157 research outputs found
Successive merging of plasmoids and fragmentation in flare current sheet and their X-ray and radio signatures
Based on our recent MHD simulations, first, a concept of the successive
merging of plasmoids and fragmentation in the current sheet in the standard
flare model is presented. Then, using a 2.5-D electromagnetic particle-in-cell
model with free boundary conditions, these processes were modelled on the
kinetic level of plasma description. We recognized the plasmoids which mutually
interacted and finally merged into one large plasmoid. Between interacting
plasmoids further plasmoids and current sheets on smaller and smaller spatial
scales were formed in agreement with the fragmentation found in MHD
simulations. During interactions (merging - coalescences) of the plasmoids the
electrons were very efficiently accelerated and heated. We found that after a
series of such merging processes the electrons in some regions reached the
energies relevant for the emission in the hard X-ray range. Considering these
energetic electrons and assuming the plasma density 10^9-10^10 cm^{-3} and the
source volume as in the December 31, 2007 flare (Krucker at al. 2010, ApJ 714,
1108), we computed the X-ray spectra as produced by the bremsstrahlung emission
process. Comparing these spectra with observations, we think that these
processes can explain the observed above-the-loop-top hard X-ray sources.
Furthermore, we show that the process of a fragmentation between two merging
plasmoids can generate the narrowband dm-spikes. Formulas for schematic fractal
reconnection structures were derived. Finally, the results were discussed.Comment: 8 pages, 8 figure
Diagnostics of solar flare reconnection
We present new diagnostics of the solar flare reconnection, mainly based on the plasma radio emission. We propose that the high-frequency (600-2000 MHz) slowly drifting pulsating structures map the flare magnetic field reconnection. These structures correspond to the radio emission from plasmoids which are formed in the extended current sheet due to tearing and coalescence processes. An increase of the frequency drift of the drifting structures is interpreted as an increase of the reconnection rate. Using this model, time scales of slowly drifting pulsating structure observed during the 12 April 2001 flare by the Trieste radiopolarimeter with high time resolution (1 ms) are interpreted as a radio manifestation of electron beams accelerated in the multi-scale reconnection process. For short periods Fourier spectra of the observed structure have a power-law form with power-law indices in the 1.3-1.6 range. For comparison the 2-D MHD numerical modeling of the multi-scale reconnection is made and it is shown that Fourier spectrum of the reconnection dissipation power has also a power-law form, but with power-law index 2. Furthermore, we compute a time evolution of plasma parameters (density, magnetic field etc) in the 2-D MHD model of the reconnection. Then assuming a plasma radio emission from locations, where the 'double-resonance' instability generates the upper-hybrid waves due to unstable distribution function of suprathermal electrons, we model radio spectra. Effects of the MHD turbulence are included. The resulting spectra are compared with those observed. It is found, that depending on model parameters the lace bursts and the decimetric spikes can be reproduced. Thus, it is shown that the model can be used for diagnostics of the flare reconnection process. We also point out possible radio signatures of reconnection outflow termination shocks. They are detected as type II-like herringbone structures in the 200-700 MHz frequency range. Finally, we mention Hα spectra of the 18 September 1995 eruptive prominence which indicate the bi-directional plasma flow as expected in the reconnection process
First analysis of solar structures in 1.21 mm full-disc ALMA image of the Sun
Various solar features can be seen on maps of the Sun in the mm and sub-mm
wavelength range. The recently installed Atacama Large Millimeter/submillimeter
Array (ALMA) is capable of observing the Sun in that wavelength range with an
unprecedented spatial, temporal and spectral resolution. To interpret solar
observations with ALMA the first important step is to compare ALMA maps with
simultaneous images of the Sun recorded in other spectral ranges. First we
identify different structures in the solar atmosphere seen in the optical, IR
and EUV parts of the spectrum (quiet Sun (QS), active regions (AR), prominences
on the disc, magnetic inversion lines (IL), coronal holes (CH) and coronal
bright points (CBPs)) in a full disc solar ALMA image. The second aim is to
measure the intensities (brightness temperatures) of those structures and
compare them with the corresponding QS level. A full disc solar image at 1.21
mm obtained on December 18, 2015 during a CSV-EOC campaign with ALMA is
calibrated and compared with full disc solar images from the same day in
H\alpha, in He I 1083 nm core, and with SDO images (AIA at 170 nm, 30.4 nm,
21.1 nm, 19.3 nm, and 17.1 nm and HMI magnetogram). The brightness temperatures
of various structures are determined by averaging over corresponding regions of
interest in the ALMA image. Positions of the QS, ARs, prominences on the disc,
ILs, CHs and CBPs are identified in the ALMA image. At 1.21 mm ARs appear as
bright areas (but sunspots are dark), while prominences on the disc and CHs are
not discernible from the QS background, although having slightly less intensity
than surrounding QS regions. ILs appear as large, elongated dark structures and
CBPs correspond to ALMA bright points. These results are in general agreement
with sparse earlier measurements at similar wavelengths. The identification of
CBPs represents the most important new result.Comment: 9 pages, 3 figure
Bioactivation versus detoxication of the urothelial carcinogen aristolochic acid I by human cytochrome P450 1A1 and 1A2
Exposure to aristolochic acid (AA) is associated with human nephropathy and urothelial cancer. Individual susceptibility to AA-induced disease likely reflects individual differences in enzymes that metabolize AA. Herein, we evaluated AAI metabolism by human cytochrome P450 (CYP) 1A1 and 1A2 in two CYP1A-humanized mouse lines that carry functional human CYP1A1 and CYP1A2 genes in the absence of the mouse Cyp1a1/1a2 orthologs. Human and mouse hepatic microsomes and human CYPs were also studied. Human CYP1A1 and 1A2 were found to be principally responsible for reductive activation of AAI to form AAI-DNA adducts and for oxidative detoxication to 8-hydroxyaristolochic acid (AAIa), both in the intact mouse and in microsomes. Overall, AAI-DNA adduct levels were higher in CYP1A-humanized mice relative to wild-type mice, indicating that expression of human CYP1A1 and 1A2 in mice leads to higher AAI bioactivation than in mice containing the mouse CYP1A1 and 1A2 orthologs. Furthermore, an exclusive role of human CYP1A1 and 1A2 in AAI oxidation to AAIa was observed in human liver microsomes under the aerobic (i.e., oxidative) conditions. Because CYP1A2 levels in human liver are at least 100-fold greater than those of CYP1A1 and there exists a > 60-fold genetic variation in CYP1A2 levels in human populations, the role of CYP1A2 in AAI metabolism is clinically relevant. The results suggest that, in addition to CYP1A1 and 1A2 expression levels, in vivo oxygen concentration in specific tissues might affect the balance between AAI nitroreduction and demethylation, which in turn would influence tissue-specific toxicity or carcinogenicity
Multiwavelength Observations of Supersonic Plasma Blob Triggered by Reconnection Generated Velocity Pulse in AR10808
Using multi-wavelength observations of Solar and Heliospheric Observatory
(SoHO)/Michelson Doppler Imager (MDI), Transition Region and Coronal Explorer
(TRACE) 171 \AA, and H from Culgoora Solar Observatory at Narrabri,
Australia, we present a unique observational signature of a propagating
supersonic plasma blob before an M6.2 class solar flare in AR10808 on 9th
September 2005. The blob was observed between 05:27 UT to 05:32 UT with almost
a constant shape for the first 2-3 minutes, and thereafter it quickly vanished
in the corona. The observed lower bound speed of the blob is estimated as
215 km s in its dynamical phase. The evidence of the blob with
almost similar shape and velocity concurrent in H and TRACE 171 \AA\
supports its formation by multi-temperature plasma. The energy release by a
recurrent 3-D reconnection process via the separator dome below the magnetic
null point, between the emerging flux and pre-existing field lines in the lower
solar atmosphere, is found to be the driver of a radial velocity pulse outwards
that accelerates this plasma blob in the solar atmosphere. In support of
identification of the possible driver of the observed eruption, we solve the
two-dimensional ideal magnetohydrodynamic equations numerically to simulate the
observed supersonic plasma blob. The numerical modelling closely match the
observed velocity, evolution of multi-temperature plasma, and quick vanishing
of the blob found in the observations. Under typical coronal conditions, such
blobs may also carry an energy flux of 7.0 ergs cm
s to re-balance the coronal losses above active regions.Comment: Solar Physics; 22 Pages; 8 Figure
Reversed Drifting Quasi-periodic Pulsating Structure in an X1.3 Solar Flare on 2005 July 30
Based on the analysis of the microwave observations at frequency of 2.60 --
3.80 GHz in a solar X1.3 flare event observed at Solar Broadband
RadioSpectrometer in Huairou (SBRS/Huairou) on 2005 July 30, an interesting
reversed drifting quasi-periodic pulsating structure (R-DPS) is confirmed. The
R-DPS is mainly composed of two drifting pulsating components: one is a
relatively slow very short-period pulsation (VSP) with period of about 130 --
170 ms, the other is a relatively fast VSP with period of about 70 -- 80 ms.
The R-DPS has a weak left-handed circular polarization. Based on the synthetic
investigations of Reuven Ramaty High Energy Solar Spectroscopic Imaging
(RHESSI) hard X-ray, Geostationary Operational Environmental Satellite (GOES)
soft X-ray observation, and magnetic field extrapolation, we suggest the R-DPS
possibly reflects flaring dynamic processes of the emission source regions
Study of flare energy release using events with numerous type III-like bursts in microwaves
The analysis of narrowband drifting of type III-like structures in radio
bursts dynamic spectra allows to obtain unique information about primary energy
release mechanisms in solar flares. The SSRT spatially resolved images and a
high spectral and temporal resolution allow direct determination not only the
positions of its sources but also the exciter velocities along the flare loop.
Practically, such measurements are possible during some special time intervals
when the SSRT (about 5.7 GHz) is observing the flare region in two high-order
fringes; thus, two 1D scans are recorded simultaneously at two frequency bands.
The analysis of type III-like bursts recorded during the flare 14 Apr 2002 is
presented. Using-muliwavelength radio observations recorded by SSRT, SBRS,
NoRP, RSTN we study an event with series of several tens of drifting microwave
pulses with drift rates in the range from -7 to 13 GHz/s. The sources of the
fast-drifting bursts were located near the top of the flare loop in a volume of
a few Mm in size. The slow drift of the exciters along the flare loop suggests
a high pitch-anisotropy of the emitting electrons.Comment: 16 pages, 6 figures, Solar Physics, in press, 201
Fractal Reconnection in Solar and Stellar Environments
Recent space based observations of the Sun revealed that magnetic
reconnection is ubiquitous in the solar atmosphere, ranging from small scale
reconnection (observed as nanoflares) to large scale one (observed as long
duration flares or giant arcades). Often the magnetic reconnection events are
associated with mass ejections or jets, which seem to be closely related to
multiple plasmoid ejections from fractal current sheet. The bursty radio and
hard X-ray emissions from flares also suggest the fractal reconnection and
associated particle acceleration. We shall discuss recent observations and
theories related to the plasmoid-induced-reconnection and the fractal
reconnection in solar flares, and their implication to reconnection physics and
particle acceleration. Recent findings of many superflares on solar type stars
that has extended the applicability of the fractal reconnection model of solar
flares to much a wider parameter space suitable for stellar flares are also
discussed.Comment: Invited chapter to appear in "Magnetic Reconnection: Concepts and
Applications", Springer-Verlag, W. D. Gonzalez and E. N. Parker, eds. (2016),
33 pages, 18 figure
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