2,778 research outputs found
Thermal Diagnostics with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions
We present a new method for performing differential emission measure (DEM)
inversions on narrow-band EUV images from the Atmospheric Imaging Assembly
(AIA) onboard the Solar Dynamics Observatory (SDO). The method yields positive
definite DEM solutions by solving a linear program. This method has been
validated against a diverse set of thermal models of varying complexity and
realism. These include (1) idealized gaussian DEM distributions, (2) 3D models
of NOAA Active Region 11158 comprising quasi-steady loop atmospheres in a
non-linear force-free field, and (3) thermodynamic models from a
fully-compressible, 3D MHD simulation of AR corona formation following magnetic
flux emergence. We then present results from the application of the method to
AIA observations of Active Region 11158, comparing the region's thermal
structure on two successive solar rotations. Additionally, we show how the DEM
inversion method can be adapted to simultaneously invert AIA and XRT data, and
how supplementing AIA data with the latter improves the inversion result. The
speed of the method allows for routine production of DEM maps, thus
facilitating science studies that require tracking of the thermal structure of
the solar corona in time and space.Comment: 21 pages, 18 figures, accepted for publication in Ap
Data-Driven Radiative Magnetohydrodynamics Simulations with the MURaM code
We present a method of conducting data-driven simulations of solar active
regions and flux emergence with the MURaM radiative magnetohydrodynamics (MHD)
code. The horizontal electric field derived from the full velocity and magnetic
vectors, is implemented at the photospheric (bottom) boundary to drive the
induction equation. The energy equation accounts for thermal conduction along
magnetic fields, optically-thin radiative loss, and heating of coronal plasma
by viscous and resistive dissipation, which allows for a realistic presentation
of the thermodynamic properties of coronal plasma that are key to predicting
the observational features of solar active regions and eruptions. To validate
the method, the photospheric data from a comprehensive radiative MHD simulation
of solar eruption (the ground truth) are used to drive a series of numerical
experiments. The data-driven simulation reproduces the accumulation of free
magnetic energy over the course of flux emergence in the ground truth with an
error of 3\%. The onset time is approximately 8\,min delayed compared to the
ground truth. However, a precursor-like signature can be identified at the
correct onset time. The data-driven simulation captures key eruption-related
emission features and plasma dynamics of the ground truth flare over a wide
temperature span from to . The evolution of
the flare and coronal mass ejection as seen in synthetic extreme ultraviolet
images is also reproduced with high fidelity. The method helps to understand
the evolution of magnetic field in a more realistic coronal environment and to
link the magnetic structures to observable diagnostics.Comment: 35 pages, 24 figures, accepted for publication in Ap
Magnetohydrodynamics of the Weakly Ionized Solar Photosphere
We investigate the importance of ambipolar diffusion and Hall currents for
high-resolution comprehensive ('realistic') photospheric simulations. To do so
we extended the radiative magnetohydrodynamics code \emph{MURaM} to use the
generalized Ohm's law under the assumption of local thermodynamic equilibrium.
We present test cases comparing analytical solutions with numerical simulations
for validation of the code. Furthermore, we carried out a number of numerical
experiments to investigate the impact of these neutral-ion effects in the
photosphere. We find that, at the spatial resolutions currently used (5-20 km
per grid point), the Hall currents and ambipolar diffusion begin to become
significant -- with flows of 100 m/s in sunspot light bridges, and changes of a
few percent in the thermodynamic structure of quiet-Sun magnetic features. The
magnitude of the effects is expected to increase rapidly as smaller-scale
variations are resolved by the simulations.Comment: accepted Ap
Polarimetry and the High-Energy Emission Mechanisms in Quasar Jets. The Case of PKS 1136-135
Since the discovery of kiloparsec-scale X-ray emission from quasar jets, the
physical processes responsible for their high-energy emission have been poorly
defined. A number of mechanisms are under active debate, including synchrotron
radiation, inverse-Comptonized CMB (IC/CMB) emission, and other Comptonization
processes. In a number of cases, the optical and X-ray emission of jet regions
are inked by a single spectral component, and in those, high- resolution
multi-band imaging and polarimetry can be combined to yield a powerful
diagnostic of jet emission processes. Here we report on deep imaging photometry
of the jet of PKS 1136135 obtained with the {\it Hubble Space Telescope.} We
find that several knots are highly polarized in the optical, with fractional
polarization . When combined with the broadband spectral shape
observed in these regions, this is very difficult to explain via IC/CMB models,
unless the scattering particles are at the lowest-energy tip of the electron
energy distribution, with Lorentz factor , and the jet is also
very highly beamed () and viewed within a few degrees of the
line of sight. We discuss both the IC/CMB and synchrotron interpretation of the
X-ray emission in the light of this new evidence, presenting new models of the
spectral energy distribution and also the matter content of this jet. The high
polarizations do not completely rule out the possibility of IC/CMB
optical-to-X-ray emission in this jet, but they do strongly disfavor the model.
We discuss the implications of this finding, and also the prospects for future
work.Comment: 14 pages, 8 figures, ApJ in pres
The theory of international business: the role of economic models
This paper reviews the scope for economic modelling in international business studies. It argues for multi-level theory based on classic internalisation theory. It present a systems approach that encompasses both firm-level and industry-level analysis
Implications of Different Solar Photospheric Flux-Transport Models for Global Coronal and Heliospheric Modeling
The concept of surface-flux transport (SFT) is commonly used in evolving
models of the large-scale solar surface magnetic field. These photospheric
models are used to determine the large-scale structure of the overlying coronal
magnetic field, as well as to make predictions about the fields and flows that
structure the solar wind. We compare predictions from two SFT models for the
solar wind, open magnetic field footpoints, and the presence of coronal
magnetic null points throughout various phases of a solar activity cycle,
focusing on the months of April in even-numbered years between 2012 and 2020,
inclusive. We find that there is a solar cycle dependence to each of the
metrics considered, but there is not a single phase of the cycle in which all
the metrics indicate good agreement between the models. The metrics also reveal
large, transient differences between the models when a new active region is
rotating into the assimilation window. The evolution of the surface flux is
governed by a combination of large scale flows and comparatively small scale
motions associated with convection. Because the latter flows evolve rapidly,
there are intervals during which their impact on the surface flux can only be
characterized in a statistical sense, thus their impact is modeled by
introducing a random evolution that reproduces the typical surface flux
evolution. We find that the differences between the predicted properties are
dominated by differences in the model assumptions and implementation, rather
than selection of a particular realization of the random evolution.Comment: Accepted for publication in The Astrophysical Journa
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