6 research outputs found
Extreme Spatial Dispersion in Nonlocally-Resonant Elastic Metamaterials
To date, the vast majority of architected materials have leveraged two
physical principles to control wave behavior, namely Bragg interference and
local resonances. Here, we describe a third path: structures that accommodate a
finite number of delocalized zero-energy modes, leading to anomalous dispersion
cones that nucleate from extreme spatial dispersion at 0 Hz. We explain how to
design such zero-energy modes in the context of elasticity and show that many
of the landmark wave properties of metamaterials can also be induced at an
extremely subwavelength scale by the associated anomalous cones, without
suffering from the same bandwidth limitations. We then validate our theory
through a combination of simulations and experiments. Finally, we present an
inverse design method to produce anomalous cones at desired locations in
momentum space
The Alfv\'enic nature of chromospheric swirls
We investigate the evolution and origin of small-scale chromospheric swirls
by analyzing numerical simulations of the quiet solar atmosphere, using the
radiative magnetohydrodynamic code COBOLD. We are interested in finding
their relation with magnetic field perturbations and in the processes driving
their evolution. For the analysis, the swirling strength criterion and its
evolution equation are applied in order to identify vortical motions and to
study their dynamics. We introduce a new criterion, the magnetic swirling
strength, which allows us to recognize torsional perturbations in the magnetic
field. We find a strong correlation between swirling strength and magnetic
swirling strength, in particular in intense magnetic flux concentrations, which
suggests a tight relation between vortical motions and torsional magnetic field
perturbations. Furthermore, we find that swirls propagate upward with the local
Alfv\'en speed as unidirectional swirls, in the form of pulses, driven by
magnetic tension forces alone. In the photosphere and low chromosphere, the
rotation of the plasma co-occurs with a twist in the upwardly directed magnetic
field that is in the opposite direction of the plasma flow. All together, these
are characteristics of torsional Alfv\'en waves. We also find indications of an
imbalance between the hydrodynamic and magnetohydrodynamic baroclinic effects
being at the origin of the swirls. At the base of the chromosphere, we find a
net upwardly directed Poynting flux, which is mostly associated with large and
complex swirling structures that we interpret as the superposition of various
small-scale vortices. We conclude that the ubiquitous swirling events observed
in simulations are tightly correlated with perturbations of the magnetic field.
At photospheric and chromospheric levels, they form Alfv\'en pulses that
propagate upward and may contribute to chromospheric heating.Comment: 23 pages, 18 figures, 1 movie, ready for the production stage in A&
The Alfvénic nature of chromospheric swirls
Context. Observations show that small-scale vortical plasma motions are ubiquitous in the quiet solar atmosphere. They have received increasing attention in recent years because they are a viable candidate mechanism for the heating of the outer solar atmospheric layers. However, the true nature and the origin of these swirls, and their effective role in the energy transport, are still unclear.
Aims. We investigate the evolution and origin of chromospheric swirls by analyzing numerical simulations of the quiet solar atmosphere. In particular, we are interested in finding their relation with magnetic field perturbations and in the processes driving their evolution.
Methods. The radiative magnetohydrodynamic code CO5BOLD is used to perform realistic numerical simulations of a small portion of the solar atmosphere, ranging from the top layers of the convection zone to the middle chromosphere. For the analysis, the swirling strength criterion and its evolution equation are applied in order to identify vortical motions and to study their dynamics. As a new criterion, we introduce the magnetic swirling strength, which allows us to recognize torsional perturbations in the magnetic field.
Results. We find a strong correlation between swirling strength and magnetic swirling strength, in particular in intense magnetic flux concentrations, which suggests a tight relation between vortical motions and torsional magnetic field perturbations. Furthermore, we find that swirls propagate upward with the local Alfvén speed as unidirectional swirls driven by magnetic tension forces alone. In the photosphere and low chromosphere, the rotation of the plasma co-occurs with a twist in the upwardly directed magnetic field that is in the opposite direction of the plasma flow. All together, these are clear characteristics of torsional Alfvén waves. Yet, the Alfvén wave is not oscillatory but takes the form of a unidirectional pulse. The novelty of the present work is that these Alfvén pulses naturally emerge from realistic numerical simulations of the solar atmosphere. We also find indications of an imbalance between the hydrodynamic and magnetohydrodynamic baroclinic effects being at the origin of the swirls. At the base of the chromosphere, we find a mean net upwardly directed Poynting flux of 12.8 ± 6.5 kW m, which is mainly due to swirling motions. This energy flux is mostly associated with large and complex swirling structures, which we interpret as the superposition of various small-scale vortices.
Conclusions. We conclude that the ubiquitous swirling events observed in numerical simulations are tightly correlated with perturbations of the magnetic field. At photospheric and chromospheric levels, they form Alfvén pulses that propagate upward and may contribute to chromospheric heating
The Alfvénic nature of chromospheric swirls
Context. Observations show that small-scale vortical plasma motions are ubiquitous in the quiet solar atmosphere. They have received increasing attention in recent years because they are a viable candidate mechanism for the heating of the outer solar atmospheric layers. However, the true nature and the origin of these swirls, and their effective role in the energy transport, are still unclear.
Aims. We investigate the evolution and origin of chromospheric swirls by analyzing numerical simulations of the quiet solar atmosphere. In particular, we are interested in finding their relation with magnetic field perturbations and in the processes driving their evolution.
Methods. The radiative magnetohydrodynamic code CO5BOLD is used to perform realistic numerical simulations of a small portion of the solar atmosphere, ranging from the top layers of the convection zone to the middle chromosphere. For the analysis, the swirling strength criterion and its evolution equation are applied in order to identify vortical motions and to study their dynamics. As a new criterion, we introduce the magnetic swirling strength, which allows us to recognize torsional perturbations in the magnetic field.
Results. We find a strong correlation between swirling strength and magnetic swirling strength, in particular in intense magnetic flux concentrations, which suggests a tight relation between vortical motions and torsional magnetic field perturbations. Furthermore, we find that swirls propagate upward with the local Alfvén speed as unidirectional swirls driven by magnetic tension forces alone. In the photosphere and low chromosphere, the rotation of the plasma co-occurs with a twist in the upwardly directed magnetic field that is in the opposite direction of the plasma flow. All together, these are clear characteristics of torsional Alfvén waves. Yet, the Alfvén wave is not oscillatory but takes the form of a unidirectional pulse. The novelty of the present work is that these Alfvén pulses naturally emerge from realistic numerical simulations of the solar atmosphere. We also find indications of an imbalance between the hydrodynamic and magnetohydrodynamic baroclinic effects being at the origin of the swirls. At the base of the chromosphere, we find a mean net upwardly directed Poynting flux of 12.8 ± 6.5 kW m−2, which is mainly due to swirling motions. This energy flux is mostly associated with large and complex swirling structures, which we interpret as the superposition of various small-scale vortices.
Conclusions. We conclude that the ubiquitous swirling events observed in numerical simulations are tightly correlated with perturbations of the magnetic field. At photospheric and chromospheric levels, they form Alfvén pulses that propagate upward and may contribute to chromospheric heating