We will review the theoretical background and the development of the so-called Grad-Shafranov (GS) reconstruction technique that has been used for the past two decades. The GS method employs in-situ spacecraft measurements, including both magnetic field and plasma parameters, to derive a two and a half dimensional cross section of the space plasma structure traversed by the spacecraft. It has been applied to space plasma measurements in the solar wind, at the Earth’s magnetopause, in the magnetotail, and even in the Martian environment. We will present results obtained from the GS reconstruction of magnetic flux ropes in the solar wind, ranging from a few minutes to a few days in duration, with the largest ones traditionally identified as magnetic clouds (MCs). In particular, we will discuss quantitative analysis of the connection between the physical characterizations of MCs and the corresponding source region properties on the Sun. This original study, interdisciplinary in nature, offers unique physical insight into the origination of this important type of solar eruptions, and is also highly relevant to solar observations and associated studies.
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10月12日
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