March 1, 2021 Poster Open Access

Criscuoli, Serena; Marchenko, Sergey; DeLand, Matthew; Choudary, Debi; Kopp, Greg

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  <identifier identifierType="DOI">10.5281/zenodo.4570266</identifier>
  <creators>
    <creator>
      <creatorName>Criscuoli, Serena</creatorName>
      <givenName>Serena</givenName>
      <familyName>Criscuoli</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-4525-9038</nameIdentifier>
      <affiliation>National Solar Observatory</affiliation>
    </creator>
    <creator>
      <creatorName>Marchenko, Sergey</creatorName>
      <givenName>Sergey</givenName>
      <familyName>Marchenko</familyName>
      <affiliation>Goddard Space Flight Center</affiliation>
    </creator>
    <creator>
      <creatorName>DeLand, Matthew</creatorName>
      <givenName>Matthew</givenName>
      <familyName>DeLand</familyName>
      <affiliation>Goddard Space Flight Center</affiliation>
    </creator>
    <creator>
      <creatorName>Choudary, Debi</creatorName>
      <givenName>Debi</givenName>
      <familyName>Choudary</familyName>
      <affiliation>San Fernando Observatory</affiliation>
    </creator>
    <creator>
      <creatorName>Kopp, Greg</creatorName>
      <givenName>Greg</givenName>
      <familyName>Kopp</familyName>
      <affiliation>LASP</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Understanding variability of solar Balmer lines</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <subjects>
    <subject>Balmer lines</subject>
    <subject>Stellar variability</subject>
    <subject>Stellar Chromosphere</subject>
    <subject>Solar Irradiance variability</subject>
    <subject>Magnetic activity</subject>
    <subject>Activity Indices</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2021-03-01</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/4570266</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.4570265</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/coolstars20half</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="https://creativecommons.org/licenses/by/4.0/legalcode">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;Precise, adequately high-cadence, long-term records of spectral variability at different temporal scales lead to better understanding of&amp;nbsp; a wide variety of phenomena including&amp;nbsp; stellar atmospheres and dynamos, evolution of the magnetic fields on a stellar photosphere, convective motions, and rotational periods. These, in turn, are fundamental for the detectability of exoplanets, the characterization of their atmospheres&amp;nbsp;and habitability, as well as characterization of stellar magnetospheres and winds. The Sun, viewed as a star via spectral irradiance measurements, offers a means of exploring such measurements while also having the imaging capability to help discern the causes of observed spectral variations. &amp;nbsp;In this study, we investigate the variability of solar Balmer lines (H-&amp;alpha;, &amp;beta;, &amp;gamma; and &amp;delta;) observed by space-borne radiometers, combining these precise, long-term observations with abundant, high-resolution data from&amp;nbsp; the ground-based NSO/ISS spectrograph. We relate the detected variability to magnetic features on the solar disk. We find that on solar-rotation timescales (~month), the Balmer line activity indices (defined as line-core to line-wing ratios) closely follow variations in the total solar irradiance (which is predominantly photospheric), thus frequently (specifically, during passages of big sunspot groups) deviates from behavior of the line-activity indices that track chromospheric activity levels. At longer timescales (years), the correlation with chromospheric indices increases, with periods of low- or even anti- correlation found at intermediate timescales. Comparisons with Balmer-line variability patterns obtained from a semi-empirical model indicate&amp;nbsp; the periods of low/anti correlations should be attributed to the increase of the relative abundance of network, which affects the Ca-index while leaving almost un-altered the H&amp;alpha;-index.&lt;/p&gt;</description>
  </descriptions>
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