481 research outputs found
Gravitational time advancement and its possible detection
The gravitational time advancement is a natural but a consequence of curve
space-time geometry. In the present work the expressions of gravitational time
advancement have been obtained for geodesic motions. The situation when the
distance of signal travel is small in comparison to the distance of closest
approach has also been considered. The possibility of experimental detection of
time advancement effect has been explored.Comment: 5 pages, 4 figures, a part of the work has been changed in the
revised versio
Geodesy by radio interferometry: Effects of atmospheric modeling errors on estimates of baseline length
Analysis of very long baseline interferometry data indicates that systematic errors in prior estimates
of baseline length, of order 5 cm for ~8000-km baselines, were due primarily to mismodeling of the
electrical path length of the troposphere and mesosphere ("atmospheric delay"). Here we discuss
observational evidence for the existence of such errors in the previously used models for the atmospheric
delay and develop a new "mapping" function for the elevation angle dependence of this delay. The
delay predicted by this new mapping function differs from ray trace results by less than ~5 mm, at all
elevations down to 5° elevation, and introduces errors into the estimates of baseline length of âą< 1 cm,
for the multistation intercontinental experiment analyzed here
Relativistic Effects in the Motion of the Moon
The main general relativistic effects in the motion of the Moon are briefly
reviewed. The possibility of detection of the solar gravitomagnetic
contributions to the mean motions of the lunar node and perigee is discussed.Comment: LaTeX file, no figures, 13 pages, to appear in: 'Testing relativistic
gravity in space', edited by C. Laemmerzahl, C.W.F. Everitt and F.W. Hehl
(Springer, Berlin 2000
Light-time computations for the BepiColombo radioscience experiment
The radioscience experiment is one of the on board experiment of the Mercury
ESA mission BepiColombo that will be launched in 2014. The goals of the
experiment are to determine the gravity field of Mercury and its rotation
state, to determine the orbit of Mercury, to constrain the possible theories of
gravitation (for example by determining the post-Newtonian (PN) parameters), to
provide the spacecraft position for geodesy experiments and to contribute to
planetary ephemerides improvement. This is possible thanks to a new technology
which allows to reach great accuracies in the observables range and range rate;
it is well known that a similar level of accuracy requires studying a suitable
model taking into account numerous relativistic effects. In this paper we deal
with the modelling of the space-time coordinate transformations needed for the
light-time computations and the numerical methods adopted to avoid rounding-off
errors in such computations.Comment: 14 pages, 7 figures, corrected reference
Low autocorrelated multi-phase sequences
The interplay between the ground state energy of the generalized Bernasconi
model to multi-phase, and the minimal value of the maximal autocorrelation
function, , , is examined analytically and
the main results are: (a) The minimal value of is
significantly smaller than the typical value for random
sequences . (b) over all sequences
of length N is obtained in an energy which is about 30% above the ground-state
energy of the generalized Bernasconi model, independent of the number of phases
m. (c) The maximal merit factor grows linearly with m. (d) For a
given N, indicating that for m=N,
, i.e. a Barker code exits. The analytical results are
confirmed by simulations.Comment: 4 pages, 4 figure
The relativistic precession of the orbits
The relativistic precession can be quickly inferred from the nonlinear polar
orbit equation without actually solving it.Comment: Accepted for publication in Astrophysics & Space Scienc
On the 0-dimensional cusps of the Kahler moduli of a K3 surface
Let S be a projective K3 surface. It is proved that the 0-dimensional cusps
of the Kahler moduli of S are in one-to-one correspondence with the twisted
Fourier-Mukai partners of S. This leads to a counting formula for the
0-dimensional cusps of the Kahler moduli. Applications to rational maps between
K3 surfaces with large Picard numbers are given. When the Picard number of S is
1, the bijective correspondence is calculated explicitly.Comment: 24page
Giant Coulomb broadening and Raman lasing on ionic transitions
CW generation of anti-Stokes Raman laser on a number of blue-green argon-ion
lines (4p-4s, 4p-3d) has been demonstrated with optical pumping from metastable
levels 3d'^2G, 3d^4F. It is found, that the population transfer rate is
increased by a factor of 3-5 (and hence, the output power of such Raman laser)
owing to Coulomb diffusion in the velocity space. Measured are the excitation
and relaxation rates for the metastable level. The Bennett hole on the
metastable level has been recorded using the probe field technique. It has been
shown that the Coulomb diffusion changes shape of the contour to exponential
cusp profile while its width becomes 100 times the Lorentzian one and reaches
values close to the Doppler width. Such a giant broadening is also confirmed by
the shape of the absorption saturation curve.Comment: RevTex 18 pages, 5 figure
Time transfer and frequency shift to the order 1/c^4 in the field of an axisymmetric rotating body
Within the weak-field, post-Newtonian approximation of the metric theories of
gravity, we determine the one-way time transfer up to the order 1/c^4, the
unperturbed term being of order 1/c, and the frequency shift up to the order
1/c^4. We adapt the method of the world-function developed by Synge to the
Nordtvedt-Will PPN formalism. We get an integral expression for the
world-function up to the order 1/c^3 and we apply this result to the field of
an isolated, axisymmetric rotating body. We give a new procedure enabling to
calculate the influence of the mass and spin multipole moments of the body on
the time transfer and the frequency shift up to the order 1/c^4. We obtain
explicit formulas for the contributions of the mass, of the quadrupole moment
and of the intrinsic angular momentum. In the case where the only PPN
parameters different from zero are beta and gamma, we deduce from these results
the complete expression of the frequency shift up to the order 1/c^4. We
briefly discuss the influence of the quadrupole moment and of the rotation of
the Earth on the frequency shifts in the ACES mission.Comment: 17 pages, no figure. Version 2. Abstract and Section II revised. To
appear in Physical Review
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