mechanisms and to estimate effects on radio wave propagation quantitatively.

Reference: Yokoyama, T., H. Shinagawa, and H. Jin (2014), Nonlinear growth, bifurcation and pinching of equatorial plasma bubble simulated by three-dimensional high-resolution bubble model, J. Geophys. Res. Space Physics, 119, pages 10,474–10,482. doi:10.1002/2014JA020708.

Link to the reference: http://onlinelibrary.wiley.com/doi/10.1002/2014JA020708/abstract

Related PSTEP groups: A03

HF-START

Developer: Kornyanat Hozumi, Takashi Maruyama, Susumu Saito

HF-START (HF Simulator Targeting for All-users’ Regional Telecommunications) is the HF propagation simulator that is developed to meet the needs of space weather users for, but not limit to, telecommunications. It is a user-friendly model.

Related PSTEP groups: A01

GEMSIS-RB (Geospace Environment Modeling System for Integrated Studies – Radiation Belt)

Developer:Shinji Saito

GEMSIS-RB code solves equation of motion for guiding center of charged particles in time-varying, three dimensional electromagnetic fields. The RB code demonstrates trajectories of radiation belt electrons and flux distribution in time-varying, given three dimensional electromagnetic fields from such as empirical geomagnetic field model and global MHD model.

Reference: Saito, S., Y. Miyoshi, and K. Seki (2010), A split in the outer radiation belt by magnetopause shadowing: Test particle simulations, J. Geophys. Res., 115, A08210, doi:10.1029/2009JA014738.

Link to the reference:http://onlinelibrary.wiley.com/doi/10.1029/2009JA014738/abstract

Related PSTEP groups: A03

GEMSIS-RBW (Geospace Environment Modeling System for Integrated Studies – Radiation Belt with Wave particle interaction)

Developer:Shinji Saito

GEMSIS-RBW code calculates acceleration, pitch angle scattering, and atmospheric precipitation of radiation belt electrons bouncing along the magnetic field. This model assumes the scattering by whistler chorus waves propagating parallel to the magnetic field line. This model is supposed to be installed into the RB model in order to demonstrate acceleration and loss process by whistler chorus waves which are expected to cause drastic variation of electron flux in the radiation belt.

Reference: Saito, S., Y. Miyoshi, and K. Seki (2012), Relativistic electron microbursts associated with whistler chorus rising tone elements: GEMSIS-RBW simulations, J. Geophys. Res., 117, A10206, doi:10.1029/2012JA018020.

Link to the reference:http://onlinelibrary.wiley.com/doi/10.1029/2012JA018020/abstract

Related PSTEP groups: A03

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