REVIEW 6 cited by
Numerical simulations of quiet Sun magnetism: On the contribution from a small-scale dynamo
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Numerical simulations of quiet Sun magnetism: On the contribution from a small-scale dynamo
read the original abstract
We present a series of radiative MHD simulations addressing the origin and distribution of mixed polarity magnetic field in the solar photosphere. To this end we consider numerical simulations that cover the uppermost 2-6 Mm of the solar convection zone and we explore scales ranging from 2 km to 25 Mm. We study how the strength and distribution of magnetic field in the photosphere and subsurface layers depend on resolution, domain size and boundary conditions. We find that 50% of the magnetic energy at the \tau=1 level comes from field with the less than 500 G strength and that 50% of the energy resides on scales smaller than about 100 km. While probability distribution functions are essentially independent of resolution, properly describing the spectral energy distribution requires grid spacings of 8 km or smaller. The formation of flux concentrations in the photosphere exceeding 1 kG requires a mean vertical field strength greater than 30-40 G at \tau=1. The filling factor of kG flux concentrations increases with overall domain size as magnetic field becomes organized by larger, longer lived flow structures. A solution with a mean vertical field strength of around 85 G at \tau=1 requires a subsurface RMS field strength increasing with depth at the same rate as the equipartition field strength. We consider this an upper limit for the quiet Sun field strength, which implies that most of the convection zone is magnetized close to equipartition. We discuss these findings in view of recent high-resolution spectropolarimetric observations of quiet Sun magnetism.
Forward citations
Cited by 6 Pith papers
-
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 spectr...
-
Towards inertial-mode helioseismology: Direct sensing of solar rotation at 75 deg latitude and 0.8 Rsun
The m=1 high-latitude inertial mode frequency implies solar rotation of 365.3 nHz at 75° latitude and 0.8 R_sun, exceeding the p-mode reference by 8.1 nHz.
-
Predictability of a solar flare in May 2024 using observational data-driven MHD simulations
Observational data-driven MHD simulations reproduced an X1.6 flare's onset and showed that photospheric velocity input extends prediction lead time beyond one hour.
-
Solar Vortices: Catalysts of Magnetoacoustic Wave Dissipation and Atmospheric Heating
Simulations indicate photospheric vortices produce higher chromospheric temperatures and stronger supersonic upflows than non-vortex regions, without shifting shock formation heights.
-
Solar Vortices: Catalysts of Magnetoacoustic Wave Dissipation and Atmospheric Heating
Simulations find vortex regions exhibit higher temperatures and faster shock upflows, indicating they boost magnetoacoustic wave dissipation in the chromosphere.
-
Research Progress on Solar Small-Scale Dynamo
Literature review summarizing observations, theoretical models, and MHD simulations of the small-scale solar dynamo operating in the solar photosphere and convection zone.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.