| GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS |
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Numerical Validation and Comparison of Three Solar Wind Heating Methods by the SIP-CESE MHD Model |
| YANG Li-Ping1,2**, FENG Xue-Shang1, XIANG Chang-Qing1, JIANG Chao-Wei1,2
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1SIGMA Weather Group, State Key Laboratory for Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190
2 College of Earth Sciences, Graduate University of Chinese Academy of Sciences, Beijing 100049
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| Cite this article: |
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YANG Li-Ping, FENG Xue-Shang, XIANG Chang-Qing et al 2011 Chin. Phys. Lett. 28 039601 |
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Abstract We conduct simulations using the three-dimensional (3D) solar-interplanetary conservation element/solution element (SIP-CESE) magnetohydrodynamic (MHD) model and magnetogram data from a Carrington rotation (CR) 1897 to compare the three commonly used heating methods, i.e. the Wentzel–Kramers–Brillouin (WKB) Alfvén wave heating method, the turbulence heating method and the volumetric heating method. Our results show that all three heating models can basically reproduce the bimodal structure of the solar wind observed near the solar minimum. The results also demonstrate that the major acceleration interval terminates about 4RS for the turbulence heating method and 10RS for both the WKB Alfvén wave heating method and the volumetric heating method. The turbulence heating and the volumetric heating methods can capture the observed changing trends by the WIND satellite, while the WKB Alfvén wave heating method does not.
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| Keywords:
96.50.Bh
96.50.Ci
96.50.Tf
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Received: 07 December 2010
Published: 28 February 2011
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| PACS: |
96.50.Bh
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(Interplanetary magnetic fields)
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96.50.Ci
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(Solar wind plasma; sources of solar wind)
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96.50.Tf
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(MHD waves; plasma waves, turbulence)
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