Matthias Rempel

A distinct magnetic property of the inner penumbral boundary III. Analysis of simulated sunspots

Graphic image depicting radial profiles of continuum intensity
Friday, May 8, 2020

The analyses of sunspot observations revealed a fundamental magnetic property of the umbral boundary, the invariance of the vertical component of the magnetic field.

Opposite Polarity Magnetic Fields and Convective Downflows in a Simulated Sunspot Penumbra

Graphic image of opposite polarity magnetic fields
Tuesday, March 31, 2020

Recent numerical simulations and observations of sunspots show a significant amount of opposite polarity magnetic fields within the sunspot penumbra. Most of the opposite polarity fields are associated with convective downflows.

Constraining nonlinear dynamo models using quasi-biennial oscillations from sunspot area data

Graphic depicting continuous wavelet spectra of the sunspot area (SSA)
Thursday, July 25, 2019

Solar magnetic activity exhibits variations with periods between 1.5–4 years, the so-called quasi-biennial oscillations (QBOs), in addition to the well-known 11-year Schwabe cycles. The solar dynamo is thought to be the responsible mechanism for the generation of the QBOs.

Three-dimensional modeling of chromospheric spectral lines in a simulated active region

Simulated images of Ca II 8542 Å, Ca II K, Mg II k, and H
Friday, May 3, 2019

Recently, the radiative magnetohydrodynamic (R-MHD) code MURaM was extended to include the corona. The code was used to simulate a bipolar active region with additional parasitic flux emergence near one of the sunspots that produced a flare.

First computer model to simulate a realistic solar flare

Image depicting a solar flare or cme

A team of scientists has, for the first time, used a single, cohesive computer model to simulate the entire life cycle of a solar flare.

Transport of Internetwork Magnetic Flux Elements in the Solar Photosphere

Graph of displacement probability distributions
Tuesday, October 23, 2018

The motions of small-scale magnetic flux elements in the solar photosphere can provide some measure of the Lagrangian properties of the convective flow.

Evershed and Counter-Evershed Flows In Sunspot MHD Simulations

Field line connectivity and associated pressure perturbation image
Wednesday, December 13, 2017

There have been a number of reports in the literature of counter-Evershed flows in well developed sunspot penumbrae, i.e. flows directed towards the umbra.

Small-scale dynamo Simulations

Magnetic field amplification in exploding granules image
Wednesday, December 13, 2017

Magnetic field amplification in exploding granules and the role of deep and shallow recirculation

Nature of Grand Minima and Maxima from Fully Non-Linear Flux-Transport Dynamos

Identified Grand Minima and Maxima
Thursday, September 7, 2017

We aim to investigate the nature and occurrence characteristics of grand solar minimum and maximum periods, which are observed in the solar proxy records such as 10Be and 14C, using a fully non-linear Babcock-Leighton type flux transport dynamo including momentum and entropy equations.

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