| Co-Investigator(Kenkyū-buntansha) |
高野 秀路 日本大学, 工学部, 准教授 (00222084)
小川 英夫 大阪府立大学, 理学(系)研究科(研究院), 教授 (20022717)
土橋 一仁 東京学芸大学, 教育学部, 教授 (20237176)
亀野 誠二 国立天文台, チリ観測所, 教授 (20270449)
松本 倫明 法政大学, 人間環境学部, 教授 (60308004)
伊王野 大介 国立天文台, チリ観測所, 准教授 (60425402)
|
|---|
| Budget Amount *help |
¥47,710,000 (Direct Cost: ¥36,700,000、Indirect Cost: ¥11,010,000)
Fiscal Year 2016: ¥3,380,000 (Direct Cost: ¥2,600,000、Indirect Cost: ¥780,000)
Fiscal Year 2015: ¥2,860,000 (Direct Cost: ¥2,200,000、Indirect Cost: ¥660,000)
Fiscal Year 2014: ¥7,410,000 (Direct Cost: ¥5,700,000、Indirect Cost: ¥1,710,000)
Fiscal Year 2013: ¥7,020,000 (Direct Cost: ¥5,400,000、Indirect Cost: ¥1,620,000)
Fiscal Year 2012: ¥27,040,000 (Direct Cost: ¥20,800,000、Indirect Cost: ¥6,240,000)
|
|---|
| Outline of Final Research Achievements |
It remains uncertain how magnetic fields are important in the process of star formation. The main reason is the technical difficulty of the measurements of the field strength. In this study, to derive the magnetic field associated with dense cores, we carried out Zeeman observations of CCS which is abundant in the prestellar phase. As a result, we detected a first clear Zeeman spliting of CCS and derived the field strength of about 200 micro Gauss toward TMC-1.
This suggests that the TMC-1 core is magnetically supported against the gravitational collapse.
For theoretical study, we developed a tool to make polarisation maps with numerical simulation data.
|
