10,607 research outputs found
The Family SU(2)_l x SU(2)_h x U(1) Model
We consider extension of the standard model where the first two families of quarks and leptons transform according to
the group and the third family according to the group. In
this approach, the largeness of top-quark mass is associated with the large
vacuum expectation value of the corresponding Higgs field. The model predicts
almost degenerate heavy and bosons with non-universal couplings, and
extra Higgs bosons. We present in detail the symmetry breaking mechanism, and
carry out the subsequent phenomenology of the gauge sector. We compare the
model with electroweak precision data, and conclude that the extra gauge bosons
and the Higgs bosons whose masses lie in the TeV range, can be discovered at
the LHC.Comment: Latex 18 pages. No figure. Some references added. Version appeared in
PR
Reverberation Mapping and the Disk Wind Model of the Broad Line Region
Using the disk wind model of Murray et al. (1995), we calculate line profiles
and frequency-resolved response functions for broad line emission from the
surface of an accretion disk in an AGN in the presence of a radiatively driven
wind. We find that the combined effects of the shears in the wind and in the
disk itself produce anisotropic line emission which solves several well-known
problems connected with disk models of the broad line region. In particular,
the broadening of resonance lines such as \Civ, \Lya, and \Nv\/ can be
attributed to orbital motion of the disk gas at radii as close as ~cm in Seyferts without requiring unrealistically large emission
regions in order to produce single-peaked profiles. Furthermore, the anisotropy
of the line emission results in frequency-dependent response functions which
are no longer red-blue symmetric so that the time delays inferred for the
various red and blue components of the line agree qualitatively with recent
reverberation mapping observations of NGC~5548.Comment: 17 pages text, 8 postscript figure
Testing Gaussian random hypothesis with the cosmic microwave background temperature anisotropies in the three-year WMAP data
We test the hypothesis that the temperature of the cosmic microwave
background is consistent with a Gaussian random field defined on the celestial
sphere, using de-biased internal linear combination (DILC) map produced from
the 3-year WMAP data. We test the phases for spherical harmonic modes with l <=
10 (which should be the cleanest) for their uniformity, randomness, and
correlation with those of the foreground templates. The phases themselves are
consistent with a uniform distribution, but not for l <= 5, and the differences
between phases are not consistent with uniformity. For l=3 and l=6, the phases
of the CMB maps cross-correlate with the foregrounds, suggestion the presence
of residual contamination in the DLC map even on these large scales. We also
use a one-dimensional Fourier representation to assemble a_lm into the \Delta
T_l(\phi) for each l mode, and test the positions of the resulting maxima and
minima for consistency with uniformity randomness on the unit circle. The
results show significant departures at the 0.5% level, with the one-dimensional
peaks being concentrated around \phi=180 degs. This strongly significant
alignment with the Galactic meridian, together with the cross-correlation of
DILC phases with the foreground maps, strongly suggests that even the lowest
spherical harmonic modes in the map are significantly contaminated with
foreground radiation.Comment: submitted to ApJL, one paragraph is added in Section 3 and some more
in the Referenc
Shifts of the nuclear resonance in the vortex lattice in YBaCuO
The NMR and NQR spectra of Cu in the CuO plane of
YBaCuO in the superconducting state are discussed in terms of the
phenomenological theory of Ginzburg-Landau type extended to lower temperatures.
We show that the observed spectra, Kumagai {\em et al.}, PRB {\bf 63}, 144502
(2001), can be explained by a standard theory of the Bernoulli potential with
the charge transfer between CuO planes and CuO chains assumed.Comment: 11 pages 7 figure
The Origin of the Young Stars in the Nucleus of M31
The triple nucleus of M31 consists of a population of old red stars in an
eccentric disk (P1 and P2) and another population of younger A stars in a
circular disk (P3) around M31's central supermassive black hole (SMBH). We
argue that P1 and P2 determine the maximal radial extent of the younger A star
population and provide the gas that fueled the starburst that generated P3. The
eccentric stellar disk creates an non-axisymmetric perturbation to the
potential. This perturbed potential drives gas into the inner parsec around the
SMBH, if the pattern speed of the eccentric stellar disk is . We show that stellar mass loss from P1 and P2 is
sufficient to create a gravitationally unstable gaseous disk of \sim
10^5\Msun every Gyrs, consistent with the 200 Myr age of P3. Similar
processes may act in other systems to produce very compact nuclear starbursts.Comment: 10 pages, 7 figures, accepted by ApJ, changes made from referee
suggestion
Long-Distance Contributions to D^0-D^0bar Mixing Parameters
Long-distance contributions to the - mixing parameters and
are evaluated using latest data on hadronic decays. In particular, we
take on two-body and decays to evaluate the contributions of
two-body intermediate states because they account for of hadronic
decays. Use of the diagrammatic approach has been made to estimate
yet-observed decay modes. We find that is of order a few
and of order from hadronic and modes. These are in good
agreement with the latest direct measurement of - mixing
parameters using the and decays by
BaBar. We estimate the contribution to from the modes using the
factorization model and comment on the single-particle resonance effects and
contributions from other two-body modes involving even-parity states.Comment: 18 pages and 1 figure; footnotes and references added; to appear in
Phys. Rev.
On the Antenna Beam Shape Reconstruction Using Planet Transit
The calibration of the in-flight antenna beam shape and possible
beamdegradation is one of the most crucial tasks for the upcoming Planck
mission. We examine several effects which could significantly influence the
in-flight main beam calibration using planet transit: the problems of the
variability of the Jupiter's flux, the antenna temperature and passing of the
planets through the main beam. We estimate these effects on the antenna beam
shape calibration and calculate the limits on the main beam and far sidelobe
measurements, using observations of Jupiter and Saturn. We also discuss
possible effects of degradation of the mirror surfaces and specify
corresponding parameters which can help us to determine these effects.Comment: 10 pages, 8 figure
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