11,154 research outputs found
The genus of the configuration spaces for Artin groups of affine type
Let be a Coxeter system, finite, and let be the
associated Artin group. One has configuration spaces where
and a natural -covering The
Schwarz genus is a natural topological invariant to consider. In
this paper we generalize this result by computing the Schwarz genus for a class
of Artin groups, which includes the affine-type Artin groups. Let be
the simplicial scheme of all subsets such that the parabolic group
is finite. We introduce the class of groups for which equals
the homological dimension of and we show that is always the
maximum possible for such class of groups. For affine Artin groups, such
maximum reduces to the rank of the group. In general, it is given by
where is a well-known -complex
which has the same homotopy type as Comment: To appear in Atti Accad. Naz. Lincei Rend. Lincei Mat. App
Superconductivity emerging from an electronic phase separation in the charge ordered phase of RbFeAs
As, Rb and Rb nuclear quadrupole resonance (NQR) and
Rb nuclear magnetic resonance (NMR) measurements in RbFeAs
iron-based superconductor are presented. We observe a marked broadening of
As NQR spectrum below K which is associated with the
onset of a charge order in the FeAs planes. Below we observe a power-law
decrease in As nuclear spin-lattice relaxation rate down to K. Below that temperature the nuclei start to probe different dynamics
owing to the different local electronic configurations induced by the charge
order. A fraction of the nuclei probes spin dynamics associated with electrons
approaching a localization while another fraction probes activated dynamics
possibly associated with a pseudogap. These different trends are discussed in
the light of an orbital selective behaviour expected for the electronic
correlations.Comment: 5 pages, 3 figures and 4 pages of supplemental materia
Phase diagram of soft-core bosons in two dimensions
The low temperature phase diagram of Bose soft disks in two dimensions is
studied by numerical simulations. It is shown that a supersolid cluster phase
exists, within a range of the model parameters, analogous to that recently
observed for a system of aligned dipoles interacting via a softened potential
at short distance. These findings indicate that a long-range tail of the
interaction is unneeded to obtain such a phase, and that the soft-core
repulsive interaction is the minimal model for supersolidity
Imaginary Time Correlations and the phaseless Auxiliary Field Quantum Monte Carlo
The phaseless Auxiliary Field Quantum Monte Carlo method provides a well
established approximation scheme for accurate calculations of ground state
energies of many-fermions systems. Here we apply the method to the calculation
of imaginary time correlation functions. We give a detailed description of the
technique and we test the quality of the results for static and dynamic
properties against exact values for small systems.Comment: 13 pages, 6 figures; submitted to J. Chem. Phy
Dynamic structure factor for 3He in two-dimensions
Recent neutron scattering experiments on 3He films have observed a zero-sound
mode, its dispersion relation and its merging with -and possibly emerging from-
the particle-hole continuum. Here we address the study of the excitations in
the system via quantum Monte Carlo methods: we suggest a practical scheme to
calculate imaginary time correlation functions for moderate-size fermionic
systems. Combined with an efficient method for analytic continuation, this
scheme affords an extremely convincing description of the experimental
findings.Comment: 5 pages, 5 figure
Cumulative physical uncertainty in modern stellar models. II. The dependence on the chemical composition
We extend our work on the effects of the uncertainties on the main input
physics for the evolution of low-mass stars. We analyse the dependence of the
cumulative physical uncertainty affecting stellar tracks on the chemical
composition. We calculated more than 6000 stellar tracks and isochrones, with
metallicity ranging from Z = 0.0001 to 0.02, by changing the following physical
inputs within their current range of uncertainty: 1H(p,nu e+)2H,
14N(p,gamma)15O and triple-alpha reaction rates, radiative and conductive
opacities, neutrino energy losses, and microscopic diffusion velocities. The
analysis was performed using a latin hypercube sampling design. We examine in a
statistical way the dependence on the variation of the physical inputs of the
turn-off (TO) luminosity, the central hydrogen exhaustion time (t_H), the
luminosity and the helium core mass at the red-giant branch (RGB) tip, and the
zero age horizontal branch (ZAHB) luminosity in the RR Lyrae region. For the
stellar tracks, an increase from Z = 0.0001 to Z = 0.02 produces a cumulative
physical uncertainty in TO luminosity from 0.028 dex to 0.017 dex, while the
global uncertainty on t_H increases from 0.42 Gyr to 1.08 Gyr. For the RGB tip,
the cumulative uncertainty on the luminosity is almost constant at 0.03 dex,
whereas the one the helium core mass decreases from 0.0055 M_sun to 0.0035
M_sun. The dependence of the ZAHB luminosity error is not monotonic with Z, and
it varies from a minimum of 0.036 dex at Z = 0.0005 to a maximum of 0.047 dex
at Z = 0.0001. Regarding stellar isochrones of 12 Gyr, the cumulative physical
uncertainty on the predicted TO luminosity and mass increases respectively from
0.012 dex to 0.014 dex and from 0.0136 M_sun to 0.0186 M_sun. Consequently, for
ages typical of galactic globular clusters, the uncertainty on the age inferred
from the TO luminosity increases from 325 Myr to 415 Myr.Comment: Accepted for publication in A&
On the age of Galactic bulge microlensed dwarf and subgiant stars
Recent results by Bensby and collaborators on the ages of microlensed stars
in the Galactic bulge have challenged the picture of an exclusively old stellar
population. However, these age estimates have not been independently confirmed.
In this paper we verify these results by means of a grid-based method and
quantify the systematic biases that might be induced by some assumptions
adopted to compute stellar models. We explore the impact of increasing the
initial helium abundance, neglecting the element microscopic diffusion, and
changing the mixing-length calibration in theoretical stellar track
computations. We adopt the SCEPtER pipeline with a novel stellar model grid for
metallicities [Fe/H] from -2.00 to 0.55 dex, and masses in the range [0.60;
1.60] Msun from the ZAMS to the helium flash at the red giant branch tip. We
show for the considered evolutionary phases that our technique provides
unbiased age estimates. Our age results are in good agreement with Bensby and
collaborators findings and show 16 stars younger than 5 Gyr and 28 younger than
9 Gyr over a sample of 58. The effect of a helium enhancement as large as Delta
Y/Delta Z = 5 is quite modest, resulting in a mean age increase of metal rich
stars of 0.6 Gyr. Even simultaneously adopting a high helium content and the
upper values of age estimates, there is evidence of 4 stars younger than 5 Gyr
and 15 younger than 9 Gyr. For stars younger than 5 Gyr, the use of stellar
models computed by neglecting microscopic diffusion or by assuming a
super-solar mixing-length value leads to a mean increase in the age estimates
of about 0.4 Gyr and 0.5 Gyr respectively. Even considering the upper values
for the age estimates, there are four stars estimated younger than 5 Gyr is in
both cases. Thus, the assessment of a sizeable fraction of young stars among
the microlensed sample in the Galactic bulge appears robust.Comment: Accepted for publication in A&A. Abstract shortene
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