supported by the National Natural Science Foundation of China (NSFC 42174200);Shenzhen Science and Technology Program (grant No. RCJC20210609 104422048);Shenzhen Key Laboratory Launching Project (No. ZDSYS20210702140800001);Guangdong Basic and Applied Basic Research Foundation (2023B1515040021);the Fundamental Research Funds for the Central Universities (grant No. HIT.OCEF.2023047)。
The solar coronal magnetic field is a pivotal element in the study of eruptive phenomena, and understanding its dynamic evolution has long been a focal point in solar physics. Numerical models, driven directly by obse...
supported by Strategic Priority Research Program of the Chinese Academy of Sciences No. XDB0560000;National Key R&D Program of China No. 2022YFF0503804;NSFC grants 11933009, 12273107, U2031141 and 12073073;grants associated with the Yunling Scholar Project of Yunnan Province;the Yunnan Province Scientist Workshop of Solar Physics;the Yunnan Key Laboratory of Solar Physics and Space Exploration of Code 202205AG070009;the Special Project for the construction of science and technology innovation centers faced to South Asiaand Southeast Asia-Yunnan International Joint Innovation Platform: “China-Malaysia HF-VHF Advanced Radio Astronomy Technology International Joint Laboratory of Yunnan” (202303AP140003);the support by grants associated with the Yunnan Revitalization Talent Support Program;the Foundation of the Chinese Academy of Sciences (Light of West China Program)。
The propagation of disturbances in the solar atmosphere is inherently three-dimensional(3D), yet comprehensive studies on the spatial structure and dynamics of 3D wave fronts are scarce. Here we conduct high-resolutio...
support from the National Natural Science Foundation of China(NSFC,Grant Nos.41974197,41804162,and 42104158);supported by Central Plains Science and Technology Innovation Leading Talents of Henan Province under grant No.244200510012。
It is generally believed that coronal mass ejections(CMEs)have magnetic flux rope structures because of their helical shapes.However,only about 30%–40%of interplanetary CMEs(ICMEs)have a local magnetic flux rope stru...
supported by the National Key Research and Development Projects (Grant Nos.2021YFB3300601,2021YFB3300603,2021YFB3300604);Fundamental Research Funds for the Central Universities (No.DUT22QN241).
Traditional topology optimization methods often suffer from the“dimension curse”problem,wherein the com-putation time increases exponentially with the degrees of freedom in the background grid.Overcoming this challe...
The objective of this article was to carry out a statistical study of the occurrences of CMEs from solar cycles 23 and 24 and to deduce interpretations as a contribution to a greater understanding of heliosphere dynam...
funding by Fundamental Research Grant Scheme(FRGS)under Ministry of Higher Education(KPT)Malaysia with the grant No.FRGS/1/2023/STG07/UKM/02/1;supported by Universiti Sains Malaysia through Short-Term Grant with project No.304/PFIZIK/6315730;supported by JSPS KAKENHI grant Nos.JP20H01961,JP22K03707,JP21H04518,JP22K21345。
A geomagnetic storm is a global disturbance of Earth?s magnetosphere,occurring as a result of the interaction with magnetic plasma ejected from the Sun.Despite considerable research,a comprehensive classification of s...
supported by the National Natural Science Foundation of China(NSFC)U2031108;Yunnan Key Laboratory of Solar Physics and Space Science under the number YNSPCC202213。
Solar active regions(ARs)are formed by the emergence of current-carrying magnetic flux tubes from below the photosphere.Although for an isolated flux tube the direct and return currents flowing along the tube should b...