High minor ion outflow speeds in the inner corona and observed ion charge states in interplanetary space

摘要: Flow speeds recently derived from chromospheric/transition region and coronal observations indicate that the solar wind acceleration process takes place at heights in atmosphere much lower than previously imagined. Doppler-dimming of O VI λ1032 λ1037 spectral lines show this is not only true for background electron-proton but also minor ions. The limits these on flow speed O+5 ions are least a factor 3-4 higher highest expected earlier ion studies. It likely other reach similar inner corona. interpretation situ charge state needs to be reexamined light new velocity measurements. Large imply some species may close equilibrium corona any distance. Given large deviation equilibrium, use ratios determine temperatures no longer appropriate. Using newest available atomic data together with most recent observational constraints electron temperatures, densities, speeds, we find models high outflow order (about 130-230 km s-1 below 3 R☉) consistent observations. We then discuss how can used future theoretical studies heating mechanisms.