36,124 research outputs found
Atmospheric turbulence and superstatistics
Nonequilibrium systems with large-scale fluctuations of a suitable system
parameter are often effectively described by a superposition of two statistics,
a superstatistics. Here we illustrate this concept by analysing experimental
data of fluctuations in atmospheric wind velocity differences at Florence
airport.Comment: 9 pages, 4 figures. New version to appear in Europhysics News (2005
High-shock FM transmitter Final report, phase I
Electronic component testing of high-shock FM TRANSMITTER
Can Long-Range Nuclear Properties Be Influenced By Short Range Interactions? A chiral dynamics estimate
Recent experiments and many-body calculations indicate that approximately
20\% of the nucleons in medium and heavy nuclei () are part of
short-range correlated (SRC) primarily neutron-proton () pairs. We find
that using chiral dynamics to account for the formation of pairs due to
the effects of iterated and irreducible two-pion exchange leads to values
consistent with the 20\% level. We further apply chiral dynamics to study how
these correlations influence the calculations of nuclear charge radii, that
traditionally truncate their effect, to find that they are capable of
introducing non-negligible effects.Comment: 6 pages, 0 figures. This version includes many improvement
The Local Radio-IR Relation in M51
We observed M51 at three frequencies, 1.4 GHz (20 cm), 4.9 GHz (6 cm), and 8.4 GHz (3.6 cm), with the Very Large Array and the Effelsberg 100 m telescope to obtain the highest quality radio continuum images of a nearby spiral galaxy. These radio data were combined with deconvolved Spitzer IRAC 8 μm and MIPS 24 μm images to search for and investigate local changes in the radio-IR correlation. Utilizing wavelet decomposition, we compare the distribution of the radio and IR emission on spatial scales between 200 pc and 30 kpc. We show that the radio-IR correlation is not uniform across the galactic disk. It presents a complex behavior with local extrema corresponding to various galactic structures, such as complexes of H II regions, spiral arms, and interarm filaments, indicating that the contribution of the thermal and non-thermal radio emission is a strong function of environment. In particular, the relation of the 24 μm and 20 cm emission presents a linear relation within the spiral arms and globally over the galaxy, while it deviates from linearity in the interarm and outer regions as well in the inner region, with two different behaviors: it is sublinear in the interarm and outer region and overlinear in the central 3.5 kpc. Our analysis suggests that the changes in the radio/IR correlation reflect variations of interstellar medium properties between spiral arms and interarm region. The good correlation in the spiral arms implies that 24 μm and 20 cm are tracing recent star formation, while a change in the dust opacity, "Cirrus" contribution to the IR emission and/or the relation between the magnetic field strength and the gas density can explain the different relations found in the interarm, outer, and inner regions
Money in monetary policy design: monetary cross-checking in the New-Keynesian model
In the New-Keynesian model, optimal interest rate policy under uncertainty is formulated without reference to monetary aggregates as long as certain standard assumptions on the distributions of unobservables are satisfied. The model has been criticized for failing to explain common trends in money growth and inflation, and that therefore money should be used as a cross-check in policy formulation (see Lucas (2007)). We show that the New-Keynesian model can explain such trends if one allows for the possibility of persistent central bank misperceptions. Such misperceptions motivate the search for policies that include additional robustness checks. In earlier work, we proposed an interest rate rule that is near-optimal in normal times but includes a cross-check with monetary information. In case of unusual monetary trends, interest rates are adjusted. In this paper, we show in detail how to derive the appropriate magnitude of the interest rate adjustment following a significant cross-check with monetary information, when the New-Keynesian model is the central bank’s preferred model. The cross-check is shown to be effective in offsetting persistent deviations of inflation due to central bank misperceptions. Keywords: Monetary Policy, New-Keynesian Model, Money, Quantity Theory, European Central Bank, Policy Under Uncertaint
Tsallis' q index and Mori's q phase transitions at edge of chaos
We uncover the basis for the validity of the Tsallis statistics at the onset
of chaos in logistic maps. The dynamics within the critical attractor is found
to consist of an infinite family of Mori's -phase transitions of rapidly
decreasing strength, each associated to a discontinuity in Feigenbaum's
trajectory scaling function . The value of at each transition
corresponds to the same special value for the entropic index , such that the
resultant sets of -Lyapunov coefficients are equal to the Tsallis rates of
entropy evolution.Comment: Significantly enlarged version, additional figures and references. To
be published in Physical Review
Formation of a penumbra in a decaying sunspot
Context : Penumbrae are an important characteristic of sunspots, whose
formation is intricately related to the nature of sub-photospheric magnetic
fields. Aims : We study the formation of a penumbra in a decaying sunspot and
compare its properties with those seen during the development of a proto-spot.
Methods : High-resolution spectropolarimetric observations of active region
NOAA 11283 were obtained from the spectro-polarimeter on board Hinode. These
were complemented with full-disk filtergrams of continuum intensity,
line-of-sight magnetograms, and dopplergrams from the Helioseismic and Magnetic
Imager at high cadence. Results : The formation of a penumbra in the decaying
sunspot occurs after the coalescence of the sunspot with a magnetic
fragment/pore, which initially formed in the quiet Sun close to an emerging
flux region. At first, a smaller set of penumbral filaments develop near the
location of the merger with very bright penumbral grains with intensities of
1.2 I_QS, upflows of 4 km/s, and a lifetime of 10 hr. During the decay of these
filaments, a larger segment of a penumbra forms at the location of the
coalescence. These new filaments are characterized by nearly supersonic
downflows of 6.5 km/s that change to a regular Evershed flow nearly 3 hr later.
Conclusions : The coalescence of the pore with the decaying sunspot provided
sufficient magnetic flux for the penumbra to form in the sunspot. The emerging
flux region could have played a decisive role in this process because the
formation occurred at the location of the merger and not on the opposite side
of the sunspot.Comment: Accepted for publication in A&A Letters, 6 pages, 4 figure
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