Anthony R. Yeates
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View article: Witnessing Magnetic Reconnection in Tangled Superpenumbral Fibrils Around a Sunspot
Witnessing Magnetic Reconnection in Tangled Superpenumbral Fibrils Around a Sunspot Open
Three-dimensional magnetic reconnection is a fundamental plasma process crucial for heating the solar corona and generating the solar wind, but resolving and characterizing it on the Sun remains challenging. Using high-quality data from th…
View article: The Sun’s Open–Closed Flux Boundary and the Origin of the Slow Solar Wind
The Sun’s Open–Closed Flux Boundary and the Origin of the Slow Solar Wind Open
The Sun’s open–closed flux boundary (OCB) separates closed and open magnetic field lines, and is the site for interchange magnetic reconnection processes thought to be linked to the origin of the slow solar wind (SSW). We analyze the globa…
View article: Winding and magnetic helicity in periodic domains
Winding and magnetic helicity in periodic domains Open
In simply-connected Euclidean domains, it is well-known that the topological complexity of a given magnetic field can be quantified by its magnetic helicity, which is equivalent to the total, flux-weighted winding number of magnetic field …
View article: Persistence and Burn-in in Solar Coronal Magnetic Field Simulations
Persistence and Burn-in in Solar Coronal Magnetic Field Simulations Open
Simulations of solar phenomena play a vital role in space-weather prediction. A critical computational question for automating research workflows in the context of data-driven solar coronal magnetic field simulations is quantifying a simul…
View article: Latitude Quenching Nonlinearity in the Solar Dynamo
Latitude Quenching Nonlinearity in the Solar Dynamo Open
We compare two candidate nonlinearities for regulating the solar cycle within the Babcock–Leighton paradigm: tilt quenching (whereby the tilt of active regions is reduced in stronger cycles) and latitude quenching (whereby flux emerges at …
View article: Latitude Quenching Nonlinearity in the Solar Dynamo
Latitude Quenching Nonlinearity in the Solar Dynamo Open
We compare two candidate nonlinearities for regulating the solar cycle within the Babcock-Leighton paradigm: tilt quenching (whereby the tilt of active regions is reduced in stronger cycles) and latitude quenching (whereby flux emerges at …
View article: A New Field Line Tracer for the Study of Coronal Magnetic Topologies
A New Field Line Tracer for the Study of Coronal Magnetic Topologies Open
We present a new code for the tracing of magnetic field lines and calculation of related quantities such as the squashing factor in the solar corona. The Universal Fieldline Tracer ( UFiT ) is an open-source package that can currently take…
View article: The Sun’s Non-Potential Corona over Solar Cycle 24
The Sun’s Non-Potential Corona over Solar Cycle 24 Open
The global magnetic field in the solar corona is known to contain free magnetic energy and magnetic helicity above that of a current-free (potential) state. But the strength of this non-potentiality and its evolution over the solar cycle r…
View article: The Sun's Non-Potential Corona over Solar Cycle 24
The Sun's Non-Potential Corona over Solar Cycle 24 Open
The global magnetic field in the solar corona is known to contain free magnetic energy and magnetic helicity above that of a current-free (potential) state. But the strength of this non-potentiality and its evolution over the solar cycle r…
View article: Transition to a weaker Sun: Changes in the solar atmosphere during the decay of the Modern Maximum
Transition to a weaker Sun: Changes in the solar atmosphere during the decay of the Modern Maximum Open
The Sun experienced a period of unprecedented activity during the 20th century, now called the Modern Maximum (MM). The decay of the MM after cycle 19 has changed the Sun, the heliosphere, and the planetary environments in many ways. Howev…
View article: Transition to a weaker Sun: Changes in the solar atmosphere during the decay of the Modern Maximum
Transition to a weaker Sun: Changes in the solar atmosphere during the decay of the Modern Maximum Open
Context. The Sun experienced a period of unprecedented activity during the 20th century, now called the Modern Maximum (MM). The decay of the MM after its maximum in cycle 19 has changed the Sun, the heliosphere, and the planetary environm…
View article: A change in solar radio spectrum during the decay of the Modern Maximum
A change in solar radio spectrum during the decay of the Modern Maximum Open
The Sun experienced a period of unprecedented activity during solar cycle 19 in 1950s and 1960s, now called the Modern Maximum (MM). The decay of the MM has changed the Sun, the heliosphere and the planetary environments in many ways. Howe…
View article: A Near-half-century Simulation of the Solar Corona
A Near-half-century Simulation of the Solar Corona Open
We present an overview of results from a magnetofrictional model of the entire solar corona over a period of 47 yr. The simulation self-consistently reproduces decades of solar phenomena, varying in duration between rapid eruptions and the…
View article: Introduction to Field Line Helicity
Introduction to Field Line Helicity Open
Field line helicity measures the net linking of magnetic flux with a single magnetic field line.It offers a finer topological description than the usual global magnetic helicity integral, while still being invariant in an ideal evolution u…
View article: Introduction to Field Line Helicity
Introduction to Field Line Helicity Open
Field line helicity measures the net linking of magnetic flux with a single magnetic field line. It offers a finer topological description than the usual global magnetic helicity integral, while still being invariant in an ideal evolution …
View article: Computation of Winding-Based Magnetic Helicity and Magnetic Winding Density for SHARP Magnetograms in Spherical Coordinates
Computation of Winding-Based Magnetic Helicity and Magnetic Winding Density for SHARP Magnetograms in Spherical Coordinates Open
Magnetic helicity has been used widely in the analysis and modelling of solar active regions. However, it is difficult to evaluate and interpret helicity in spherical geometry since coronal magnetic fields are rooted in the photosphere and…
View article: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models Open
We investigate which scalar quantity or quantities can best predict the loss of equilibrium and subsequent eruption of magnetic flux ropes in the solar corona. Our models are initialized with a potential magnetic arcade, which is then evol…
View article: Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models
Eruptivity Criteria for Solar Coronal Flux Ropes in Magnetohydrodynamic and Magnetofrictional Models Open
We investigate which scalar quantity or quantities can best predict the loss of equilibrium and subsequent eruption of magnetic flux ropes in the solar corona. Our models are initialized with a potential magnetic arcade, which is then evol…
View article: Surface Flux Transport on the Sun
Surface Flux Transport on the Sun Open
We review the surface flux transport model for the evolution of magnetic flux patterns on the Sun’s surface. Our underlying motivation is to understand the model’s prediction of the polar field (or axial dipole) strength at the end of the …
View article: Spherical winding and helicity
Spherical winding and helicity Open
In ideal magnetohydrodynamics, magnetic helicity is a conserved dynamical quantity and a topological invariant closely related to Gauss linking numbers. However, for open magnetic fields with non-zero boundary components, the latter geomet…
View article: Surface Flux Transport on the Sun
Surface Flux Transport on the Sun Open
We review the surface flux transport model for the evolution of magnetic flux patterns on the Sun's surface. Our underlying motivation is to understand the model's prediction of the polar field (or axial dipole) strength at the end of the …
View article: Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms
Comparing the Performance of a Solar Wind Model from the Sun to 1 au Using Real and Synthetic Magnetograms Open
The input of the solar wind models plays a significant role in accurate solar wind predictions at 1 au. This work introduces a synthetic magnetogram produced from a dynamo model as an input for magnetohydrodynamics simulations. We perform …
View article: Application of historic datasets to understanding open solar flux and the 20th-century grand solar maximum. 2. Solar observations
Application of historic datasets to understanding open solar flux and the 20th-century grand solar maximum. 2. Solar observations Open
We study historic observations of solar activity from the 20th-century rise towards the peak of the Modern Grand Solar Maximum (MGSM) and compare with observations of the decline that has occurred since. The major difference in available s…
View article: Comparing the Performance of a Solar Wind model from the Sun to 1 AU using Real and Synthetic Magnetograms
Comparing the Performance of a Solar Wind model from the Sun to 1 AU using Real and Synthetic Magnetograms Open
The input of the Solar wind models plays a significant role in accurate solar wind predictions at 1 AU. This work introduces a synthetic magnetogram produced from a dynamo model as an input for Magnetohydrodynamics (MHD) simulations. We pe…
View article: Automated Driving for Global Nonpotential Simulations of the Solar Corona
Automated Driving for Global Nonpotential Simulations of the Solar Corona Open
We describe a new automated technique for active region emergence in coronal magnetic field models, based on the inversion of the electric field locally from a single line-of-sight magnetogram for each region. The technique preserves the a…
View article: Eruptivity Criteria for Two-Dimensional Magnetic Flux Ropes in the Solar Corona
Eruptivity Criteria for Two-Dimensional Magnetic Flux Ropes in the Solar Corona Open
We apply the magneto-frictional approach to investigate which quantity or quantities can best predict the loss of equilibrium of a translationally-invariant magnetic flux rope. The flux rope is produced self-consistently by flux cancellati…
View article: Eruptivity Criteria for Two-dimensional Magnetic Flux Ropes in the Solar Corona
Eruptivity Criteria for Two-dimensional Magnetic Flux Ropes in the Solar Corona Open
We apply the magneto-frictional approach to investigate which quantity or quantities can best predict the loss of equilibrium of a translationally-invariant magnetic flux rope. The flux rope is produced self-consistently by flux cancellati…
View article: Exploring the Origin of Stealth Coronal Mass Ejections with Magnetofrictional Simulations
Exploring the Origin of Stealth Coronal Mass Ejections with Magnetofrictional Simulations Open
Coronal mass ejections (CMEs) – among the most energetic events originating from the Sun – can cause significant and sudden disruption to the magnetic and particulate environment of the heliosphere. Thus, in the current era of space-based …
View article: On the limitations of magneto-frictional relaxation
On the limitations of magneto-frictional relaxation Open
The magneto-frictional method is used in solar physics to compute both static and quasi-static models of the
\nSun’s coronal magnetic field. Here, we examine how accurately magneto-friction (without fluid pressure) is
\nable to predict the…
View article: Global Coronal Equilibria with Solar Wind Outflow
Global Coronal Equilibria with Solar Wind Outflow Open
Given a known radial magnetic field distribution on the Sun’s photospheric surface, there exist well-established methods for computing a potential magnetic field in the corona above. Such potential fields are routinely used as input to sol…