Poster Open Access

Spatially resolved solar spectroscopy as benchmark

Ellwarth, Monika


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  <identifier identifierType="DOI">10.5281/zenodo.5558036</identifier>
  <creators>
    <creator>
      <creatorName>Ellwarth, Monika</creatorName>
      <givenName>Monika</givenName>
      <familyName>Ellwarth</familyName>
      <affiliation>Georg-August-Universität Göttingen</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Spatially resolved solar spectroscopy as benchmark</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <dates>
    <date dateType="Issued">2021-10-08</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/5558036</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.5558035</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/plato2021</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;For the detection and characterization of exoplanets, observed spectra need to be understood at extremely high detail. Knowledge about the radiation emitted from the host star is of utmost importance, and the Sun is the best available laboratory to understand Sun-like stars. At the Institute for Astrophysics G&amp;ouml;ttingen, we observe the Sun using a high resolution Fourier Transform Spectrograph (FTS). Our observations of the resolved Sun provide insight into the variable spectral behaviour across different limb angles, which can provide crucial information about limb darkening, convective velocities, and line profile variability relevant for radial velocity (RV) work. We show first results from our atlas of the solar spectrum at different limb angles that can put models of transit observations and stellar RV variability on a firm footing.&lt;/p&gt;</description>
  </descriptions>
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