HR: 11:20h
AN: SH41C-05 INVITED     [PDF]
TI: IPS/SMEI potential joint observations
AU: * Tokumaru, M
EM: tokumaru@stelab.nagoya-u.ac.jp
AF: STE Lab., Nagoya Univ., 3-13 Honohara, Toyokawa, 442-8507 Japan
AU: Kojima, M
EM: kojima@stelab.nagoya-u.ac.jp
AF: STE Lab., Nagoya Univ., 3-13 Honohara, Toyokawa, 442-8507 Japan
AU: Fujiki, K
EM: fujiki@stelab.nagoya-u.ac.jp
AF: STE Lab., Nagoya Univ., 3-13 Honohara, Toyokawa, 442-8507 Japan
AU: Jackson, B V
EM: bvjackson@ucsd.edu
AF: CASS/UCSD, 9500 Gilman Dr., La Jolla,, San Diego, CA 92093-0424 United States
AU: Hick, P
EM: pphick@ucsd.edu
AF: CASS/UCSD, 9500 Gilman Dr., La Jolla,, San Diego, CA 92093-0424 United States
AB: Interplanetary scintillation (IPS) measurements are known as one of remote-sensing techniques which enable us to gain access to global features of the solar wind (e.g. quasi-stationary corotating structures, transient streams associated with CMEs). We have carried out a long-term collaboration on the reconstruction of the heliospheric features from IPS measurements made with the 327 MHz four-station system of the Solar-Terrestrial Environment Laboratory (STEL), Nagoya University. Under the collaboration, we have developed the computer-assisted tomography (CAT) analysis method, which allows us to retrieve the 3D distribution of the solar wind velocity and density from IPS data. We also have been making the real-time reconstruction experiment of heliospheric features using STEL IPS data and the CAT method. Based on these results, we propose here the joint observations of IPS and SMEI. The SMEI is a powerful tool to investigate the global heliospheric features, and its capability is complementary to one of IPS observations; That is, SMEI observations provide a high-resolution image of the solar wind density distribution, while IPS observations provide reliable estimates of the solar wind velocity. Therefore, a combination of IPS and SMEI observations is essential for achieving a precise reconstruction of global heliospheric (velocity and density) features by the CAT analysis.
DE: 2102 Corotating streams
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2139 Interplanetary shocks
DE: 2164 Solar wind plasma
DE: 7513 Coronal mass ejections
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting