October 6, 2021 Poster Open Access

Pezzotti, Camilla

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  <identifier identifierType="DOI">10.5281/zenodo.5552517</identifier>
  <creators>
    <creator>
      <creatorName>Pezzotti, Camilla</creatorName>
      <givenName>Camilla</givenName>
      <familyName>Pezzotti</familyName>
      <affiliation>University of Geneva</affiliation>
    </creator>
  </creators>
  <titles>
    <title>The key role of the host star's rotational history on the evolution of the planetary system - The case of TOI-849 and Kepler-444</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2021</publicationYear>
  <contributors>
    <contributor contributorType="Supervisor">
      <contributorName>Eggenberger, Patrick</contributorName>
      <givenName>Patrick</givenName>
      <familyName>Eggenberger</familyName>
      <affiliation>University of Geneva</affiliation>
    </contributor>
    <contributor contributorType="Researcher">
      <contributorName>Buldgen, Gaël</contributorName>
      <givenName>Gaël</givenName>
      <familyName>Buldgen</familyName>
      <affiliation>University of Geneva</affiliation>
    </contributor>
    <contributor contributorType="Researcher">
      <contributorName>Attia, Omar</contributorName>
      <givenName>Omar</givenName>
      <familyName>Attia</familyName>
      <affiliation>University of Geneva</affiliation>
    </contributor>
    <contributor contributorType="Researcher">
      <contributorName>Bourrier, Vincent</contributorName>
      <givenName>Vincent</givenName>
      <familyName>Bourrier</familyName>
      <affiliation>University of Geneva</affiliation>
    </contributor>
    <contributor contributorType="Supervisor">
      <contributorName>Meynet, Georges</contributorName>
      <givenName>Georges</givenName>
      <familyName>Meynet</familyName>
      <affiliation>University of Geneva</affiliation>
    </contributor>
    <contributor contributorType="Researcher">
      <contributorName>Mordasini, Christoph</contributorName>
      <givenName>Christoph</givenName>
      <familyName>Mordasini</familyName>
      <affiliation>University of Bern</affiliation>
    </contributor>
  </contributors>
  <dates>
    <date dateType="Issued">2021-10-06</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Poster</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/5552517</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.5552516</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;The interaction between the host star and planets has a significant&lt;/p&gt;

&lt;p&gt;role in shaping the evolution of the planetary system. The dissipation of&lt;/p&gt;

&lt;p&gt;tides and the consequent exchange of angular momentum between star and&lt;/p&gt;

&lt;p&gt;planets may significantly impact their orbits and modify the architecture of&lt;/p&gt;

&lt;p&gt;the system. The emission of high-energy stellar radiation is directly linked&lt;/p&gt;

&lt;p&gt;to the stellar rotation rate and its role in determining the efficiency of&lt;/p&gt;

&lt;p&gt;planetary atmospheric evaporation represents a key process suitable to&lt;/p&gt;

&lt;p&gt;explain some peculiar features observed in the population of detected&lt;/p&gt;

&lt;p&gt;exoplanets. In this context, the rotational history of the host star plays a&lt;/p&gt;

&lt;p&gt;key role. In our work, we aim at having an as detailed as possible&lt;/p&gt;

&lt;p&gt;characterisation of the host star of the system provided by thorough&lt;/p&gt;

&lt;p&gt;asteroseismic modelling (when available). Rotating models of the host star&lt;/p&gt;

&lt;p&gt;are then computed by accounting for a comprehensive treatment of angular&lt;/p&gt;

&lt;p&gt;momentum transport by hydrodynamic and magnetic instabilities. We explore a&lt;/p&gt;

&lt;p&gt;range of initial surface rotation rates representative of slow, medium and&lt;/p&gt;

&lt;p&gt;fast rotators, accounting for the degeneracy on the stellar rotational&lt;/p&gt;

&lt;p&gt;history. We finally study the interaction between star and planet, by&lt;/p&gt;

&lt;p&gt;coupling the host star model to our orbital evolution code, simultaneously&lt;/p&gt;

&lt;p&gt;following the impact of tides and atmospheric evaporation. We present recent&lt;/p&gt;

&lt;p&gt;results found in the context of the TOI-849 and Kepler-444 systems.&lt;/p&gt;</description>
  </descriptions>
</resource>