4,956 research outputs found
Pion's valence-quark GPD and its extension beyond DGLAP region
We briefly report on a recent computation, with the help of a fruitful
algebraic model, sketching the pion valence dressed-quark generalized parton
distribution and, very preliminary, discuss on a possible avenue to get
reliable results in both Dokshitzer-Gribov-Lipatov-Altarelli-Parisi (DGLAP) and
Efremov-Radyushkin-Brodsky-Lepage (ERBL) kinematial regions.Comment: 6 pages, 4 figures, contribution to 21st International conference on
Few-Body Problem
A brief comment on the similarities of the IR solutions for the ghost propagator DSE in Landau and Coulomb gauges
This brief note is devoted to reconcile the conclusions from a recent
analysis of the IR solutions for the ghost propagator Dyson-Schwinger equations
in Coulomb gauge with previous studies in Landau gauge.Comment: 4 pages, 1 figur
AuNx stabilization with interstitial nitrogen atoms: A Density Functional Theory Study
Researchers have been studying 4d and 5d Series Transition Metal Nitrides lately as a result of the experimental production of AuN, PtN, CuN. In this paper, we used the Density Functional Theory (DFT) implementing a pseudopotential plane-wave method to study the incorporation of nitrogen atoms in the face-centered cube (fcc) lattice of gold (Au). First, we took the fcc structure of gold, and gradually located the nitrogen atoms in tetrahedral (TH) and octahedral (OH) interstitial sites. AuN stabilized in: 2OH (30%), 4OH and 4TH (50%), 4OH - 2TH (close to the wurtzite structure) and 6TH (60%). This leads us to think that AuN behaves like a Transition Metal Nitride since the nitrogen atoms look for tetrahedral sites. © Published under licence by IOP Publishing Ltd
Temporal relation between quiet-Sun transverse fields and the strong flows detected by IMaX/SUNRISE
Localized strongly Doppler-shifted Stokes V signals were detected by
IMaX/SUNRISE. These signals are related to newly emerged magnetic loops that
are observed as linear polarization features. We aim to set constraints on the
physical nature and causes of these highly Doppler-shifted signals. In
particular, the temporal relation between the appearance of transverse fields
and the strong Doppler shifts is analyzed in some detail. We calculated the
time difference between the appearance of the strong flows and the linear
polarization. We also obtained the distances from the center of various
features to the nearest neutral lines and whether they overlap or not. These
distances were compared with those obtained from randomly distributed points on
observed magnetograms. Various cases of strong flows are described in some
detail. The linear polarization signals precede the appearance of the strong
flows by on average 84+-11 seconds. The strongly Doppler-shifted signals are
closer (0.19") to magnetic neutral lines than randomly distributed points
(0.5"). Eighty percent of the strongly Doppler-shifted signals are close to a
neutral line that is located between the emerging field and pre-existing
fields. That the remaining 20% do not show a close-by pre-existing field could
be explained by a lack of sensitivity or an unfavorable geometry of the
pre-existing field, for instance, a canopy-like structure. Transverse fields
occurred before the observation of the strong Doppler shifts. The process is
most naturally explained as the emergence of a granular-scale loop that first
gives rise to the linear polarization signals, interacts with pre-existing
fields (generating new neutral line configurations), and produces the observed
strong flows. This explanation is indicative of frequent small-scale
reconnection events in the quiet Sun.Comment: 11 pages, 8 figure
Quintessential Kination and Thermal Production of SUSY e-WIMPs
The impact of a kination-dominated phase generated by a quintessential
exponential model on the thermal abundance of Supersymmetric (SUSY) extremely
Weekly Interacting Massive Particles (e-WIMPs) is investigated. For values of
the quintessential energy-density parameter on the eve of nucleosynthesis close
to its upper bound, we find that: (i) the gravitino constraint is totally
evaded for unstable gravitinos; (ii) the thermal abundance of stable gravitinos
is not sufficient to account for the cold dark matter of the universe; (iii)
the thermal abundance of axinos can satisfy the cold dark matter constraint for
values of the initial (``reheating'') temperature well above those required in
the standard cosmology.Comment: To appear in the proceedings of 4th International Workshop On The
Dark Side Of The Universe (DSU 2008) 1-5 Jun 2008, Cairo, Egyp
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