7,940 research outputs found
MHD mode conversion in a stratified atmosphere
Mode conversion in the region where the sound and Alfven speeds are equal is
a complex process, which has been studied both analytically and numerically,
and has been seen in observations. In order to further the understanding of
this process we set up a simple, one-dimensional model, and examine wave
propagation through this system using a combination of analytical and numerical
techniques. Simulations are carried out in a gravitationally stratified
atmosphere with a uniform, vertical magnetic field for both isothermal and
non-isothermal cases. For the non-isothermal case a temperature profile is
chosen to mimic the steep temperature gradient encountered at the transition
region. In all simulations, a slow wave is driven on the upper boundary, thus
propagating down from low-beta to high-beta plasma across the mode-conversion
region. In addition, a detailed analytical study is carried out where we
predict the amplitude and phase of the transmitted and converted components of
the incident wave as it passes through the mode-conversion region. A comparison
of these analytical predictions with the numerical results shows good
agreement, giving us confidence in both techniques. This knowledge may be used
to help determine wave types observed and give insight into which modes may be
involved in coronal heating.Comment: 7 pages, 5 figure
MHD Mode Conversion around a 2D Magnetic Null Point
Mode conversion occurs when a wave passes through a region where the sound
and Alfven speeds are equal. At this point there is a resonance, which allows
some of the incident wave to be converted into a different mode. We study this
phenomenon in the vicinity of a two-dimensional, coronal null point. As a wave
approaches the null it passes from low- to high-beta plasma, allowing
conversion to take place. We simulate this numerically by sending in a slow
magnetoacoustic wave from the upper boundary; as this passes through the
conversion layer a fast wave can clearly be seen propagating ahead. Numerical
simulations combined with an analytical WKB investigation allow us to determine
and track both the incident and converted waves throughout the domain.Comment: 4 pages, 2 figure
Arkansas Cotton Variety Test 2008
The primary goal of the Arkansas Cotton Variety Test is to provide unbiased data regarding the agronomic performance of cotton varieties and advanced breeding lines in the major cotton-growing areas of Arkansas. This information helps seed companies establish marketing strategies and assists producers in choosing varieties to plant
Arkansas Cotton Variety Test 2007
The primary goal of the Arkansas Cotton Variety Test is to provide unbiased data regarding the agronomic performance of cotton varieties and advanced breeding lines in the major cotton-growing areas of Arkansas. This information helps seed companies establish marketing strategies and assists producers in choosing varieties to plant
Sunspot rotation. I. A consequence of flux emergence
Context. Solar eruptions and high flare activity often accompany the rapid
rotation of sunspots. The study of sunspot rotation and the mechanisms driving
this motion are therefore key to our understanding of how the solar atmosphere
attains the conditions necessary for large energy release.
Aims. We aim to demonstrate and investigate the rotation of sunspots in a 3D
numerical experiment of the emergence of a magnetic flux tube as it rises
through the solar interior and emerges into the atmosphere. Furthermore, we
seek to show that the sub-photospheric twist stored in the interior is injected
into the solar atmosphere by means of a definitive rotation of the sunspots.
Methods. A numerical experiment is performed to solve the 3D resistive
magnetohydrodynamic (MHD) equations using a Lagrangian-Remap code. We track the
emergence of a toroidal flux tube as it rises through the solar interior and
emerges into the atmosphere investigating various quantities related to both
the magnetic field and plasma.
Results. Through detailed analysis of the numerical experiment, we find clear
evidence that the photospheric footprints or sunspots of the flux tube undergo
a rotation. Significant vertical vortical motions are found to develop within
the two polarity sources after the field emerges. These rotational motions are
found to leave the interior portion of the field untwisted and twist up the
atmospheric portion of the field. This is shown by our analysis of the relative
magnetic helicity as a significant portion of the interior helicity is
transported to the atmosphere. In addition, there is a substantial transport of
magnetic energy to the atmosphere. Rotation angles are also calculated by
tracing selected fieldlines; the fieldlines threading through the sunspot are
found to rotate through angles of up to 353 degrees over the course of the
experiment
Conditional evolution in single-atom cavity QED
We consider a typical setup of cavity QED consisting of a two-level atom
interacting strongly with a single resonant electromagnetic field mode inside a
cavity. The cavity is resonantly driven and the output undergoes continuous
homodyne measurements. We derive an explicit expression for the state of the
system conditional on a discrete photocount record. This expression takes a
particularly simple form if the system is initially in the steady state. As a
byproduct, we derive a general formula for the steady state that had been
conjectured before in the strong driving limit.Comment: 15 pages, 1 postscript figure, added discussion of mode
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