Wolk, Scott
Sowmya, Krishnamurthy
Shapiro, Alexander I.
Witzke, Veronika
Nèmec, Nina-E.
Chatzistergos, Theodosis
Yeo, Kok Leng
Krivova, Natalie A.
Solanki, Sami K.
2021-02-26
<p>The emission in the near ultraviolet Ca II H&K lines, often quantified via the S-index, has been serving as a prime proxy of solar and stellar magnetic activity. Despite the broad usage of the S-index, the link between the coverage of a stellar disk by magnetic features and Ca II H&K emission is not fully understood. In order to fill this gap we developed a physics-based model to calculate the solar S-index. To this end, we made use of the distributions of the solar magnetic features derived from the simulations of magnetic flux emergence and surface transport, together with the Ca II H&K spectra synthesized using a non-local thermodynamic equilibrium (non-LTE) radiative transfer code.</p>
<p>We show that the value of the solar S-index is influenced by the inclination angle between the solar rotation axis and the observer’s line-of-sight, i.e. the solar S-index values obtained by an out-of-ecliptic observer are different from those obtained by an ecliptic-bound observer. This is important for comparing the magnetic activity of the Sun to other stars. We computed time series of the S-index as they would be observed at various inclinations dating back to 1700. We find that depending on the inclination and period of observations, the activity cycle in solar S-index can appear weaker or stronger than in stars with a solar-like level of magnetic activity. We show that there is nothing unusual about the solar chromospheric emission variations in the context of stars with near-solar magnetic activity.</p>
https://doi.org/10.5281/zenodo.4564796
oai:zenodo.org:4564796
eng
Zenodo
https://zenodo.org/communities/coolstars20half
https://zenodo.org/communities/eu
https://doi.org/10.5281/zenodo.4564795
info:eu-repo/semantics/openAccess
Creative Commons Attribution 4.0 International
https://creativecommons.org/licenses/by/4.0/legalcode
CS20.5, The 20.5th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, virtually anywhere, March 2-4, 2021
The Sun and the Heliosphere
Solar activity
Solar chromosphere
Stellar activity
Modelling Solar Ca II H&K Emission Variations
info:eu-repo/semantics/conferencePoster