Chromospheres of Various Cool Stars from Models of the UV
Paper presented at the Triennial Earth-Sun Summit (TESS) 2015, held in Indianapolis, IN, USA, 29 April 2015.
Co-authored with Juan Fontenla, Kevin France, Jeff Linsky, and Mariela Vieytes.
Abstract:
One important clue to the physical mechanism of chromospheric heating in the Sun is provided by the well-known widespread presence of chromospheres in most cool stars. Recent UV observations are shedding more light into the characteristics of these chromospheres and transition-regions. The physical modeling of these, combined with the older, observations provides much less ambiguous constraints than the Ca II line and other visible data could provide. We are building this new generation of models that are providing interesting trends that give clues on the atmospheric parameters where physical mechanisms of chromospheric and coronal heating operate. We will present some of the current results and will point to some of the trends that are starting to emerge. This is of course an ongoing topic and much remains to be learnt.
One important clue to the physical mechanism of chromospheric heating in the Sun is provided by the well-known widespread presence of chromospheres in most cool stars. Recent UV observations are shedding more light into the characteristics of these chromospheres and transition-regions. The physical modeling of these, combined with the older, observations provides much less ambiguous constraints than the Ca II line and other visible data could provide. We are building this new generation of models that are providing interesting trends that give clues on the atmospheric parameters where physical mechanisms of chromospheric and coronal heating operate. We will present some of the current results and will point to some of the trends that are starting to emerge. This is of course an ongoing topic and much remains to be learnt.