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Mirror instability upstream of the termination shock (TS) and in the heliosheath
Authors:Bruce T Tsurutani  Ezequiel Echer  Olga P Verkhoglyadova  Gurbax S Lakhina  FL Guarnieri
Institution:1. Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA;2. INPE, Sao Jose dos Campos, SP, Brazil;3. CSPAR, University of Alabama, Huntsville, AL, USA;4. Indian Institute of Geomagnetism, Navi Mumbai, India;5. UNIVAP, Sao Jose dos Campos, SP, Brazil;1. Scuola di Ingegneria SI, Università della Basilicata, via dell’Ateneo Lucano, 10 - 85100 Potenza, Italy;2. CNR-IMIP Bari, via Amendola 122/D - 70126 Bari, Italy;3. Dipartimento di Ingegneria Meccanica e Aerospaziale, Università di Roma La Sapienza, via Eudossiana, 18 - 00183 Roma, Italy;1. Department of Aerospace Engineering, Shenyang Aerospace University, Shenyang 110000, China;2. Department of Aerospace Engineering, Harbin Institute of Technology, Harbin 150001, China;1. School of Systems Science, Beijing Normal University, Beijing, 100875, China;2. Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, 100029, China;3. SIGMA Weather Group, State Key Laboratory for Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China;1. National Institute for Space Research (INPE), Sao Jose dos Campos, Brazil;2. Federal University of Goias, Jatai, Brazil;3. Federal University of Jataí (UFJ), Jataí, Brazil;1. Department of Civil Engineering, Faculty of Engineering, Suleyman Demirel University, Isparta, Turkey;2. Department of Engineering Mathematics, Faculty of Engineering and Natural Sciences, Bahcesehir University, Istanbul, Turkey;1. State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China;2. Key Laboratory of Science and Technology on Environmental Space Situation Awareness, Chinese Academy of Sciences, Beijing 100190, China;3. University of Chinese Academy of Sciences, Beijing 100190, China
Abstract:We experimentally identify mirror mode (MM) structures in the Voyager 1 heliosheath data for the first time. This is done using the magnetic field data alone. The heliosheath MM structures are found to have the following characteristics: (1) quasiperiodic spacings with a typical scale size of ~57 ρp, (2) little or no angular changes across the structures (~3° longitude and ~3° latitude), and (3) a lack of sharp boundaries at the magnetic dip edges. It is demonstrated that the pickup of interstellar neutrals in the upstream region of the termination shock (TS) and quasiperpendicular TS plasma compression are the causes of MM instability during intervals when the IMF is nearly orthogonal to the solar wind flow direction. Concomitant additional injection of pickup ions (PUIs) throughout the heliosheath will lead to further MM amplification. MM structures in planetary magnetosheaths and interplanetary sheaths are discussed for comparative purposes. Multiple sources of free energy are often involved.
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