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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The diagnostic separates granulation-sensitive and stable lines in late-G and K dwarfs, with FeI lines showing lower velocity sensitivity than FeII as effective temperature decreases, making solar line selections non-portable.
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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Sensitivity of spectral lines to granulation: from the Sun to K-type stars
The diagnostic separates granulation-sensitive and stable lines in late-G and K dwarfs, with FeI lines showing lower velocity sensitivity than FeII as effective temperature decreases, making solar line selections non-portable.