Poster Open Access

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

Pezzotti, Camilla


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    <dct: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</dct:title>
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    <dct:description>&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;</dct:description>
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