Poster Open Access

What M dwarf models reveal about their UV spectra?

Tilipman, Dennis; Vieytes, Mariela; Linsky, Jeffrey L.; Andrea Buccino; Kevin France

Dublin Core Export

<?xml version='1.0' encoding='utf-8'?>
<oai_dc:dc xmlns:dc="" xmlns:oai_dc="" xmlns:xsi="" xsi:schemaLocation="">
  <dc:creator>Tilipman, Dennis</dc:creator>
  <dc:creator>Vieytes, Mariela</dc:creator>
  <dc:creator>Linsky, Jeffrey L.</dc:creator>
  <dc:creator>Andrea Buccino</dc:creator>
  <dc:creator>Kevin France</dc:creator>
  <dc:description>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.</dc:description>
  <dc:subject>Cool Stars on the main sequence</dc:subject>
  <dc:title>What M dwarf models reveal about their UV spectra?</dc:title>
All versions This version
Views 11975
Downloads 8649
Data volume 177.6 MB101.3 MB
Unique views 8862
Unique downloads 8049


Cite as