Published February 26, 2021 | Version v3
Poster Open

What M dwarf models reveal about their UV spectra?

  • 1. National Solar Observatory, University of Colorado, Boulder
  • 2. Instituto de Astronomia y Fisica del Espacio (UBA-CONICET), Buenos Aires, Argentina
  • 3. JILA, University of Colorado, Boulder
  • 4. Instituto de Astronom ́ıa y F ́ısica del Espacio (UBA-CONICET), Buenos Aires, Argentina
  • 5. LASP, University of Colorado, Boulder


Stellar ultraviolet (UV) radiation has significant implications on habitability of their exoplanets, yet this radiation is partly unobservable due to interstellar medium absorption. We used the radiative transfer code SSRPM to build stellar models of two M dwarfs and synthesize their UV spectra, particularly focusing on the far-UV and extreme-UV spectra. Our most important findings are that 1) the coronae of two M dwarfs are responsible for more than half of their respective EUV fluxes, and 2) the continuum in the FUV band between 145 and 170 nm is responsible for about half of total emission in this band. Here, we discuss the significance of these results and outline future projects aimed to improve our understanding of solar and stellar UV emission.



Files (2.1 MB)

Name Size Download all
2.1 MB Preview Download