Correlation Height of the Source Region of Si II Emission Lines in Coronal Hole Regions |
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| Institution: | 1. Department of Geophysics, Peking University, Beijing 100871;2. Max-Plank-Institut für Sonnensystemforschung, Germany;1. P.K. Sternberg Astronomical Institute of M.V. Lomonosov Moscow State University, Universitetskii prosp. 13, 119234 Moscow, Russia;2. Space Research Institute of Russian Academy of Sciences, Profsoyuznaya str. 84/32, 117997 Moscow, Russia;3. Max Planck Institute for the Physics of Complex Systems, Noethnitzer Str. 38, 01187 Dresden, Germany;1. Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, PR China;2. Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China;3. Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Shandong University at Weihai, Weihai 264209, PR China;4. University of Chinese Academy of Sciences, Beijing 100049, PR China;1. EötvösUniversity, Department of Astronomy, Budapest, Hungary;2. EötvösUniversity, Department of Geophysics and Space Science, Budapest, Hungary;1. Faculty of Physics, Sofia University, 1164 Sofia, Bulgaria;2. IGAM, Institute of Physics, University of Graz, 8010 Graz, Austria;3. Abastumani Astrophysical Observatory at Ilia State University, 0162 Tbilisi, Georgia;4. Space Research Institute, Austrian Academy of Sciences, 8042 Graz, Austria;5. Catholic University of America, Washington, DC 20064, USA;6. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;7. Visiting, Department of Geosciences, Tel Aviv University, Ramat-Aviv, Tel Aviv 69978, Israel;8. Department of Physics, DSB Campus, Kumaun University, Nainital 263 001, India |
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| Abstract: | The height of the source region of Si II emission lines characterizes the height of the bottom layer of solar atmosphere's transition region. The correlation analysis of the intensities of ultraviolet spectral lines and the threedimensional structure of magnetic field yielded by force-free extrapolation is a new method for determining the height of ultraviolet emission lines’ source region. It has been found that the height thus obtained is larger than that given by traditional viewpoint. Because the existing numerical analyses with this method are scarce, this result has to be further verified with more observational materials. In this work, this method is applied to the Si II emission lines observed by SOHO/SUMER for the solar surface region beneath the solar coronal hole at southern pole and to the magnetic fields measured by National Solar Observatory/Kitt Peak (NSO/KP) in U.S.A. The correlation height of the source region of Si II emission lines in coronal hole region is approximately 5.0 Mm. This result supports the conclusion that the height of the bottom layer of transition region in coronal hole region is larger than that in quiet regions. Moreover, some new phenomena have been discovered and their causes are probed. |
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