17,375 research outputs found
Comparison of |Q|=1 and |Q|=2 gauge-field configurations on the lattice four-torus
It is known that exactly self-dual gauge-field configurations with
topological charge |Q|=1 cannot exist on the untwisted continuum 4-torus. We
explore the manifestation of this remarkable fact on the lattice 4-torus for
SU(3) using advanced techniques for controlling lattice discretization errors,
extending earlier work of De Forcrand et. al. for SU(2). We identify three
distinct signals for the instability of |Q|=1 configurations, and show that
these manifest themselves early in the cooling process, long before the
would-be instanton has shrunk to a size comparable to the lattice
discretization threshold. These signals do not appear for our |Q|=2
configurations. This indicates that these signals reflect the truly global
nature of the instability, rather than local discretization effects.
Monte-Carlo generated SU(3) gauge field configurations are cooled to the
self-dual limit using an O(a^4)-improved gauge action chosen to have small but
positive O(a^6) errors. This choice prevents lattice discretization errors from
destroying instantons provided their size exceeds the dislocation threshold of
the cooling algorithm. Lattice discretization errors are evaluated by comparing
the O(a^4)-improved gauge-field action with an O(a^4)-improved action
constructed from the square of an O(a^4)-improved lattice field-strength
tensor, thus having different O(a^6) discretization errors. The number of
action-density peaks, the instanton size and the topological charge of
configurations is monitored. We observe a fluctuation in the total topological
charge of |Q|=1 configurations, and demonstrate that the onset of this unusual
behavior corresponds with the disappearance of multiple-peaks in the action
density. At the same time discretization errors are minimal.Comment: 12 pages, 9 figures, submitted to Phys. Rev.
Rubidium and zirconium abundances in massive Galactic asymptotic giant branch stars revisited
Luminous Galactic OH/IR stars have been identified as massive (>4-5 M_s) AGB
stars experiencing HBB and Li production. Their Rb abundances and [Rb/Zr]
ratios derived from hydrostatic model atmospheres, are significantly higher
than predictions from AGB nucleosynthesis models, posing a problem to our
understanding of AGB evolution and nucleosynthesis. We report new Rb and Zr
abundances in the full sample of massive Galactic AGB stars, previously studied
with hydrostatic models, by using more realistic extended model atmospheres. We
use a modified version of the spectral synthesis code Turbospectrum and
consider the presence of a circumstellar envelope and radial wind. The Rb and
Zr abundances are determined from the 7800 A Rb I resonant line and the 6474 A
ZrO bandhead, respectively, and we explore the sensitivity of the derived
abundances to variations of the stellar (Teff) and wind (M_loss, beta and vexp)
parameters in the extended models. The Rb and Zr abundances derived from the
best spectral fits are compared with the most recent AGB nucleosynthesis
theoretical models. The new Rb abundances are much lower (even 1-2 dex) than
those derived with the hydrostatic models, while the Zr abundances are similar.
The Rb I line profile and Rb abundance are very sensitive to the M_loss rate
but much less sensitive to variations of the wind velocity-law and the
vexp(OH). We confirm the earlier preliminary results based on a smaller sample
of massive O-rich AGB stars, that the use of extended atmosphere models can
solve the discrepancy between the AGB nucleosynthesis theoretical models and
the observations of Galactic massive AGB stars. The Rb abundances, however, are
still strongly dependent of the M_loss, which is unknown in these AGB stars.
Accurate M_loss rates in these massive Galactic AGB stars are needed in order
to break the models degeneracy and get reliable Rb abundances in these stars.Comment: Accepted for publication in A&A, 14 pages, 12 figures, 4 table
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