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Fractionation of the Solar Wind
1995
Highlights of Astronomy
The composition of the solar wind (SW) is not a true sample of the solar composition, but it is fractionated with respect to the solar photosphere. This fractionation follows the well-known first ionization potential (FIP) pattern: When plotting the SW abundances with respect to the solar abundances as a function of FIP, a step function is obtained (Fig. 1). The step at ∼ 10eV has a height of 3-5 in the slow SW, but this is reduced to 1.5-2 in the fast streams, which originate in the coronal
doi:10.1017/s153929960001131x
fatcat:7nxmyx3ntnbjxafiqvxn76ao4u