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- W1678814124 abstract "It is suggested that protons and minor ions in the solar corona can be heated and accelerated by fast shocks. Weak fast shocks with an Alfvén Mach number MA<1.5 can be generated by the interaction between network magnetic fields and emerging intranetwork fields which leads to magnetic reconnection and microflares. The nearly nondeflection of ion motion across the shock ramp leads to a large perpendicular thermal velocity (νth), which is an increasing function of the mass/charge ratio. The heating by subcritical shocks with MA≈1.3 (1.1≤MA≤1.5) leads to a large temperature anisotropy with T⊥/T‖≈50 for O5+ ions and a mild anisotropy with T⊥/T‖≈1.2 for protons. The large perpendicular thermal velocity of He++ and O5+ ions can be partly converted to the radial outflow velocity (u) in the divergent coronal field lines. The heating and acceleration by shocks with MA≈1.3 can lead to u(O5+)≈νth(O5+)≈460 km/s for O5+ ions, u(He++)≈νth(He++)≈360 km/s for He++ ions, and u(H+)≈νth(H+)≈240 km/s for protons at r=3–4 R⊙. These results can explain recent SOHO observations of the heating and acceleration of protons and minor ions in the solar corona. It is suggested that an observational search for weak fast shocks in the coronal holes is important." @default.
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- W1678814124 date "2002-01-01" @default.
- W1678814124 modified "2023-10-14" @default.
- W1678814124 title "Solar coronal heating and weak fast shocks" @default.
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- W1678814124 doi "https://doi.org/10.1016/s0964-2749(02)80208-6" @default.
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