9,655 research outputs found
Simulations of the relativistic parsec-scale jet in 3C273
We present a hydrodynamical 3D simulation of the relativistic jet in 3C273,
in comparison to previous linear perturbation analysis of Kelvin-Helmholtz
instability developing in the jet. Our aim is to assess advantages and
limitations of both analytical and numerical approaches and to identify spatial
and temporal scales on which the linear regime of Kelvin-Helmholtz instability
can be applied in studies of morphology and kinematics of parsec-scale jets.Comment: 4 pages, 3 figures; to be published in Proceedings of the workshop
"Multiband Approach to AGN", held on Sep.30-Oct.2 in Bonn. Publication:
Memorie della Societa Astronomica Italiana, v. 26, No.1 (2005). Reduced
figure resolution! Version with original figures is availavble at
http://www.mpifr-bonn.mpg.de/bonn04/proceedings/perucho.pd
Dynamical analysis of the Gliese-876 Laplace resonance
The existence of multiple planetary systems involved in mean motion
conmensurabilities has increased significantly since the Kepler mission.
Although most correspond to 2-planet resonances, multiple resonances have also
been found. The Laplace resonance is a particular case of a three-body
resonance where the period ratio between consecutive pairs is n_1/n_2 near to
n_2/n_3 near to 2/1. It is not clear how this triple resonance can act in order
to stabilize (or not) the systems.
The most reliable extrasolar system located in a Laplace resonance is GJ876
because it has two independent confirmations. However best-fit parameters were
obtained without previous knowledge of resonance structure and no exploration
of all the possible stable solutions for the system where done.
In the present work we explored the different configurations allowed by the
Laplace resonance in the GJ876 system by varying the planetary parameters of
the third outer planet. We find that in this case the Laplace resonance is a
stabilization mechanism in itself, defined by a tiny island of regular motion
surrounded by (unstable) highly chaotic orbits. Low eccentric orbits and mutual
inclinations from -20 to 20 degrees are compatible with the observations. A
definite range of mass ratio must be assumed to maintain orbital stability.
Finally we give constrains for argument of pericenters and mean anomalies in
order to assure stability for this kind of systems.Comment: 7 pages, 7 figures, accepted in MNRA
Front dynamics in turbulent media
A study of a stable front propagating in a turbulent medium is presented. The
front is generated through a reaction-diffusion equation, and the turbulent
medium is statistically modeled using a Langevin equation. Numerical
simulations indicate the presence of two different dynamical regimes. These
regimes appear when the turbulent flow either wrinkles a still rather sharp
propagating interfase or broadens it. Specific dependences of the propagating
velocities on stirring intensities appropriate to each case are found and
fitted when possible according to theoretically predicted laws. Different
turbulent spectra are considered.Comment: 8 pages, REVTEX, 6 postscript figures included. To appear in Phys.
Fluids (1997
Jet precession in the active nucleus of M81. Ongoing VLBI monitoring
In a recent publication, we reported results of a multi-frequency VLBI
campaign of observations of the Active Galactic Nucleus (AGN) in galaxy M\,81,
phase-referenced to the supernova SN\,1993J. We were able to extract precise
information on the relative astrometry of the AGN radio emission at different
epochs and frequencies. We found strong evidence of precession in the AGN jet
(i.e., a systematic evolution in the jet inclination at each frequency) coupled
to changes in the overall flux density at the different frequencies. In these
proceedings, we summarise the main contents of our previous publication and we
report on (preliminary) new results from our follow-up VLBI observations, now
phase-referenced to the young supernova SN2008iz. We also briefly discuss how
these results match the picture of our previously-reported precession model.Comment: 6 pages, 3 figures. Proceedings of EVN meeting 201
Langevin approach to generate synthetic turbulence
We present an analytical scheme, easily implemented numerically, to generate
synthetic Gaussian turbulent flows by using a linear Langevin equation, where
the noise term acts as a stochastic stirring force. The characteristic
parameters of the velocity field are well introduced, in particular the
kinematic viscosity and the spectrum of energy. As an application, the
diffusion of a passive scalar is studied for two different energy spectra.
Numerical results are compared favorably with analytical calculations.Comment: 7 pages, REVTEX, 6 figures. To appear in Physics of Fluids (April
1997
Solving the polarization problem in ALMA-VLBI observations
The Atacama Large mm-submm Array (ALMA) is, by far, the most sensitive
mm/submm telescope in the World. The ALMA Phasing Project (APP) will allow us
to phase-up all the ALMA antennas and use them as one single VLBI station. This
will be a key component of the Event Horizon Telescope (EHT), a Global VLBI
array at millimeter wavelengths. A problem in the APP is the calibration and
conversion of the polarization channels. Most VLBI stations record their
signals in a circular basis, but the ALMA receivers record in a linear basis.
The strategy that will be followed in the phased-ALMA VLBI observations will be
to correlate in "mixed" basis (i.e., linear versus circular) and convert the
visibilities to a pure circular basis after the correlation. We have developed
an algorithm to perform such a polarization conversion of the VLBI
visibilities. In these proceedings, we present the basics of the PolConvert
algorithm and discuss on the polarization conversion in the general case were
single dishes (besides phased arrays) record with linear receivers in VLBI
observations. We show some results of PolConvert applied to realistic
simulations, as well as a test with real VLBI observations at 86\,GHz between
the Onsala radiotelescope (recording in linear basis) and the Effelsberg
radiotelescope (recording in circular basis).Comment: To appear in the Proceedings of the 12th European VLBI Network
Symposium (7-10 Oct 2014, Cagliary, Italy
Deep Infrared Imaging of the Microquasars 1E1740-2942 and GRS 1758-258
We present deep infrared (m) imaging of the Galactic microquasars
1E1740-2942 and GRS 1758-258 using the Keck-I 10-meter telescope in June 1998.
The observations were taken under excellent seeing conditions (\sim 0.45
\arcsec full-width half-maximum), making them exceptionally deep for these
crowded fields. We used the USNO-A2.0 catalog to astrometrically calibrate the
infrared images (along with an optical CCD image in the case of GRS 1758-258),
providing independent frame ties to the known radio positions of the objects.
For 1E1740-2942, we confirm potential candidates for the microquasar previously
identified by Marti et al., and show that none of the objects near the
microquasar have varied significantly from 1998 to 1999. For GRS 1758-258, our
astrometry indicates a position shifted from previous reports of candidates for
the microquasar. We find no candidates inside our 90% confidence radius to a limiting magnitude of mag. We discuss the implications of
these results for the nature of the microquasar binary systems.Comment: To appear in the Astrophysical Journal; 15 pages, including 4 figure
RAM: A Relativistic Adaptive Mesh Refinement Hydrodynamics Code
We have developed a new computer code, RAM, to solve the conservative
equations of special relativistic hydrodynamics (SRHD) using adaptive mesh
refinement (AMR) on parallel computers. We have implemented a
characteristic-wise, finite difference, weighted essentially non-oscillatory
(WENO) scheme using the full characteristic decomposition of the SRHD equations
to achieve fifth-order accuracy in space. For time integration we use the
method of lines with a third-order total variation diminishing (TVD)
Runge-Kutta scheme. We have also implemented fourth and fifth order Runge-Kutta
time integration schemes for comparison. The implementation of AMR and
parallelization is based on the FLASH code. RAM is modular and includes the
capability to easily swap hydrodynamics solvers, reconstruction methods and
physics modules. In addition to WENO we have implemented a finite volume module
with the piecewise parabolic method (PPM) for reconstruction and the modified
Marquina approximate Riemann solver to work with TVD Runge-Kutta time
integration. We examine the difficulty of accurately simulating shear flows in
numerical relativistic hydrodynamics codes. We show that under-resolved
simulations of simple test problems with transverse velocity components produce
incorrect results and demonstrate the ability of RAM to correctly solve these
problems. RAM has been tested in one, two and three dimensions and in
Cartesian, cylindrical and spherical coordinates. We have demonstrated
fifth-order accuracy for WENO in one and two dimensions and performed detailed
comparison with other schemes for which we show significantly lower convergence
rates. Extensive testing is presented demonstrating the ability of RAM to
address challenging open questions in relativistic astrophysics.Comment: ApJS in press, 21 pages including 18 figures (6 color figures
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