20,169 research outputs found
Hard X-ray and UV Observations of the 2005 January 15 Two-ribbon Flare
In this paper, we present comprehensive analysis of a two-ribbon flare
observed in UV 1600{\AA} by Transition Region and Coronal Explorer and in HXRs
by Reuven Ramaty High Energy Solar Spectroscopic Imager. HXR (25-100 keV)
imaging observations show two kernels of size (FWHM) 15?? moving along the two
UV ribbons. We find the following results. (1) UV brightening is substantially
enhanced wherever and whenever the compact HXR kernel is passing, and during
the HXR transit across a certain region, the UV count light curve in that
region is temporally correlated with the HXR total flux light curve. After the
passage of the HXR kernel, the UV light curve exhibits smooth monotonical
decay. (2)We measure the apparent motion speed of the HXR sources and UV ribbon
fronts, and decompose the motion into parallel and perpendicular motions with
respect to the magnetic polarity inversion line (PIL). It is found that HXR
kernels and UV fronts exhibit similar apparent motion patterns and speeds. The
parallel motion dominates during the rise of the HXR emission, and the
perpendicular motion starts and dominates at the HXR peak, the apparent motion
speed being 10-40 km s-1. (3) We also find that UV emission is characterized by
a rapid rise correlated with HXRs, followed by a long decay on timescales of
15-30 minutes. The above analysis provides evidence that UV brightening is
primarily caused by beam heating, which also produces thick-target HXR
emission. The thermal origin of UV emission cannot be excluded, but would
produce weaker heating by one order of magnitude. The extended UV ribbons in
this event are most likely a result of sequential reconnection along the PIL,
which produces individual flux tubes (post-flare loops), subsequent non-thermal
energy release and heating in these flux tubes, and then the very long cooling
time of the transition region at the feet of these flux tubes.Comment: 8 figure
Vortex melting and decoupling transitions in YBaCuO single crystals
The vortex correlation along the c-axis in high quality single crystals of
YBaCuO has been investigated as a function of temperature T
in different magnetic fields, using the quasi-flux transformer configuration. A
simultaneous sharp drop associated with the vortex lattice melting is observed
in both the primary and secondary voltages(V and V). Just above
the melting temperature, the vortices form three-dimensional line liquid with
the correlation length along the c direction t, the sample
thickness. The temperature where a resistive peak in R develops
corresponds to the decoupling temperature T at which the vortices loose
their correlation along the c-direction and they dissolve into the two
dimensional pancake vortices. The H-T phase diagram for the
YBaCuO single crystal is obtained.Comment: 1 Text file, 3 eps figure
Solar flare hard X-ray spikes observed by RHESSI: a statistical study
Context. Hard X-ray (HXR) spikes refer to fine time structures on timescales
of seconds to milliseconds in high-energy HXR emission profiles during solar
flare eruptions. Aims. We present a preliminary statistical investigation of
temporal and spectral properties of HXR spikes. Methods. Using a three-sigma
spike selection rule, we detected 184 spikes in 94 out of 322 flares with
significant counts at given photon energies, which were detected from
demodulated HXR light curves obtained by the Reuven Ramaty High Energy Solar
Spectroscopic Imager (RHESSI). About one fifth of these spikes are also
detected at photon energies higher than 100 keV. Results. The statistical
properties of the spikes are as follows. (1) HXR spikes are produced in both
impulsive flares and long-duration flares with nearly the same occurrence
rates. Ninety percent of the spikes occur during the rise phase of the flares,
and about 70% occur around the peak times of the flares. (2) The time durations
of the spikes vary from 0.2 to 2 s, with the mean being 1.0 s, which is not
dependent on photon energies. The spikes exhibit symmetric time profiles with
no significant difference between rise and decay times. (3) Among the most
energetic spikes, nearly all of them have harder count spectra than their
underlying slow-varying components. There is also a weak indication that spikes
exhibiting time lags in high-energy emissions tend to have harder spectra than
spikes with time lags in low-energy emissions.Comment: 16 pages, 13 figure
Chromospheric Evaporation in an X1.0 Flare on 2014 March 29 Observed with IRIS and EIS
Chromospheric evaporation refers to dynamic mass motions in flare loops as a
result of rapid energy deposition in the chromosphere. These have been observed
as blueshifts in X-ray and extreme-ultraviolet (EUV) spectral lines
corresponding to upward motions at a few tens to a few hundreds of km/s. Past
spectroscopic observations have also revealed a dominant stationary component,
in addition to the blueshifted component, in emission lines formed at high
temperatures (~10 MK). This is contradictory to evaporation models predicting
predominant blueshifts in hot lines. The recently launched Interface Region
Imaging Spectrograph (IRIS) provides high resolution imaging and spectroscopic
observations that focus on the chromosphere and transition region in the UV
passband. Using the new IRIS observations, combined with coordinated
observations from the EUV Imaging Spectrometer, we study the chromospheric
evaporation process from the upper chromosphere to corona during an X1.0 flare
on 2014 March 29. We find evident evaporation signatures, characterized by
Doppler shifts and line broadening, at two flare ribbons separating from each
other, suggesting that chromospheric evaporation takes place in successively
formed flaring loops throughout the flare. More importantly, we detect dominant
blueshifts in the high temperature Fe XXI line (~10 MK), in agreement with
theoretical predictions. We also find that, in this flare, gentle evaporation
occurs at some locations in the rise phase of the flare, while explosive
evaporation is detected at some other locations near the peak of the flare.
There is a conversion from gentle to explosive evaporation as the flare
evolves.Comment: ApJ in pres
Solar flare hard X-ray spikes observed by RHESSI: a case study
In this paper, we analyze hard X-ray spikes observed by RHESSI to understand
their temporal, spectral, and spatial properties. A recently developed
demodulation code was applied to hard X-ray light curves in several energy
bands observed by RHESSI. Hard X-ray spikes were selected from the demodulated
flare light curves. We measured the spike duration, the energy-dependent time
delay, and count spectral index of these spikes. We also located the hard X-ray
source emitting these spikes from RHESSI mapping that was coordinated with
imaging observations in visible and UV wavelengths. We identify quickly varying
structures of <1 s during the rise of hard X-rays in five flares. These hard
X-ray spikes can be observed at photon energies over 100 keV. They exhibit
sharp rise and decay with a duration (FWHM) of less than 1 s. Energy-dependent
time lags are present in some spikes. It is seen that the spikes exhibit harder
spectra than underlying components, typically by 0.5 in the spectral index when
they are fitted to power-law distributions. RHESSI clean maps at 25-100 keV
with an integration of 2 s centered on the peak of the spikes suggest that hard
X-ray spikes are primarily emitted by double foot-point sources in magnetic
fields of opposite polarities. With the RHESSI mapping resolution of ~ 4 arsec,
the hard X-ray spike maps do not exhibit detectable difference in the spatial
structure from sources emitting underlying components. Coordinated
high-resolution imaging UV and infrared observations confirm that hard X-ray
spikes are produced in magnetic structures embedded in the same magnetic
environment of the underlying components. The coordinated high-cadence TRACE UV
observations of one event possibly reveal new structures on spatial scales <1-2
arsec at the time of the spike superposed on the underlying component. They are
probably sources of hard X-ray spikes.Comment: 20 pages, 11 figure
Work Function of Single-wall Silicon Carbide Nanotube
Using first-principles calculations, we study the work function of single
wall silicon carbide nanotube (SiCNT). The work function is found to be highly
dependent on the tube chirality and diameter. It increases with decreasing the
tube diameter. The work function of zigzag SiCNT is always larger than that of
armchair SiCNT. We reveal that the difference between the work function of
zigzag and armchair SiCNT comes from their different intrinsic electronic
structures, for which the singly degenerate energy band above the Fermi level
of zigzag SiCNT is specifically responsible. Our finding offers potential
usages of SiCNT in field-emission devices.Comment: 3 pages, 3 figure
A compact active sound absorption system compensating near-field effect of the secondary source
© 2017 Institute of Noise Control Engineering. In a compact active sound absorption system where the error sensor is close to the secondary source, the near-field effect of the secondary source deteriorates the system performance severely. This study proposes an improved method by employing an auxiliary calibration process, in which an extra sensor is utilized to obtain relevant impulse responses, and then these impulse responses are used in the control process to eliminate the influence of the near-field effect. Experiments are carried out in a compact active sound absorption system in a duct to demonstrate the feasibility of the proposed method
Increasing the performance of active noise control systems on ground with two vertical reflecting surfaces with an included angle
© 2019 Acoustical Society of America. This paper investigates the feasibility of increasing the noise reduction performance of active noise control (ANC) systems on ground by introducing two vertical reflecting surfaces with an included angle. By using the image source method, the theory of sound wave propagation in a wedge-shaped reflector and the integral equation method, the noise reduction of the ANC systems with two infinitely large or finite size reflecting surfaces with different included angles are studied. It is demonstrated that the noise reduction of the system can be increased significantly with two reflecting surfaces after optimizing their included angle and size. The simple empirical formulas for the optimal included angle of the surfaces and the noise reduction are presented. It is found that the noise reduction at 500 Hz increases by 13.6 dB when two vertical reflecting surfaces are arranged with an optimal angle of 125° and the source distance is 0.1 m. By optimizing the size of the reflecting surfaces to about 0.35 of the wavelength, the noise reduction can be further increased by approximately 2.8 dB. The mechanisms for the performance improvement are disclosed, and the experiments are conducted to validate the results
Resummation of nuclear enhanced higher twist in the Drell Yan process
We investigate higher twist contributions to the transverse momentum
broadening of Drell Yan pairs in proton nucleus collisions. We revisit the
contribution of matrix elements of twist-4 and generalize this to matrix
elements of arbitrary twist. An estimate of the maximal nuclear broadening
effect is derived. A model for nuclear enhanced matrix elements of arbitrary
twist allows us to give the result of a resummation of all twists in closed
form. Subleading corrections to the maximal broadening are discussed
qualitatively.Comment: 10 pages, 5 figures; v2: minor changes in text, acknowledgement
added; v3: mistake in fig. 1 correcte
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