119,369 research outputs found
Switching speed distribution of spin-torque-induced magnetic reversal
The switching probability of a single-domain ferromagnet under spin-current
excitation is evaluated using the Fokker-Planck equation(FPE). In the case of
uniaxial anisotropy, the FPE reduces to an ordinary differential equation in
which the lowest eigenvalue determines the slowest switching
events. We have calculated by using both analytical and numerical
methods. It is found that the previous model based on thermally distributed
initial magnetization states \cite{Sun1} can be accurately justified in some
useful limiting conditions.Comment: The 10th Joint MMM/Intermag, HA-0
Effects of current on vortex and transverse domain walls
By using the spin torque model in ferromagnets, we compare the response of
vortex and transverse walls to the electrical current. For a defect-free sample
and a small applied current, the steady state wall mobility is independent of
the wall structure. In the presence of defects, the minimum current required to
overcome the wall pinning potential is much smaller for the vortex wall than
for the transverse wall. During the wall motion, the vortex wall tends to
transform to the transverse wall. We construct a phase diagram for the wall
mobility and the wall transformation driven by the current
Searching for radiative pumping lines of OH masers: II. The 53.3um absorption line towards 1612MHz OH maser sources
This paper analyzes the 53.3um line in the ISO LWS spectra towards a similar
sample of OH/IR sources. We find 137 LWS spectra covering 53.3um and associated
with 47 galactic OH/IR sources. Ten of these galactic OH/IR sources are found
to show and another 5 ones tentatively show the 53.3um absorption while another
7 sources highly probably do not show this line. The source class is found to
be correlated with the type of spectral profile: red supergiants (RSGs) and AGB
stars tend to show strong blue-shifted filling emission in their 53.3um
absorption line profiles while HII regions tend to show a weak red-shifted
filling emission in the line profile. GC sources and megamasers do not show
filling emission feature. It is argued that the filling emission might be the
manifestation of an unresolved half emission half absorption profile of the
53.3um doublet. The 53.3 to 34.6um equivalent width (EW) ratio is close to
unity for RSGs but much larger than unity for GC sources and megamasers while H
II regions only show the 53.3um line. The pump rate defined as maser to IR
photon flux ratio is approximately 5% for RSGs. The pump rates of GC sources
are three order of magnitude smaller. Both the large 53.3 to 34.6um EW ratio
and the small pump rate of the GC OH masers reflect that the two detected
`pumping lines' in these sources are actually of interstellar origin. The pump
rate of Arp 220 is 32%--much larger than that of RSGs, which indicates that the
contribution of other pumping mechanisms to this megamaser is important.Comment: 34 pages, 12 figures, 4 table
Koszul differential graded algebras and BGG correspondence
The concept of Koszul differential graded algebra (Koszul DG algebra) is
introduced. Koszul DG algebras exist extensively, and have nice properties
similar to the classic Koszul algebras. A DG version of the Koszul duality is
proved. When the Koszul DG algebra is AS-regular, the Ext-algebra of
is Frobenius. In this case, similar to the classical BGG correspondence,
there is an equivalence between the stable category of finitely generated left
-modules, and the quotient triangulated category of the full triangulated
subcategory of the derived category of right DG -modules consisting of all
compact DG modules modulo the full triangulated subcategory consisting of all
the right DG modules with finite dimensional cohomology. The classical BGG
correspondence can derived from the DG version.Comment: 29 page
Solar transition region in the quiet Sun and active regions
The solar transition region (TR), in which above the photosphere the tempera-
ture increases rapidly and the density drops dramatically, is believed to play
an important role in coronal heating and solar wind acceleration. Long-lasting
up-flows are present in the upper TR and interpreted as signatures of mass
supply to large coronal loops in the quiet Sun. Coronal bright points (BPs) are
local heating phenomena and we found a different Doppler-shift pattern at TR
and coronal temperatures in one BP, which might be related to the twisted loop
system. The dominant energy loss in the lower TR is the Ly-alpha emission. It
has been found that most Ly-alpha radiance profiles are stronger in the blue
peak, an asymmetry opposite to higher order Lyman lines. This asymmetry is
stronger when the downflow in the middle TR is stronger, indicating that the TR
flows play an important role in the line formation process. The peak separation
of Ly-alpha is found to be larger in coronal holes than in the quiet Sun,
reflecting the different magnetic structures and radiation fields between the
two regions. The Lyman line profiles are found to be not reversed in sunspot
plume and umbra regions, while they are obviously reversed in the surrounding
plage region. At TR temperatures, the densities of the sunspot plume and umbra
are a factor of 10 lower than of the plage, indicating that the sunspot plasma
emitting at TR temperatures is higher and possibly more extended above sunspots
than above the plage region.Comment: This paper has been withdrawn by the author because it's not a
referred pape
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