Heating of stellar chromospheres and coronae: Evidence for non-magnetic heating

摘要: A detailed analysis of the radiative losses from outer atmospheres magnetically active stars suggests that two emission components are present. These may correspond to distinct mechanisms non-radiative heating operate in cool stars. One these depends on stellar rotation rate, and is associated with magnetic activity. The other component varies effective temperature, appears be insensitive surface gravity, independent rate. energy loss this second results observed lower boundaries diagrams flux density versus colour, hence name “basal chromosphere.” mechanism dissipation acoustic waves. temperatures basal part atmosphere limited a few tens thousands degrees or less G- K-type F-type dwarfs reach up transition-region temperatures, higher.