3,703 research outputs found
Is the energy density of the ground state of the sine-Gordon model unbounded from below for beta^2 > 8 pi ?
We discuss Coleman's theorem concerning the energy density of the ground
state of the sine-Gordon model proved in Phys. Rev. D 11, 2088 (1975).
According to this theorem the energy density of the ground state of the
sine-Gordon model should be unbounded from below for coupling constants beta^2
> 8 pi. The consequence of this theorem would be the non-existence of the
quantum ground state of the sine-Gordon model for beta^2 > 8 pi. We show that
the energy density of the ground state in the sine-Gordon model is bounded from
below even for beta^2 > 8 pi. This result is discussed in relation to Coleman's
theorem (Comm. Math. Phys. 31, 259 (1973)), particle mass spectra and
soliton-soliton scattering in the sine-Gordon model.Comment: 22 pages, Latex, no figures, revised according to the version
accepted for publication in Journal of Physics
Galaxies at z=4 and the Formation of Population II
We report the discovery of four high-redshift objects (3.3 < z < 4) observed
behind the rich cluster CL0939+4713 (Abell 851). One object (DG 433) has a
redshift of z=3.3453; the other three objects have redshifts of z\approx 4: A0
at z=3.9819, DG 353 and P1/P2 at z=3.9822. It is possible that all four objects
are being lensed in some way by the cluster, DG 433 being weakly sheared, A0
being strongly sheared, and DG 353 and P1/P2 being an image pair of a common
source object; detailed modelling of the cluster potential will be necessary to
confirm this hypothesis. The weakness of common stellar wind features like N V
and especially C IV in the spectra of these objects argues for sub-solar
metallicities, at least as low as the SMC. DG 353 and DG 433, which have
ground-based colors, are moderately dusty [E_{int}(B-V) < 0.15], similar to
other z>3 galaxies. Star formation rates range from 2.5 (7.8) h^{-2} to 22.
(78.) h^{-2} M_{\odot}/yr, for q_0=0.5 (0.05), depending on assumptions about
gravitational lensing and extinction, also typical of other z>3 galaxies. These
objects are tenatively identified as the low-metallicity proto-spheroid clumps
that will merge to form the Population II components of today's spheroids.Comment: 16 pages, including 2 PostScript figures. Needs aaspp4.sty
(included). Accepted for publication in the Astrophysical Journa
Massless Thirring model in canonical quantization scheme
It is shown that the exact solvability of the massless Thirring model in the
canonical quantization scheme originates from the intrinsic linearizability of
its Heisenberg equations in the method of dynamical mappings. The corresponding
role of inequivalent representations of free massless Dirac field is
elucidated.Comment: 10 page
Importance of cooling in triggering the collapse of hypermassive neutron stars
The inspiral and merger of a binary neutron star (NSNS) can lead to the
formation of a hypermassive neutron star (HMNS). As the HMNS loses thermal
pressure due to neutrino cooling and/or centrifugal support due to
gravitational wave (GW) emission, and/or magnetic breaking of differential
rotation it will collapse to a black hole. To assess the importance of
shock-induced thermal pressure and cooling, we adopt an idealized equation of
state and perform NSNS simulations in full GR through late inspiral, merger,
and HMNS formation, accounting for cooling. We show that thermal pressure
contributes significantly to the support of the HMNS against collapse and that
thermal cooling accelerates its "delayed" collapse. Our simulations demonstrate
explicitly that cooling can induce the catastrophic collapse of a hot
hypermassive neutron star formed following the merger of binary neutron stars.
Thus, cooling physics is important to include in NSNS merger calculations to
accurately determine the lifetime of the HMNS remnant and to extract
information about the NS equation of state, cooling mechanisms, bar
instabilities and B-fields from the GWs emitted during the transient phase
prior to BH formation.Comment: 13 pages, 7 figures, matches published versio
Static SU(3) potentials for sources in various representations
The potentials and string tensions between static sources in a variety of
representations (fundamental, 8, 6, 15-antisymmetric, 10, 27 and 15-symmetric)
have been computed by measuring Wilson loops in pure gauge SU(3). The
simulations have been done primarily on anisotropic lattices, using a tadpole
improved action improved to O(a_{s}^4). A range of lattice spacings (0.43 fm,
0.25 fm and 0.11 fm) and volumes (, , and ) has been used in an attempt to control
discretization and finite volume effects. At intermediate distances, the
results show approximate Casimir scaling. Finite lattice spacing effects
dominate systematic error, and are particularly large for the representations
with the largest string tensions.Comment: Version to appear in PR
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