206 research outputs found
Multi-thermal dynamics and energetics of a coronal mass ejection in the low solar atmosphere
The aim of this work is to determine the multi-thermal characteristics and
plasma energetics of an eruptive plasmoid and occulted flare observed by Solar
Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA). We study an event
from 03-Nov-2010 (peaking at 12:20UT in GOES soft X-rays) of a coronal mass
ejection and occulted flare which demonstrates the morphology of a classic
erupting flux rope. The high spatial, and time resolution, and six coronal
channels, of the SDO/AIA images allows the dynamics of the multi-thermal
emission during the initial phases of eruption to be studied in detail. The
Differential Emission Measure (DEM) is calculated, using an optimised version
of a regularized inversion method (Hannah & Kontar 2012), for each pixel across
the six channels at different times, resulting in emission measure maps and
movies in a variety of temperature ranges. We find that the core of the
erupting plasmoid is hot (8-11, 11-14MK) with a similarly hot filamentary
"stem" structure connecting it to the lower atmosphere, which could be
interpreted as the current sheet in the flux rope model, though is wider than
these models suggest. The velocity of the leading edge of the eruption is
597-664 km s in the temperature range 3-4MK and between 1029-1246
km s for 2-3MK. We estimate the density (in 11-14 MK) of the
erupting core and stem during the impulsive phase to be about
cm, cm, cm in the plasmoid
core, stem and surrounding envelope of material. This gives thermal energy
estimates of erg, erg and
erg. The kinetic energy for the core and envelope is slightly smaller. The
thermal energy of the core and current sheet grows during the eruption,
suggesting continuous influx of energy presumably via reconnection.Comment: Submitted to A&A: in revisio
Solar Physics with the Square Kilometre Array
The Square Kilometre Array (SKA) will be the largest radio telescope ever
built, aiming to provide collecting area larger than 1 km. The SKA will
have two independent instruments, SKA-LOW comprising of dipoles organized as
aperture arrays in Australia and SKA-MID comprising of dishes in South Africa.
Currently the phase-1 of SKA, referred to as SKA1, is in its late design stage
and construction is expected to start in 2020. Both SKA1-LOW (frequency range
of 50-350 MHz) and SKA1-MID Bands 1, 2, and 5 (frequency ranges of 350-1050,
950-1760, and 4600-15300 MHz, respectively) are important for solar
observations. In this paper we present SKA's unique capabilities in terms of
spatial, spectral, and temporal resolution, as well as sensitivity and show
that they have the potential to provide major new insights in solar physics
topics of capital importance including (i) the structure and evolution of the
solar corona, (ii) coronal heating, (iii) solar flare dynamics including
particle acceleration and transport, (iv) the dynamics and structure of coronal
mass ejections, and (v) the solar aspects of space weather. Observations of the
Sun jointly with the new generation of ground-based and space-borne instruments
promise unprecedented discoveries.Comment: Accepted for publication in Advances in Space Researc
LOFAR observations of fine spectral structure dynamics in type IIIb radio bursts
Solar radio emission features a large number of fine structures demonstrating
great variability in frequency and time. We present spatially resolved spectral
radio observations of type IIIb bursts in the MHz range made by the Low
Frequency Array (LOFAR). The bursts show well-defined fine frequency
structuring called "stria" bursts. The spatial characteristics of the stria
sources are determined by the propagation effects of radio waves; their
movement and expansion speeds are in the range of 0.1-0.6c. Analysis of the
dynamic spectra reveals that both the spectral bandwidth and the frequency
drift rate of the striae increase with an increase of their central frequency;
the striae bandwidths are in the range of ~20-100 kHz and the striae drift
rates vary from zero to ~0.3 MHz s^-1. The observed spectral characteristics of
the stria bursts are consistent with the model involving modulation of the type
III burst emission mechanism by small-amplitude fluctuations of the plasma
density along the electron beam path. We estimate that the relative amplitude
of the density fluctuations is of dn/n~10^-3, their characteristic length scale
is less than 1000 km, and the characteristic propagation speed is in the range
of 400-800 km/s. These parameters indicate that the observed fine spectral
structures could be produced by propagating magnetohydrodynamic waves
Hard X-ray footpoint sizes and positions as diagnostics of flare accelerated energetic electrons in the low solar atmosphere
The hard X-ray (HXR) emission in solar flares comes almost exclusively from a
very small part of the flaring region, the footpoints of magnetic loops. Using
RHESSI observations of solar flare footpoints, we determine the radial
positions and sizes of footpoints as a function of energy in six near-limb
events to investigate the transport of flare accelerated electrons and the
properties of the chromosphere. HXR visibility forward fitting allows to find
the positions/heights and the sizes of HXR footpoints along and perpendicular
to the magnetic field of the flaring loop at different energies in the HXR
range. We show that in half of the analyzed events, a clear trend of decreasing
height of the sources with energy is found. Assuming collisional thick-target
transport, HXR sources are located between 600 and 1200 km above the
photosphere for photon energies between 120 and 25 keV respectively. In the
other events, the position as a function of energy is constant within the
uncertainties. The vertical sizes (along the path of electron propagation)
range from 1.3 to 8 arcseconds which is up to a factor 4 larger than predicted
by the thick-target model even in events where the positions/heights of HXR
sources are consistent with the collisional thick-target model. Magnetic
mirroring, collisional pitch angle scattering and X-ray albedo are discussed as
potential explanations of the findings.Comment: 10 pages, 8 figures, accepted for publication in Ap
The influence of albedo on the size of hard X-ray flare sources
Context: Hard X-rays from solar flares are an important diagnostic of
particle acceleration and transport in the solar atmosphere. Any observed X-ray
flux from on-disc sources is composed of direct emission plus Compton
backscattered photons (albedo). This affects both the observed spectra and
images as well as the physical quantities derived from them such as the spatial
and spectral distributions of accelerated electrons or characteristics of the
solar atmosphere. Aims: We propose a new indirect method to measure albedo and
to infer the directivity of X-rays in imaging using RHESSI data. Methods:
Visibility forward fitting is used to determine the size of a disc event
observed by RHESSI as a function of energy. This is compared to the sizes of
simulated sources from a Monte Carlo simulation code of photon transport in the
chromosphere for different degrees of downward directivity and true source
sizes to find limits on the true source size and the directivity. Results: The
observed full width half maximum of the source varies in size between 7.4
arcsec and 9.1 arcsec with the maximum between 30 and 40 keV. Such behaviour is
expected in the presence of albedo and is found in the simulations. A source
size smaller than 6 arcsec is improbable for modest directivities and the true
source size is likely to be around 7 arcsec for small directivities.
Conclusions: While it is difficult to image the albedo patch directly, the
effect of backscattered photons on the observed source size can be estimated.
The increase in source size caused by albedo has to be accounted for when
computing physical quantities that include the size as a parameter such as
flare energetics. At the same time, the study of the albedo signature provides
vital information about the directivity of X-rays and related electrons.Comment: 8 pages, 6 figures, A&A (accepted
Dynamics of electron beams in the solar corona plasma with density fluctuations
The problem of beam propagation in a plasma with small scale and low intensity inhomogeneities is investigated. It is shown that the electron beam propagates in a plasma as a beam-plasma structure and is a source of Langmuir waves. The plasma inhomogeneity changes the spatial distribution of the waves. The spatial distribution of the waves is fully determined by the distribution of plasma inhomogeneities. The possible applications to the theory of radio emission associated with electron beams are discussed
Turbulent pitch-angle scattering and diffusive transport of hard-X-ray producing electrons in flaring coronal loops
Recent observations from {\em RHESSI} have revealed that the number of
non-thermal electrons in the coronal part of a flaring loop can exceed the
number of electrons required to explain the hard X-ray-emitting footpoints of
the same flaring loop. Such sources cannot, therefore, be interpreted on the
basis of the standard collisional transport model, in which electrons stream
along the loop while losing their energy through collisions with the ambient
plasma; additional physical processes, to either trap or scatter the energetic
electrons, are required. Motivated by this and other observations that suggest
that high energy electrons are confined to the coronal region of the source, we
consider turbulent pitch angle scattering of fast electrons off low frequency
magnetic fluctuations as a confinement mechanism, modeled as a spatial
diffusion parallel to the mean magnetic field. In general, turbulent scattering
leads to a reduction of the collisional stopping distance of non-thermal
electrons along the loop and hence to an enhancement of the coronal HXR source
relative to the footpoints. The variation of source size with electron
energy becomes weaker than the quadratic behavior pertinent to collisional
transport, with the slope of depending directly on the mean free path
again pitch angle scattering. Comparing the predictions of the model
with observations, we find that cm for
keV, less than the length of a typical flaring loop and smaller than, or
comparable to, the size of the electron acceleration region.Comment: 25 pages, 5 figures, accepted for publication in Astrophysical
Journa
Regularized energy-dependent solar flare hard x-ray spectral index
The deduction from solar flare X-ray photon spectroscopic data of the energy
dependent model-independent spectral index is considered as an inverse problem.
Using the well developed regularization approach we analyze the energy
dependency of spectral index for a high resolution energy spectrum provided by
Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The regularization
technique produces much smoother derivatives while avoiding additional errors
typical of finite differences. It is shown that observations imply a spectral
index varying significantly with energy, in a way that also varies with time as
the flare progresses. The implications of these findings are discussed in the
solar flare context.Comment: 13 pages; 5 figures, Solar Physics in pres
Combined STEREO/RHESSI study of CME acceleration and particle acceleration in solar flares
Using the potential of two unprecedented missions, STEREO and RHESSI, we
study three well observed fast CMEs that occurred close to the limb together
with their associated high energy flare emissions in terms of RHESSI HXR
spectra and flux evolution. From STEREO/EUVI and STEREO/COR1 data the full CME
kinematics of the impulsive acceleration phase up to 4 Rs is measured with a
high time cadence of less equal 2.5 min. For deriving CME velocity and
acceleration we apply and test a new algorithm based on regularization methods.
The CME maximum acceleration is achieved at heights h < 0.4 Rs, the peak
velocity at h < 2.1 Rs (in one case as small as 0.5 Rs). We find that the CME
acceleration profile and the flare energy release as evidenced in the RHESSI
hard X-ray flux evolve in a synchronized manner. These results support the
standard flare/CME model which is characterized by a feed-back relationship
between the large-scale CME acceleration process and the energy release in the
associated flare.Comment: accepted for Ap
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