253 research outputs found
Differences in the Cooling Behavior of Strange Quark Matter Stars and Neutron Stars
The general statement that hypothetical strange (quark matter) stars cool
more rapidly than neutron stars is investigated in greater detail. It is found
that the direct Urca process could be forbidden not only in neutron stars but
also in strange stars. In this case, strange stars are slowly cooling, and
their surface temperatures are more or less indistinguishable from those of
slowly cooling neutron stars. Furthermore the case of enhanced cooling is
reinvestigated. It shows that strange stars cool significantly more rapidly
than neutron stars within the first years after birth. This feature
could become particularly interesting if continued observation of SN 1987A
would reveal the temperature of the possibly existing pulsar at its center.Comment: 9 pages, LaTeX (aas-style file), 2 ps-figures. To be published in ApJ
Letter
Strangeness in Neutron Stars
It is generally agreed on that the tremendous densities reached in the
centers of neutron stars provide a high-pressure environment in which numerous
novel particles processes are likely to compete with each other. These
processes range from the generation of hyperons to quark deconfinement to the
formation of kaon condensates and H-matter. There are theoretical suggestions
of even more exotic processes inside neutron stars, such as the formation of
absolutely stable strange quark matter, a configuration of matter even more
stable than the most stable atomic nucleus, iron. In the latter event, neutron
stars would be largely composed of pure quark matter, eventually enveloped in a
thin nuclear crust. No matter which physical processes are actually realized
inside neutron stars, each one leads to fingerprints, some more pronounced than
others though, in the observable stellar quantities. This feature combined with
the unprecedented progress in observational astronomy, which allows us to see
vistas with remarkable clarity that previously were only imagined, renders
neutron stars to nearly ideal probes for a wide range of physical studies,
including the role of strangeness in dense matter.Comment: 15 pages, 6 figures, Presented at the 5th International Conference on
Strangeness in Quark Matter (Strangeness 2000), Berkeley, California, USA,
July 20-25, 200
Are strange stars distinguishable from neutron stars by their cooling behaviour?
The general statement that strange stars cool more rapidly than neutron stars
is investigated in greater detail. It is found that the direct Urca process
could be forbidden not only in neutron stars but also in strange stars. If so,
strange stars would be slowly cooling and their surface temperatures would be
more or less indistinguishable from those of slowly cooling neutron stars. The
case of enhanced cooling is reinvestigated as well. It is found that strange
stars cool significantly more rapidly than neutron stars within the first years after birth. This feature could become particularly interesting if
continued observation of SN 1987A would reveal the temperature of the possibly
existing pulsar at its centre.Comment: 10 pages, 3 ps-figures, to appear in the proceedings of the
International Symposium on ''Strangeness in Quark Matter 1997``, April
14--18, Thera (Santorini), Hella
Interplay between quantum criticality and geometrical frustration in Fe3Mo3N with stella quadrangula lattice
In the eta-carbide-type correlated-electron metal Fe3Mo3N, ferromagnetism is
abruptly induced from a nonmagnetic non-Fermi-liquid ground state either when a
magnetic field (~14 T) applied to it or when it is doped with a slight amount
of impurity (~5% Co). We observed a peak in the paramagnetic neutron scattering
intensity at finite wave vectors, revealing the presence of the
antiferromagnetic (AF) correlation hidden in the magnetic measurements. It
causes a new type of geometrical frustration in the stellla quadrangula lattice
of the Fe sublattice. We propose that the frustrated AF correlation suppresses
the F correlation to its marginal point and is therfore responsible for the
origin of the ferromagnetic (F) quantum critical behavior in pure Fe3Mo3N
Magnetized strangelets at finite temperature
The main properties of magnetized strangelets, namely, their energy per
baryon, radius and electric charge, are studied. Temperature effects are also
taken into account in order to study their stability compared to the 56Fe
isotope and non-magnetized strangelets using the liquid drop model. Massive
quarks are considered with the aim to have a more realistic description for
strangelets in the astrophysical context and the environment of heavy ion
colliders, playing also an important role in the thermodynamical quantities of
the quark gas. It is concluded that the presence of a magnetic field tends to
stabilize more the strangelets, even when temperature effects are taken into
account. Magnetized strangelets in a paired superconductor phase (magnetized
color flavor locked phase) are also discussed. It is shown that they are more
stable than ordinary magnetized strangelets for typical gap values of the order
of O(100) MeV.Comment: 10 pages, 10 figures, discussion extended, new references adde
The Principle of Non-Gravitating Vacuum Energy and some of its consequences
For Einstein's General Relativity (GR) or the alternatives suggested up to
date the vacuum energy gravitates. We present a model where a new measure is
introduced for integration of the total action in the D-dimensional space-time.
This measure is built from D scalar fields . As a consequence of
such a choice of the measure, the matter lagrangian can be changed by
adding a constant while no gravitational effects, like a cosmological term, are
induced. Such Non-Gravitating Vacuum Energy (NGVE) theory has an infinite
dimensional symmetry group which contains volume-preserving diffeomorphisms in
the internal space of scalar fields . Other symmetries contained
in this symmetry group, suggest a deep connection of this theory with theories
of extended objects. In general {\em the theory is different from GR} although
for certain choices of , which are related to the existence of an
additional symmetry, solutions of GR are solutions of the model. This is
achieved in four dimensions if is due to fundamental bosonic and
fermionic strings. Other types of matter where this feature of the theory is
realized, are for example: scalars without potential or subjected to nonlinear
constraints, massless fermions and point particles. The point particle plays a
special role, since it is a good phenomenological description of matter at
large distances. de Sitter space is realized in an unconventional way, where
the de Sitter metric holds, but such de Sitter space is supported by the
existence of a variable scalar field which in practice destroys the maximal
symmetry. The only space - time where maximal symmetry is not broken, in a
dynamical sense, is Minkowski space. The theory has non trivial dynamics in 1+1
dimensions, unlike GR.Comment: 23 page
Limits on excited tau leptons masses from leptonic tau decays
We study the effects induced by excited leptons on the leptonic tau decay at
one loop level. Using a general effective lagrangian approach to describe the
couplings of the excited leptons, we compute their contributions to the
leptonic decays and use the current experimental values of the branching ratios
to put limits on the mass of excited states and the substructure scale.Comment: 10 pages, 6 figures, to be published in Phys. Rev.
Sneutrino-induced like sign dilepton signal with conserved R-parity
Lepton number violation could be manifest in the sneutrino sector of
supersymmetric extensions of the standard model with conserved R-parity. Then
sneutrinos decay partly into the ``wrong sign charged lepton'' final state, if
kinematically accessible. In sneutrino pair production or associated single
sneutrino production, the signal then is a like sign dilepton final state.
Under favourable circumstances, such a signal could be visible at the LHC or a
next generation linear collider for a relative sneutrino mass-splitting of
order and sneutrino width of order (1 GeV). On the
other hand, the like sign dilepton event rate at the TEVATRON is probably too
small to be observable.Comment: 19 pages, 14 Figures. Section about LSD at LHC and TEVATRON added.
Previous Title "Single sneutrino production and the wrong charged lepton
signal
Model of the Quark Mixing Matrix
The structure of the Cabibbo-Kobayashi-Maskawa (CKM) matrix is analyzed from
the standpoint of a composite model. A model is constructed with three families
of quarks, by taking tensor products of sufficient numbers of spin-1/2
representations and imagining the dominant terms in the mass matrix to arise
from spin-spin interactions. Generic results then obtained include the familiar
relation , and a less frequently
seen relation . The magnitudes of
and come out naturally to be of the right order. The phase in
the CKM matrix can be put in by hand, but its origin remains obscure.Comment: Presented by Mihir P. Worah at DPF 92 Meeting, Fermilab, November,
1992. 3 pages, LaTeX fil
Naturalness Bounds on Dipole Moments from New Physics
Assuming naturalness that the quantum corrections to the mass should not
exceed the order of the observed mass, we derive and apply model-independent
bounds on the anomalous magnetic moments and electric dipole moments of leptons
and quarks due to new physics.Comment: 4 pages, 2 figure
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