| Project/Area Number |
17540222
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | Japan Aerospace Exploration Agency |
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Principal Investigator |
SHIMIZU Toshifumi JAXA, Institute of Space & Astronautical Science, Assistant Professor, 宇宙科学研究本部, 助教授 (60311180)
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| Co-Investigator(Kenkyū-buntansha) |
KATSUKAWA Yukio National Astronomical Observatory, Research Associate, 国立天文台・SOLAR-B推進室, 上級研究員 (00399289)
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| Project Period (FY) |
2005 – 2006
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| Project Status |
Completed (Fiscal Year 2006)
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| Budget Amount *help |
¥1,000,000 (Direct Cost: ¥1,000,000)
Fiscal Year 2006: ¥400,000 (Direct Cost: ¥400,000)
Fiscal Year 2005: ¥600,000 (Direct Cost: ¥600,000)
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| Keywords | Solar atmosphere / Coordinated observations / Magnetic fields / Photosphere / Mass flows / 国際共同観測 / コロナ活動 / 速度場 / プラズマ |
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| Research Abstract |
High spatial resolution optical observations of the solar surface was successfully performed using solar telescopes installed on the Canaries Islands, Spain on 3-14 July 2005. The telescopes and their focal plane instruments involved in this observation are : 1) two Stokes polarimeters at visible light and infrared, installed in the German Vacuum Tower Telescope at Tenerife, 2) filter imagers with Swedish Solar Telescope at La Palma, and 3) filter imagers with Dutch Open Telescope at La Palma. This observation was performed based on an observing proposal (PI: Y.Katsukawa) accepted as the International Time Program in 2005. To monitor magnetic-field structure and dynamics in the corona, the target of interest is also observed simultaneously by EUV telescopes onboard TRACE and SoHO satellites.
Studies using the data from this observation have given some new knowledge on dynamics and magnetic coupling in the solar atmosphere. One of our finding is small-scale photospheric events with extremely red-shifted Stokes V signal in sunspot moat regions. The red-shift in Stokes V signal suggests the existence of mass downflows with 〜10 km/s, which exceeds a sound velocity at the photosphere. The size of the events is extremely small and the duration of events are less than 1 hour. The red-shifted signal can be interpreted as downward flow from magnetic reconnection occurring at the upper chromosphere or lower photosphere.
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