3D Radiative MHD Simulations of Starspots II: Large-scale Structure
arXiv:2412.16921 · doi:10.1051/0004-6361/202452747
Abstract
We compute realistic 3D radiative MHD near-surface models of starspots with substantial penumbrae on cool main-sequence stars using the MURaM simulation code. This work is an improvement on the the previous starspot models in a slab geometry. The umbra, penumbra and the quiet star for all starspots are distinct, not only in intensity and temperature, but also in thermodynamic and velocity structure. These models represent a significant step towards modelling contribution of starspots to stellar lightcurves.
8 pages, 6 figures, accepted for publication in A&A
References in corpus (10)
- Numerical simulations of quiet Sun magnetism: On the contribution from a small-scale dynamo
- SOAP 2.0: A tool to estimate the photometric and radial velocity variations induced by stellar spots and plages
- spotrod: a semi-analytic model for transits of spotted stars
- Statistical methods for exoplanet detection with radial velocities
- Small-scale Dynamo in Cool Stars: I. Changes in stratification and near-surface convection for main-sequence spectral types
- Testing MURaM and MPS-ATLAS against the quiet solar spectrum
- Sunspot simulations: penumbra formation and the fluting instability
- Characterization of magneto-convection in sunspots -- The Gough & Tayler stability criterion in MURaM sunspot simulations
- A distinct magnetic property of the inner penumbral boundary III. Analysis of simulated sunspots
- How rare are counter Evershed flows?
Cited by in corpus (3)
- Doppler imaging combined with high-cadence photometry. I. Revisiting the surface of a pre-main-sequence flare star
- Simulations of facular magnetic fields on cool stars I: Main sequence stars with solar metallicity
- Sunspot simulations with MURaM -- I. Parameter study using potential field initial conditions