4,785 research outputs found
CO oxidation studies over supported noble metal catalysts and single crystals: A review
The catalytic oxidation of CO over noble metal catalysts is reviewed. Results obtained on supported noble metal catalysts and single crystals both at high pressures and under UHV conditions are compared. The underlying causes which result in surface instabilities and multiple steady-state oscillations are considered, in particular, the occurrence of hot spots. CO islands of reactivity, surface oxide formation and phase transformations under oscillatory conditions are discussed
Simple Baryon-Meson Mass Relations For A Logarithmic Interquark Potential
I consider the quantity delta(m_1m_2m_3) = M_{q_1q_2q_3} - [M_{q_1q_2bar} +
M_{q_2q_3bar} + M_{q_1q_3bar}]/2, where the M's represent the ground state
spin-averaged hadron masses with the indicated quark content and the m's the
corresponding constituent quark masses. I assume a logarithmic interquark
potential, the validity of a nonrelativistic approach, and various standard
potential model inputs. Simple scaling arguments then imply that the quantity
R(x)=delta(mmm_3)/delta(m_0m_0m_0) depends only on the ratio x=m/m_3, and is
independent of m_0 as well as any parameters appearing in the potential. A
simple and accurate analytic determination of delta(mmm_3), and hence R(x), is
given using the 1/D expansion where D is the number of spatial dimensions. When
applicable, this estimate of R(x) compares very well to experiment -- even for
hadrons containing light quarks. A prediction of the above result which is
likely to be tested in the near future is M_{Sigma_b^*}/2 + [M_{Lambda_b} +
M_{Sigma_b}]/4 = 5774 +/- 4 MeV/c^2.Comment: 13 pages, plain TeX, 1 eps figure, uses harvmac and epsf.st
Star formation in the massive cluster merger Abell 2744
We present a comprehensive study of star-forming (SF) galaxies in the HST
Frontier Field recent cluster merger A2744 (z=0.308). Wide-field,
ultraviolet-infrared (UV-IR) imaging enables a direct constraint of the total
star formation rate (SFR) for 53 cluster galaxies, with SFR{UV+IR}=343+/-10
Msun/yr. Within the central 4 arcmin (1.1 Mpc) radius, the integrated SFR is
complete, yielding a total SFR{UV+IR}=201+/-9 Msun/yr. Focussing on obscured
star formation, this core region exhibits a total SFR{IR}=138+/-8 Msun/yr, a
mass-normalised SFR{IR} of Sigma{SFR}=11.2+/-0.7 Msun/yr per 10^14 Msun and a
fraction of IR-detected SF galaxies f{SF}=0.080(+0.010,-0.037). Overall, the
cluster population at z~0.3 exhibits significant intrinsic scatter in IR
properties (total SFR{IR}, Tdust distribution) apparently unrelated to the
dynamical state: A2744 is noticeably different to the merging Bullet cluster,
but similar to several relaxed clusters. However, in A2744 we identify a trail
of SF sources including jellyfish galaxies with substantial unobscured SF due
to extreme stripping (SFR{UV}/SFR{IR} up to 3.3). The orientation of the trail,
and of material stripped from constituent galaxies, indicates that the passing
shock front of the cluster merger was the trigger. Constraints on star
formation from both IR and UV are crucial for understanding galaxy evolution
within the densest environments.Comment: Accepted by MNRAS. 12 pages, 7 figures (high resolution versions of
Figs. 1 & 2 are available in the published PDF
Selection of nonlinear interactions by a forward stepwise algorithm: Application to identifying environmental chemical mixtures affecting health outcomes
Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/149279/1/sim8059_am.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/149279/2/SIM_8059-Supp-0001-InteractionSelection_Supp.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/149279/3/sim8059.pd
Soft Resummation of Quark Anomalous Dimensions and Coefficient Functions in MS-bar Factorization
The asymptotic behaviour at large N of the MS-bar quark anomalous dimensions
is derived to all orders assuming only MS-bar factorization and standard
results for the exponentiation of soft logarithms in the quark initiated bare
cross sections for deep inelastic scattering and Drell-Yan. The result is then
used to write the MS-bar quark coefficient functions in a form in which all
terms of are resummed.Comment: 12 page
The Bullet cluster at its best: weighing stars, gas and dark matter
We present a new strong lensing mass reconstruction of the Bullet cluster (1E
0657-56) at z=0.296, based on WFC3 and ACS HST imaging and VLT/FORS2
spectroscopy. The strong lensing constraints underwent substantial revision
compared to previously published analysis, there are now 14 (six new and eight
previously known) multiply-imaged systems, of which three have
spectroscopically confirmed redshifts (including one newly measured from this
work). The reconstructed mass distribution explicitly included the combination
of three mass components: i) the intra-cluster gas mass derived from X-ray
observation, ii) the cluster galaxies modeled by their fundamental plane
scaling relations and iii) dark matter. The model that includes the
intra-cluster gas is the one with the best Bayesian evidence. This model has a
total RMS value of 0.158" between the predicted and measured image positions
for the 14 multiple images considered. The proximity of the total RMS to
resolution of HST/WFC3 and ACS (0.07-0.15" FWHM) demonstrates the excellent
precision of our mass model. The derived mass model confirms the spatial offset
between the X-ray gas and dark matter peaks. The fraction of the galaxy halos
mass to total mass is found to be f_s=11+/-5% for a total mass of 2.5+/-0.1 x
10^14 solar mass within a 250 kpc radial aperture.Comment: Accepted by A&A 15 pages, 12 figure
The Periodic Standing-Wave Approximation: Overview and Three Dimensional Scalar Models
The periodic standing-wave method for binary inspiral computes the exact
numerical solution for periodic binary motion with standing gravitational
waves, and uses it as an approximation to slow binary inspiral with outgoing
waves. Important features of this method presented here are: (i) the
mathematical nature of the ``mixed'' partial differential equations to be
solved, (ii) the meaning of standing waves in the method, (iii) computational
difficulties, and (iv) the ``effective linearity'' that ultimately justifies
the approximation. The method is applied to three dimensional nonlinear scalar
model problems, and the numerical results are used to demonstrate extraction of
the outgoing solution from the standing-wave solution, and the role of
effective linearity.Comment: 13 pages RevTeX, 5 figures. New version. A revised form of the
nonlinearity produces better result
Spitzer and Hubble Constraints on the Physical Properties of the z~7 Galaxy Strongly Lensed by Abell 2218
We report the detection of a z~7 galaxy strongly lensed by the massive galaxy
cluster Abell 2218 (z=0.175) at 3.6 and 4.5 um using the Spitzer Observatory
and at 1.1 um using the Hubble Space Telescope. The new data indicate a refined
photometric redshift in the range of 6.6-6.8 depending on the presence of
Ly-alpha emission. The spectral energy distribution is consistent with having a
significant Balmer break, suggesting that the galaxy is in the poststarburst
stage with an age of at least ~50 Myr and quite possibly a few hundred Myr.
This suggests the possibility that a mature stellar population is already in
place at such a high redshift. Compared with typical Lyman break galaxies at
z~3-4, the stellar mass is an order of magnitude smaller (~10^{9} Msun), but
the specific star formation rate (star formation rate/M_{star}) is similarly
large (> 10^{-9} yr^{-1}), indicating equally vigorous star-forming activity.Comment: 11 pages, 2 figures, 2 tables; Accepted for publication in ApJ
Rotation and lithium abundance of solar-analog stars. Theoretical analysis of observations
Rotational velocity, lithium abundance, and the mass depth of the outer
convective zone are key parameters in the study of the processes at work in the
stellar interior, in particular when examining the poorly understood processes
operating in the interior of solar-analog stars. We investigate whether the
large dispersion in the observed lithium abundances of solar-analog stars can
be explained by the depth behavior of the outer convective zone masses, within
the framework of the standard convection model based on the local mixing-length
theory. We also aims to analyze the link between rotation and lithium abundance
in solar-analog stars. We computed a new extensive grid of stellar evolutionary
models, applicable to solar-analog stars, for a finely discretized set of mass
and metallicity. From these models, the stellar mass, age, and mass depth of
the outer convective zone were estimated for 117 solar-analog stars, using Teff
and [Fe/H] available in the literature, and the new HIPPARCOS trigonometric
parallax measurements. We determine the age and mass of the outer convective
zone for a bona fide sample of 117 solar-analog stars. No significant on-to-one
correlation is found between the computed convection zone mass and published
lithium abundance, indicating that the large A(Li) dispersion in solar analogs
cannot be explained by the classical framework of envelope convective mixing
coupled with lithium depletion at the bottom of the convection zone. These
results illustrate the need for an extra-mixing process to explain lithium
behavior in solar-analog stars, such as, shear mixing caused by differential
rotation. To derive a more realistic definition of solar-analog stars, as well
as solar-twin, it seems important to consider the inner physical properties of
stars, such as convection, hence rotation and magnetic properties.Comment: 9 pages, 7 figure
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