5,035 research outputs found
DNA repair nucleases
Stability of DNA largely depends on accuracy of repair mechanisms, which remove structural anomalies induced by exogenous and endogenous agents or introduced by DNA metabolism, such as replication. Most repair mechanisms include nucleolytic processing of DNA, where nucleases cleave a phosphodiester bond between a deoxyribose and a phosphate residue, thereby producing 5′-terminal phosphate and 3′-terminal hydroxyl groups. Exonucleases hydrolyse nucleotides from either the 5′ or 3′ end of DNA, while endonucleases incise internal sites of DNA. Flap endonucleases cleave DNA flap structures at or near the junction between single-stranded and double-stranded regions. DNA nucleases play a crucial role in mismatch repair, nucleotide excision repair, base excision repair and double-strand break repair. In addition, nucleolytic repair functions are required during replication to remove misincorporated nucleotides, Okazaki fragments and 3′ tails that may be formed after repair of stalled replication fork
Detection of 3-Minute Oscillations in Full-Disk Ly Emission During A Solar Flare
In this Letter we report the detection of chromospheric 3-minute oscillations
in disk-integrated EUV irradiance observations during a solar flare. A wavelet
analysis of detrended Lyman-alpha (from GOES/EUVS) and Lyman continuum (from
SDO/EVE) emission from the 2011 February 15 X-class flare (SOL2011-02-15T01:56)
revealed a 3-minute period present during the flare's main phase. The
formation temperature of this emission locates this radiation to the flare's
chromospheric footpoints, and similar behaviour is found in the SDO/AIA
1600\AA\ and 1700\AA\ channels, which are dominated by chromospheric continuum.
The implication is that the chromosphere responds dynamically at its acoustic
cutoff frequency to an impulsive injection of energy. Since the 3-minute period
was not found at hard X-ray energies (50-100 keV) in RHESSI data we can state
that this 3-minute oscillation does not depend on the rate of energization of
non-thermal electrons. However, a second period of 120 s found in both hard
X-ray and chromospheric emission is consistent with episodic electron
energization on 2-minute timescales. Our finding on the 3-minute oscillation
suggests that chromospheric mechanical energy should be included in the flare
energy budget, and the fluctuations in the Lyman-alpha line may influence the
composition and dynamics of planetary atmospheres during periods of high
activity.Comment: 6 pages, 5 figures. Accepted for publication in Astrophysics Journal
Letter
Canonical Quantization of the Maxwell-Chern-Simons Theory in the Coulomb Gauge
The Maxwell-Chern-Simons theory is canonically quantized in the Coulomb gauge
by using the Dirac bracket quantization procedure. The determination of the
Coulomb gauge polarization vector turns out to be intrincate. A set of quantum
Poincar\'e densities obeying the Dirac-Schwinger algebra, and, therefore, free
of anomalies, is constructed. The peculiar analytical structure of the
polarization vector is shown to be at the root for the existence of spin of the
massive gauge quanta.The Coulomb gauge Feynman rules are used to compute the
M\"oller scattering amplitude in the lowest order of perturbation theory. The
result coincides with that obtained by using covariant Feynman rules. This
proof of equivalence is, afterwards, extended to all orders of perturbation
theory. The so called infrared safe photon propagator emerges as an effective
propagator which allows for replacing all the terms in the interaction
Hamiltonian of the Coulomb gauge by the standard field-current minimal
interaction Hamiltonian.Comment: 21 pages, typeset in REVTEX, figures not include
Ground-state phase diagram of the spin-1/2 square-lattice J1-J2 model with plaquette structure
Using the coupled cluster method for high orders of approximation and Lanczos
exact diagonalization we study the ground-state phase diagram of a quantum
spin-1/2 J1-J2 model on the square lattice with plaquette structure. We
consider antiferromagnetic (J1>0) as well as ferromagnetic (J1<0)
nearest-neighbor interactions together with frustrating antiferromagnetic
next-nearest-neighbor interaction J2>0. The strength of inter-plaquette
interaction lambda varies between lambda=1 (that corresponds to the uniform
J1-J2 model) and lambda=0 (that corresponds to isolated frustrated 4-spin
plaquettes). While on the classical level (s \to \infty) both versions of
models (i.e., with ferro- and antiferromagnetic J1) exhibit the same
ground-state behavior, the ground-state phase diagram differs basically for the
quantum case s=1/2. For the antiferromagnetic case (J1 > 0) Neel
antiferromagnetic long-range order at small J2/J1 and lambda \gtrsim 0.47 as
well as collinear striped antiferromagnetic long-range order at large J2/J1 and
lambda \gtrsim 0.30 appear which correspond to their classical counterparts.
Both semi-classical magnetic phases are separated by a nonmagnetic quantum
paramagnetic phase. The parameter region, where this nonmagnetic phase exists,
increases with decreasing of lambda. For the ferromagnetic case (J1 < 0) we
have the trivial ferromagnetic ground state at small J2/|J1|. By increasing of
J2 this classical phase gives way for a semi-classical plaquette phase, where
the plaquette block spins of length s=2 are antiferromagnetically long-range
ordered. Further increasing of J2 then yields collinear striped
antiferromagnetic long-range order for lambda \gtrsim 0.38, but a nonmagnetic
quantum paramagnetic phase lambda \lesssim 0.38.Comment: 10 pages, 15 figure
Acoustic-gravity wave propagation characteristics in 3D radiation hydrodynamic simulations of the solar atmosphere
There has been tremendous progress in the degree of realism of
three-dimensional radiation magneto-hydrodynamic simulations of the solar
atmosphere in the past decades. Four of the most frequently used numerical
codes are Bifrost, CO5BOLD, MANCHA3D, and MURaM. Here we test and compare the
wave propagation characteristics in model runs from these four codes by
measuring the dispersion relation of acoustic-gravity waves at various heights.
We find considerable differences between the various models. The height
dependence of wave power, in particular of high-frequency waves, varies by up
to two orders of magnitude between the models, and the phase difference spectra
of several models show unexpected features, including phase
jumps.Comment: 19 pages, 15 figure
Asymmetric Silver to Oxide Adhesion in Multilayers Deposited on Glass by Sputtering
We have developed a wedge-loaded double-cantilever beam adhesion measurement
set-up for thin films deposited on glass by sputtering. The test is described
in details. Results on the Glass/sublayer/Ag/ZnO multilayer provide evidence
that \SnOd or \TiOd perform better than ZnO as a sublayer. Then however,
rupture within the multilayer shifts to the upper Ag/ZnO interface. The latter
is shown to be tougher than the lower ZnO/Ag interface, an asymmetry due to
non-equilibrium interfacial structures
Weaning calves’ response to a medicated top dressing
Adding a medicated top dressing to a weaning calf ration did not reduce calf sickness, but increased weight gains the second and third weeks of a three-week weaning trial
The Position of High Frequency Waves with Respect to the Granulation Pattern
High frequency velocity oscillations were observed in the spectral lines Fe I
543.45nm and 543.29nm, using 2D spectroscopy with a Fabry- Perot and speckle
reconstruction, at the VTT in Tenerife. We investigate the radial component of
waves with frequencies in the range 8 - 22mHz in the internetwork, network and
a pore. We find that the occurrence of waves do not show any preference on
location and are equally distributed over down-flows and up-flows, regardless
of the activity of the observed area in the line of Fe I 543.45nm. The waves
observed in the lower formed line of Fe I 543.29nm seem to appear
preferentially over down-flows.Comment: Article has 12 pages and 7 images. It is accepted in Solar Physics
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