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INJECTION OF PLASMA INTO THE NASCENT SOLAR WIND VIA RECONNECTION DRIVEN BY SUPERGRANULAR ADVECTION
Yang, Liping; He, Jiansen; Peter, Hardi; Tu, Chuanyi; Chen, Wenlei; Zhang, Lei; Marsch, Eckart; Wang, Linghua; Feng, Xueshang; Yan, Limei; Yang, LP (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
Department空间科学部
Source PublicationASTROPHYSICAL JOURNAL
2013
Volume770Issue:1Pages:6
ISSN0004-637X
Language英语
KeywordMagnetic Reconnection Solar Wind Sun: Chromosphere Sun: Corona
AbstractTo understand the origin of the solar wind is one of the key research topics in modern solar and heliospheric physics. Previous solar wind models assumed that plasma flows outward along a steady magnetic flux tube that reaches continuously from the photosphere through the chromosphere into the corona. Inspired by more recent comprehensive observations, Tu et al. suggested a new scenario for the origin of the solar wind, in which it flows out in a magnetically open coronal funnel and mass is provided to the funnel by small-scale side loops. Thus mass is supplied by means of magnetic reconnection that is driven by supergranular convection. To validate this scenario and simulate the processes involved, a 2.5 dimensional (2.5D) numerical MHD model is established in the present paper. In our simulation a closed loop moves toward an open funnel, which has opposite polarity and is located at the edge of a supergranulation cell, and magnetic reconnection is triggered and continues while gradually opening up one half of the closed loop. Its other half connects with the root of the open funnel and forms a new closed loop which is submerged by a reconnection plasma stream flowing downward. Thus we find that the outflowing plasma in the newly reconnected funnel originates not only from the upward reconnection flow but also from the high-pressure leg of the originally closed loop. This implies an efficient supply of mass from the dense loop to the dilute funnel. The mass flux of the outflow released from the funnel considered in our study is calculated to be appropriate for providing the mass flux at the coronal base of the solar wind, though additional heating and acceleration mechanisms are necessary to keep the velocity at the higher location. Our numerical model demonstrates that in the funnel the mass for the solar wind may be supplied from adjacent closed loops via magnetic reconnection as well as directly from the footpoints of open funnels.
Indexed BySCI
Document Type期刊论文
Identifierhttp://ir.nssc.ac.cn/handle/122/5039
Collection空间科学部
Corresponding AuthorYang, LP (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
Recommended Citation
GB/T 7714
Yang, Liping,He, Jiansen,Peter, Hardi,et al. INJECTION OF PLASMA INTO THE NASCENT SOLAR WIND VIA RECONNECTION DRIVEN BY SUPERGRANULAR ADVECTION[J]. ASTROPHYSICAL JOURNAL,2013,770(1):6.
APA Yang, Liping.,He, Jiansen.,Peter, Hardi.,Tu, Chuanyi.,Chen, Wenlei.,...&Yang, LP .(2013).INJECTION OF PLASMA INTO THE NASCENT SOLAR WIND VIA RECONNECTION DRIVEN BY SUPERGRANULAR ADVECTION.ASTROPHYSICAL JOURNAL,770(1),6.
MLA Yang, Liping,et al."INJECTION OF PLASMA INTO THE NASCENT SOLAR WIND VIA RECONNECTION DRIVEN BY SUPERGRANULAR ADVECTION".ASTROPHYSICAL JOURNAL 770.1(2013):6.
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