3D MHD simulations of solar faculae reveal a center-to-limb transition in induced radial velocity from redshift to blueshift at heliocentric angles above 60 degrees, producing a phase-lagged transit profile and spectral-line dependence.
Three-dimensional simulations of near-surface convection in main-sequence stars. III. The structure of small-scale magnetic flux concentrations
3 Pith papers cite this work, alongside 63 external citations. Polarity classification is still indexing.
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abstract
The convective envelopes of cool main-sequence stars harbour magnetic fields with a complex global and local structure. These fields affect the near-surface convection and the outer stellar atmospheres in many ways and are responsible for the observable magnetic activity of stars. Our aim is to understand the local structure in unipolar regions with moderate average magnetic flux density. These correspond to plage regions covering a substantial fraction of the surface of the Sun (and likely also the surface of other Sun-like stars) during periods of high magnetic activity. We analyse the results of 18 local-box magnetohydrodynamics simulations covering the upper layers of the convection zones and the photospheres of cool main-sequence stars of spectral types F to early M. The average vertical field in these simulations ranges from 20 to 500G. We find a substantial variation of the properties of the surface magnetoconvection between main-sequence stars of different spectral types. As a consequence of a reduced efficiency of the convective collapse of flux tubes, M dwarfs lack bright magnetic structures in unipolar regions of moderate field strength. The spatial correlation between velocity and the magnetic field as well as the lifetime of magnetic structures and their sizes relative to the granules vary significantly along the model sequence of stellar types.
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astro-ph.SR 3years
2026 3verdicts
CONDITIONAL 3representative citing papers
SRA-derived photospheric activity indicators track stellar RV variability up to a factor of two better than classical proxies like logR'HK across 14 G/K stars.
Synthetic spectra tests show Zeeman broadening recovers M dwarf magnetic field strengths more reliably with joint abundance fitting and WAIC selection than with free line strengths or BIC/AIC, which underestimate by 30-50% in active cases.
citing papers explorer
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Decoding the Radial Velocity Signatures of Solar Faculae with 3D MHD Simulations
3D MHD simulations of solar faculae reveal a center-to-limb transition in induced radial velocity from redshift to blueshift at heliocentric angles above 60 degrees, producing a phase-lagged transit profile and spectral-line dependence.
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Spectral Ratio Analysis: probing of a new suite of stellar activity indicators as a tool for astrophysical noise mitigation
SRA-derived photospheric activity indicators track stellar RV variability up to a factor of two better than classical proxies like logR'HK across 14 G/K stars.
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Testing the reliability of magnetic field strength measurements for M dwarfs
Synthetic spectra tests show Zeeman broadening recovers M dwarf magnetic field strengths more reliably with joint abundance fitting and WAIC selection than with free line strengths or BIC/AIC, which underestimate by 30-50% in active cases.