Relationships among cosmic ray intensity, the photospheric magnetic field, and solar wind speed

Kazuyuki HAKAMADA; Munetoshi TOKUMARU; Ken'ichi FUJIKI; Masayoshi KOJIMA

Presentation information

Oral

Symbol P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM27_1PM2] Heliosphere and Interplanetary Space

Thu. May 1, 2014 4:15 PM - 6:00 PM 421 (4F)

Convener:*Munetoshi Tokumaru(Solar-Terrestrial Environment Laboratory, Nagoya University), Tomoko Nakagawa(Information and Communication Engineering, Tohoku Institute of Technology), Chair:Munetoshi Tokumaru(Solar-Terrestrial Environment Laboratory, Nagoya University)

4:45 PM - 5:00 PM

[PEM27-03] Relationships among cosmic ray intensity, the photospheric magnetic field, and solar wind speed

*Kazuyuki HAKAMADA¹, Munetoshi TOKUMARU², Ken'ichi FUJIKI², Masayoshi KOJIMA² (1.Chubu University, 2.Solar-Terrestrial Environment Laboratory)

Keywords:cosmic ray intensity, photoshpheric magnetic field, solar wind speed

We visualize three-dimensional structure of the coronal magneic field by using the Radial-Field model for the coronal magnetic field devised by Hakamada with synoptic maps of photospheric magnetic field observed by the NSO/Kitt Peak, USA. As the rsults, we obtained the radial component of the photospheric magnetic field (Br_pho) and the one of the coronal magnetic field (Br_sou) on the source surface on the same field line in the coronal magnetic field. We estimate the solar wind speed (SWS) by using IPS technique divised by STE Lab, Nagoya Univiersity. According to our previous analysis on the Carrignton rotation bases, Log10|Br_pho|, Log10|Br_sou| show good correlations with the SWS for the data of [ -1.0 ]