879 research outputs found
Deceleration and Dispersion of Large-scale Coronal Bright Fronts
One of the most dramatic manifestations of solar activity are large-scale
coronal bright fronts (CBFs) observed in extreme ultraviolet (EUV) images of
the solar atmosphere. To date, the energetics and kinematics of CBFs remain
poorly understood, due to the low image cadence and sensitivity of previous EUV
imagers and the limited methods used to extract the features. In this paper,
the trajectory and morphology of CBFs was determined in order to investigate
the varying properties of a sample of CBFs, including their kinematics and
pulse shape, dispersion, and dissipation. We have developed a semi-automatic
intensity profiling technique to extract the morphology and accurate positions
of CBFs in 2.5-10 min cadence images from STEREO/EUVI. The technique was
applied to sequences of 171A and 195A images from STEREO/EUVI in order to
measure the wave properties of four separate CBF events. Following launch at
velocities of ~240-450kms^{-1} each of the four events studied showed
significant negative acceleration ranging from ~ -290 to -60ms^{-2}. The CBF
spatial and temporal widths were found to increase from ~50 Mm to ~200 Mm and
~100 s to ~1500 s respectively, suggesting that they are dispersive in nature.
The variation in position-angle averaged pulse-integrated intensity with
propagation shows no clear trend across the four events studied. These results
are most consistent with CBFs being dispersive magnetoacoustic waves.Comment: 15 pages, 18 figure
On-line PCA with Optimal Regrets
We carefully investigate the on-line version of PCA, where in each trial a
learning algorithm plays a k-dimensional subspace, and suffers the compression
loss on the next instance when projected into the chosen subspace. In this
setting, we analyze two popular on-line algorithms, Gradient Descent (GD) and
Exponentiated Gradient (EG). We show that both algorithms are essentially
optimal in the worst-case. This comes as a surprise, since EG is known to
perform sub-optimally when the instances are sparse. This different behavior of
EG for PCA is mainly related to the non-negativity of the loss in this case,
which makes the PCA setting qualitatively different from other settings studied
in the literature. Furthermore, we show that when considering regret bounds as
function of a loss budget, EG remains optimal and strictly outperforms GD.
Next, we study the extension of the PCA setting, in which the Nature is allowed
to play with dense instances, which are positive matrices with bounded largest
eigenvalue. Again we can show that EG is optimal and strictly better than GD in
this setting
High cadence observations of a global coronal wave by EUVI/STEREO
We report a large-scale coronal wave (so-called "EIT wave") observed with
high cadence by EUVI onboard STEREO in association with the GOES B9.5 flare and
double CME event on 19 May 2007. The EUVI instruments provide us with the
unprecedented opportunity to study the {\it dynamics} of flare/CME associated
coronal waves imaged in the extreme ultraviolet. The coronal wave under study
reveals deceleration, indicative of a freely propagating MHD wave.
Complementary analysis of the associated flare and erupting filament/CME hint
at wave initiation by the CME expanding flanks, which drive the wave only over
a limited distance. The associated flare is very weak and occurs too late to
account for the wave initiation.Comment: Astrophysical Journal Letters (in press
Coronal Shock Waves, EUV waves, and their Relation to CMEs. II. Modeling MHD Shock Wave Propagation Along the Solar Surface, Using Nonlinear Geometrical Acoustics
We model the propagation of a coronal shock wave, using nonlinear geometrical
acoustics. The method is based on the Wentzel-Kramers-Brillouin (WKB) approach
and takes into account the main properties of nonlinear waves: i) dependence of
the wave front velocity on the wave amplitude, ii) nonlinear dissipation of the
wave energy, and iii) progressive increase in the duration of solitary shock
waves. We address the method in detail and present results of the modeling of
the propagation of shock-associated extreme-ultraviolet (EUV) waves as well as
Moreton waves along the solar surface in the simplest solar corona model. The
calculations reveal deceleration and lengthening of the waves. In contrast,
waves considered in the linear approximation keep their length unchanged and
slightly accelerate.Comment: 15 pages, 7 figures, accepted for publication in Solar Physic
Plasma heating in the very early and decay phases of solar flares
In this paper we analyze the energy budgets of two single-loop solar flares
under the assumption that non-thermal electrons are the only source of plasma
heating during all phases of both events. The flares were observed by the
Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and Geostationary
Operational Environmental Satellite (GOES) on September 20, 2002 and March 17,
2002, respectively. For both investigated flares we derived the energy fluxes
contained in non-thermal electron beams from the RHESSI observational data
constrained by observed GOES light-curves. We showed that energy delivered by
non-thermal electrons was fully sufficient to fulfil the energy budgets of the
plasma during the pre-heating and impulsive phases of both flares as well as
during the decay phase of one of them. We concluded that in the case of the
investigated flares there was no need to use any additional ad-hoc heating
mechanisms other than heating by non-thermal electrons.Comment: 22 pages, 10 figures, The Astrophysical Journal (accepted, March
2011
Electron spin coherence in metallofullerenes: Y, Sc and La@C82
Endohedral fullerenes encapsulating a spin-active atom or ion within a carbon
cage offer a route to self-assembled arrays such as spin chains. In the case of
metallofullerenes the charge transfer between the atom and the fullerene cage
has been thought to limit the electron spin phase coherence time (T2) to the
order of a few microseconds. We study electron spin relaxation in several
species of metallofullerene as a function of temperature and solvent
environment, yielding a maximum T2 in deuterated o-terphenyl greater than 200
microseconds for Y, Sc and La@C82. The mechanisms governing relaxation (T1, T2)
arise from metal-cage vibrational modes, spin-orbit coupling and the nuclear
spin environment. The T2 times are over 2 orders of magnitude longer than
previously reported and consequently make metallofullerenes of interest in
areas such as spin-labelling, spintronics and quantum computing.Comment: 5 pages, 4 figure
Spectroscopic analysis of interaction between an EIT wave and a coronal upflow region
We report a spectroscopic analysis of an EIT wave event that occurred in
active region 11081 on 2010 June 12 and was associated with an M2.0 class
flare. The wave propagated near circularly. The south-eastern part of the wave
front passed over an upflow region nearby a magnetic bipole. Using EIS raster
observations for this region, we studied the properties of plasma dynamics in
the wave front, as well as the interaction between the wave and the upflow
region. We found a weak blueshift for the Fe XII {\lambda}195.12 and Fe XIII
{\lambda}202.04 lines in the wave front. The local velocity along the solar
surface, which is deduced from the line of sight velocity in the wave front and
the projection effect, is much lower than the typical propagation speed of the
wave. A more interesting finding is that the upflow and non-thermal velocities
in the upflow region are suddenly diminished after the transit of the wave
front. This implies a significant change of magnetic field orientation when the
wave passed. As the lines in the upflow region are redirected, the velocity
along the line of sight is diminished as a result. We suggest that this
scenario is more in accordance with what was proposed in the field-line
stretching model of EIT waves.Comment: 13 pages, 7 figures, accepted for publication in Ap
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