The 17 March 2015 storm: the associated magnetic flux rope structure and the storm development

• Published in: Earth, planets, and space Vol. 68; no. 1; p. 1
• Main Authors: Marubashi, Katsuhide, Cho, Kyung-Suk, Kim, Rok-Soon, Kim, Sujin, Park, Sung-Hong, Ishibashi, Hiromitsu
• Format: Journal Article
• Language: English
• Published: Berlin/Heidelberg Springer Berlin Heidelberg 08-11-2016; Springer Nature B.V
• Subjects: 3. Space science; Earth and Environmental Science; Earth Sciences; Geology; Geophysics/Geodesy; Global Data Systems for the Study of Solar-Terrestrial Variability; Injection rate; Magnetic cloud; Coronal mass ejection; Flux rope; Ring current; Solar wind magnetic field; Geomagnetic storm; Solar wind
• ISSN: 1880-5981; 1880-5981
• DOI: 10.1186/s40623-016-0551-9

The objective of this study is (1) to determine the magnetic cloud (MC) structure associated with the 17 March 2015 storm and (2) to gain an insight into how the storm developed responding to the solar wind conditions. First, we search MC geometries which can explain the observed solar wind magnetic fields by fitting to both cylindrical and toroidal flux rope models. Then, we examine how the resultant MC geometries can be connected to the solar source region to find out the most plausible model for the observed MC. We conclude that the observations are most consistently explained by a toroidal flux rope with the torus plane nearly parallel to the ecliptic plane. It is emphasized that the observations are characterized by the peculiar spacecraft crossing through the MC, in that the magnetic fields to be observed are southward throughout the passage. For understanding of the storm development, we first estimate the injection rate of the storm ring current from the observed
Dst
variation. Then, we derive an expression to calculate the estimated injection rate from the observed solar wind variations. The point of the method is to evaluate the injection rate by the convolution of the dawn-to-dusk electric field in the solar wind and a response function. By using the optimum response function thus determined, we obtain a modeled
Dst
variation from the solar wind data, which is in good agreement with the observed
Dst
variation. The agreement supports the validity of our method to derive an expression for the ring current injection rate as a function of the solar wind variation.
Graphical abstract
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