First solar models with OPAS opacity tables
Ma\"elle Le Pennec, Sylvaine Turck-Chi\`eze, S\'ebastien Salmon,, Christophe Blancard, Philippe Coss\'e, G\'erald Faussurier, Guillaume, Mondet

TL;DR
This paper investigates the impact of new OPAS opacity tables on solar models, showing improvements in matching helioseismic data compared to traditional OPAL and OP tables, thus addressing longstanding discrepancies.
Contribution
It introduces the use of OPAS opacity tables in solar modeling and demonstrates their positive effects on helioseismic agreement, a novel application in this context.
Findings
Improved location of the base of the convective zone.
Better match of solar radiative zone profiles with helioseismic data.
OPAS tables lead to less than 6% difference in Rosseland mean opacity.
Abstract
Stellar seismology appears more and more as a powerful tool for a better determination of the fundamental properties of solar-type stars. However the particular case of Sun is still challenging. The helioseismic sound speed determination continues to disagree with the Standard Solar Model (SSM) prediction for about a decade, questioning the reliability of this model. One of the sources of uncertainty could be in the treatment of the transport of radiation from the solar core to the surface. In this letter, we use the new OPAS opacity tables, recently available for solar modelling, to address this issue. We discuss first the peculiarities of these tables, then we quantify their impact on the solar sound speed and density profiles using the reduced OPAS tables taken on the grids of the OPAL ones. We use the two evolution codes MESA and CLES that led to similar conclusions in the solar…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
