2,136 research outputs found
QCD Corrections to Electroweak Vector Boson Scattering at Small Scattering Angles
We investigate the role of a certain class of QCD corrections to electroweak
vector boson scattering at small scattering angles and large energies. These
are present since, from the perturbative analysis, the vector bosons may
dissociate into quark-antiquark pairs giving rise to colour dipoles interacting
through gluon exchanges. After the computation of the vector boson impact
factors, we present expressions for the lowest order QCD scattering amplitude
and for the leading logarithmic BFKL amplitude. Particularly we discuss
numerical results for the process . The QCD corrections to
the cross section resulting from the interference with the electroweak ones are
estimated and compared with the leading pure electroweak part. Corrections
resulting from the leading log BFKL amplitude are of the order of few percent
already at the TeV energy range.Comment: 21 pages,9 figures, discussion on the helicity-flip impact factors
added, typos correcte
Discovery of a ~7 Hz Quasi-Periodic Oscillation in the low-luminosity low-mass X-ray binary 4U 1820-30
We have discovered a 7.06+-0.08 Hz quasi-periodic oscillation (QPO) in the
X-ray flux of the low-luminosity low-mass X-ray binary (LMXB) and atoll source
4U 1820-30. This QPO was only observable at the highest observed mass accretion
rate, when the source was in the uppermost part of the banana branch, at a 2-25
keV luminosity of 5.4x10^37 erg/s (for a distance of 6.4 kpc). The QPO had a
FWHM of only 0.5+-0.2 Hz during small time intervals (32-s of data), and showed
erratic shifts in the centroid frequency between 5.5 and 8 Hz. The rms
amplitude over the energy range 2-60 keV was 5.6%+-0.2%. The amplitude
increased with photon energy from 3.7%+-0.5% between 2.8 and 5.3 keV to
7.3%+-0.6% between 6.8 and 9.3 keV, above which it remained approximately
constant at ~7%. The time lag of the QPO between 2.8-6.8 and 6.8-18.2 keV was
consistent with being zero (-1.2+-3.4 ms).
The properties of the QPO (i.e., its frequency and its presence only at the
highest observed mass accretion rate) are similar to those of the 5-20 Hz QPO
observed in the highest luminosity LMXBs (the Z sources) when they are
accreting near the Eddington mass accretion limit. If this is indeed the same
phenomenon, then models explaining the 5-20 Hz QPO in the Z sources, which
require the near-Eddington accretion rates, will not hold. Assuming isotropic
emission, the 2-25 keV luminosity of 4U 1820-30 at the time of the 7 Hz QPOs is
at maximum only 40% (for a companion star with cosmic abundances), but most
likely ~20% (for a helium companion star) of the Eddington accretion limit.Comment: Accepted for publication in ApJ Letters (6 pages, including 3
figures
Type 2 Diabetes Mellitus and COVID-19: A Narrative Review
The pandemic of coronavirus disease (COVID-19), caused by severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2), has involved more than one hundred million individuals, including more than two million deaths. Diabetes represents one of the most prevalent chronic conditions worldwide and significantly increases the risk of hospitalization and death in COVID-19 patients. In this review, we discuss the prevalence, the pathophysiological mechanisms, and the outcomes of COVID-19 infection in people with diabetes. We propose a rationale for using drugs prescribed in patients with diabetes and some pragmatic clinical recommendations to deal with COVID-19 in this kind of patient
Suprathermal particle addition to solar wind pressure: possible influence on magnetospheric transmissivity of low energy cosmic rays?
Energetic (suprathermal) solar particles, accelerated in the interplanetary
medium, contribute to the solar wind pressure, in particular during high solar
activity periods. We estimated the effect of the increase of solar wind
pressure due to suprathermal particles on magnetospheric transmissivity of
galactic cosmic rays in the case of one recent solar event
Comment on Mie Scattering from a Sonoluminescing Bubble with High Spatial and Temporal Resolution [Physical Review E 61, 5253 (2000)]
A key parameter underlying the existence of sonoluminescence (SL)is the time
relative to SL at which acoustic energy is radiated from the collapsed bubble.
Light scattering is one route to this quantity. We disagree with the statement
of Gompf and Pecha that -highly compressed water causes the minimum in
scattered light to occur 700ps before SL- and that this effect leads to an
overestimate of the bubble wall velocity. We discuss potential artifacts in
their experimental arrangement and correct their description of previous
experiments on Mie scattering.Comment: 10 pages, 2 figure
SOFIA/EXES Observations of Water Absorption in the Protostar AFGL 2591 at High Spectral Resolution
We present high spectral resolution (~3 km/s) observations of the nu_2
ro-vibrational band of H2O in the 6.086--6.135 micron range toward the massive
protostar AFGL 2591 using the Echelon-Cross-Echelle Spectrograph (EXES) on the
Stratospheric Observatory for Infrared Astronomy (SOFIA). Ten absorption
features are detected in total, with seven caused by transitions in the nu_2
band of H2O, two by transitions in the first vibrationally excited nu_2 band of
H2O, and one by a transition in the nu_2 band of H2{18}O. Among the detected
transitions is the nu_2 1(1,1)--0(0,0) line which probes the lowest lying
rotational level of para-H2O. The stronger transitions appear to be optically
thick, but reach maximum absorption at a depth of about 25%, suggesting that
the background source is only partially covered by the absorbing gas, or that
the absorption arises within the 6 micron emitting photosphere. Assuming a
covering fraction of 25%, the H2O column density and rotational temperature
that best fit the observed absorption lines are N(H2O)=(1.3+-0.3)*10^{19}
cm^{-2} and T=640+-80 K.Comment: 6 pages, 3 figures, 1 table, accepted for publication in ApJ
Mass and radius estimation for the neutron star in X-ray burster 4U 1820-30
We present a new method for determining masses and radii of neutron stars
residing in thermo-nuclear X-ray burst sources. To illustrate this method we
apply it to a burst from the source 4U 1820-30 recorded by the Rossi X-Ray
Timing Explorer. Fits of the observed X-ray spectra to grids of Comptonised
model atmospheres yield estimates for the mass and radius of the neutron star,
M=1.3 \pm 0.6 M_sol and R=11^+3_-2 km, respectively.Comment: MNRAS in prin
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