Poster Open Access

What M dwarf models reveal about their UV spectra?

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

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  <identifier identifierType="DOI">10.5281/zenodo.4570984</identifier>
      <creatorName>Tilipman, Dennis</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0001-9361-6629</nameIdentifier>
      <affiliation>National Solar Observatory, University of Colorado, Boulder</affiliation>
      <creatorName>Vieytes, Mariela</creatorName>
      <affiliation>Instituto de Astronomia y Fisica del Espacio (UBA-CONICET), Buenos Aires, Argentina</affiliation>
      <creatorName>Linsky, Jeffrey L.</creatorName>
      <givenName>Jeffrey L.</givenName>
      <affiliation>JILA, University of Colorado, Boulder</affiliation>
      <creatorName>Andrea Buccino</creatorName>
      <affiliation>Instituto de Astronom ́ıa y F ́ısica del Espacio (UBA-CONICET), Buenos Aires, Argentina</affiliation>
      <creatorName>Kevin France</creatorName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="">0000-0002-1002-3674</nameIdentifier>
      <affiliation>LASP, University of Colorado, Boulder</affiliation>
    <title>What M dwarf models reveal about their UV spectra?</title>
    <subject>Cool Stars on the main sequence</subject>
    <date dateType="Issued">2021-02-26</date>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4567475</relatedIdentifier>
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    <rights rightsURI="">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
    <description descriptionType="Abstract">&lt;p&gt;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.&lt;/p&gt;</description>
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