1,188 research outputs found
Auxiliary Field Diffusion Monte Carlo calculation of nuclei with A<40 with tensor interactions
We calculate the ground-state energy of 4He, 8He, 16O, and 40Ca using the
auxiliary field diffusion Monte Carlo method in the fixed phase approximation
and the Argonne v6' interaction which includes a tensor force. Comparison of
our light nuclei results to those of Green's function Monte Carlo calculations
shows the accuracy of our method for both open and closed shell nuclei. We also
apply it to 16O and 40Ca to show that quantum Monte Carlo methods are now
applicable to larger nuclei.Comment: 4 pages, no figure
Contact interaction in an unitary ultracold Fermi gas
An ultracold Fermi atomic gas at unitarity presents universal properties that
in the diluted limit can be well described by a contact interaction. By
employing a guide function with correct boundary conditions and making simple
modifications to the sampling procedure we are able to handle for the first
time a true contact interaction in a quantum Monte Carlo calculation. The
results are obtained with small variances. Our calculations for the Bertsch and
contact parameters are in excellent agreement with published experiments. The
possibility of using a more faithfully description of ultracold atomic gases
can help uncover features yet unknown of the ultracold atomic gases. In
addition, this work paves the way to perform quantum Monte Carlo calculations
for systems interacting with contact interactions, where in many cases the
description using potentials with finite effective range might not be accurate
CoRoT 102918586: a Gamma Dor pulsator in a short period eccentric eclipsing binary
Pulsating stars in eclipsing binary systems are powerful tools to test
stellar models. Binarity enables to constrain the pulsating component physical
parameters, whose knowledge drastically improves the input physics for
asteroseismic studies. The study of stellar oscillations allows us, in its
turn, to improve our understanding of stellar interiors and evolution. The
space mission CoRoT discovered several promising objects suitable for these
studies, which have been photometrically observed with unprecedented accuracy,
but needed spectroscopic follow-up. A promising target was the relatively
bright eclipsing system CoRoT 102918586, which turned out to be a double-lined
spectroscopic binary and showed, as well, clear evidence of Gamma Dor type
pulsations. We obtained phase resolved high-resolution spectroscopy with the
Sandiford spectrograph at the McDonald 2.1m telescope and the FEROS
spectrograph at the ESO 2.2m telescope. Spectroscopy yielded both the radial
velocity curves and, after spectra disentangling, the component effective
temperatures, metallicity and line-of-sight projected rotational velocities.
The CoRoT light curve was analyzed with an iterative procedure, devised to
disentangle eclipses from pulsations. We obtained an accurate determination of
the system parameters, and by comparison with evolutionary models strict
constraints on the system age. Finally, the residuals obtained after
subtraction of the best fitting eclipsing binary model were analyzed to
determine the pulsator properties. We achieved a quite complete and consistent
description of the system. The primary star pulsates with typical {\gamma} Dor
frequencies and shows a splitting in period which is consistent with high order
g-mode pulsations in a star of the corresponding physical parameters. The value
of the splitting, in particular, is consistent with pulsations in l = 1 modes.Comment: 12 pages, 10 figures. Accepted for publication in Astronomy and
Astrophysic
Microscopic calculation of the equation of state of nuclear matter and neutron star structure
We present results for neutron star models constructed with a new equation of
state for nuclear matter at zero temperature. The ground state is computed
using the Auxiliary Field Diffusion Monte Carlo (AFDMC) technique, with
nucleons interacting via a semi-phenomenological Hamiltonian including a
realistic two-body interaction. The effect of many-body forces is included by
means of additional density-dependent terms in the Hamiltonian. In this letter
we compare the properties of the resulting neutron-star models with those
obtained using other nuclear Hamiltonians, focusing on the relations between
mass and radius, and between the gravitational mass and the baryon number.Comment: modified version with a slightly different Hamiltonian and
parametrization of the EO
Recent progress on the accurate determination of the equation of state of neutron and nuclear matter
The problem of accurately determining the equation of state of nuclear and
neutron matter at density near and beyond saturation is still an open
challenge. In this paper we will review the most recent progress made by means
of Quantum Monte Carlo calculations, which are at present the only ab-inito
method capable to treat a sufficiently large number of particles to give
meaningful estimates depending only on the choice of the nucleon-nucleon
interaction. In particular, we will discuss the introduction of
density-dependent interactions, the study of the temperature dependence of the
equation of state, and the possibility of accurately studying the effect of the
onset of hyperons by developing an accurate hyperon-nucleon and
hyperon-nucleon-nucleon interaction.Comment: 3 figures, 1 table, to appear in the Proceedings of "XIII Convegno di
Cortona su Problemi di Fisica Nucleare Teorica", Cortona (Italy), April 6-8,
201
Equation of state of superfluid neutron matter and the calculation of pairing gap
We present a Quantum Monte Carlo study of the zero temperature equation of
state of neutron matter and the computation of the pairing gap in the
low-density regime with fm. The system is described by a
non-relativistic nuclear Hamiltonian including both two-- and three--nucleon
interactions of the Argonne and Urbana type. This model interaction provides
very accurate results in the calculation of the binding energy of light nuclei.
A suppression of the gap with respect to the pure BCS theory is found, but
sensibly weaker than in other works that attempt to include polarization
effects in an approximate way
On the accretion properties of young stellar objects in the L1615/L1616 cometary cloud
We present the results of FLAMES/UVES and FLAMES/GIRAFFE spectroscopic
observations of 23 low-mass stars in the L1615/L1616 cometary cloud,
complemented with FORS2 and VIMOS spectroscopy of 31 additional stars in the
same cloud. L1615/L1616 is a cometary cloud where the star formation was
triggered by the impact of the massive stars in the Orion OB association. From
the measurements of the lithium abundance and radial velocity, we confirm the
membership of our sample to the cloud. We use the equivalent widths of the
H, H, and the HeI 5876, 6678, 7065
\AAemission lines to calculate the accretion luminosities, ,
and the mass accretion rates, . We find in L1615/L1616 a
fraction of accreting objects (), which is consistent with the
typical fraction of accretors in T associations of similar age ( Myr).
The mass accretion rate for these stars shows a trend with the mass of the
central object similar to that found for other star-forming regions, with a
spread at a given mass which depends on the evolutionary model used to derive
the stellar mass. Moreover, the behavior of the colors with indicates that strong accretors with dex show large excesses in the bands, as in previous
studies. We also conclude that the accretion properties of the L1615/L1616
members are similar to those of young stellar objects in T associations, like
Lupus.Comment: Accepted by Astronomy and Astrophysics. 17 pages, 11 figures, 6
table
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