11,766 research outputs found
Instructors Learn from Homework, too: Streamlining Data Collection to Facilitate Reteaching Before the Test
Whether it’s for accreditation or simply as a good teaching practice to inform future instruction, gathering and analyzing data can be time consuming. This is especially true for large classes. How can you streamline the process for quick evaluation?https://digitalscholarship.unlv.edu/btp_expo/1011/thumbnail.jp
A numerical simulation of the evolution and fate of a FRI jet. The case of 3C 31
The evolution of FRI jets has been long studied in the framework of the
FRI-FRII dichotomy. In this paper, we test the present theoretical and
observational models via a relativistic numerical simulation of the jets in the
radio galaxy 3C 31. We use the parameters derived from the modelling presented
by \cite{lb02a,lb02b} as input parameters for the simulation of the evolution
of the source, thus assuming that they have not varied over the lifetime of the
source. We simulate about 10 % of the total lifetime of the jets in 3C 31.
Realistic density and pressure gradients for the atmosphere are used. The
simulation includes an equation of state for a two-component relativistic gas
that allows a separate treatment of leptonic and baryonic matter. We compare
our results with the modelling of the observational data of the source. Our
results show that the bow shock evolves self-similarly at a quasi-constant
speed, with slight deceleration by the end of the simulation, in agreement with
recent X-ray observations that show the presence of bow shocks in FRI sources.
The jet expands until it becomes underpressured with respect to the ambient
medium, and then recollimates. Subsequent oscillations around pressure
equilibrium and generation of standing shocks lead to the mass loading and
disruption of the jet flow. We derive an estimate for the minimum age of the
source of , which may imply continuous activity of 3C 31
since the triggering of its activity. The simulation shows that weak CSS
sources may be the young counterparts of FRIs. We conclude that the observed
properties of the jets in 3C 31 are basically recovered by the standing shock
scenario.Comment: Accepted for publication in MNRAS. For better quality figures, please
check http://www.mpifr-bonn.mpg.de/staff/mperucho/Research.htm
Influence of Mechanical Yielding on Predictions of Saturation: The Saturation Line
It is now well accepted that the mechanical and the water retention behaviour of a soil under unsaturated conditions are coupled and, that such coupling, should be incorporated into a constitutive model for a realistic representation of soil’s response. In existing models, the influence of the mechanical behaviour on the water retention is often represented by a shift of the main wetting retention curve to higher values of matric suction (the difference between pore air and pore water pressures) when the specific volume decreases. This means that any variation of total volumetric strains of compression (whether these are elastic or elasto-plastic) will result in a shift of the main wetting and drying curves to the right, when these curves are represented in the water retention plane. This shift of the main water retention curves, however, should not only influence the unsaturated stress states as often described in the literature, it should also have some impact on the saturated stress states and, more specifically, on the predictions of de-saturation (air-entry point) and saturation (air-exclusion point). From a modelling point of view, it is advantageous to represent this influence through the plastic component of volumetric strain of compression only because, in this way, a consistent representation of the mechanical behaviour for both unsaturated and saturated states can be naturally achieved. This and other advantages resulting from this singular approach are demonstrated in the paper in the context of the Glasgow Coupled Model (GCM)
Limit to the radio emission from a putative central compact source in SN1993J
SN1993J in M81 is the best studied young radio-luminous supernova in the
Northern Hemisphere. We recently reported results from the analysis of a
complete set of VLBI observations of this supernova at 1.7, 2.3, 5.0, and 8.4
GHz, covering a time baseline of more than one decade. Those reported results
were focused on the kinematics of the expanding shock, the particulars of its
evolving non-thermal emission, the density profile of the circumstellar medium,
and the evolving free-free opacity by the supernova ejecta. In the present
paper, we complete our analysis by performing a search for any possible signal
from a compact source (i.e., a stellar-mass black hole or a young pulsar
nebula) at the center of the expanding shell. We have performed a stacking of
all our VLBI images at each frequency, after subtraction of our best-fit shell
model at each epoch, and measured the peak intensity in the stacked residual
image. Given the large amount of available global VLBI observations, the
stacking of all the residual images allows us to put upper limits to the
eventual emission of a putative compact central source at the level of
Jy at 5 GHz (or, more conservatively, Jy, if we
make a further correction for the ejecta opacity) and somewhat larger at other
wavelengths.Comment: 4 pages, 3 figures. Accepted for publication in A&
The x-ray corona and jet of cygnus x-1
Evidence is presented indicating that in the hard state of Cygnus X-1, the
coronal mag- netic field might be below equipartition with radiation
(suggesting that the corona is not powered by magnetic field dissipation) and
that the ion temperature in the corona is significantly lower than what
predicted by ADAF like models. It is also shown that the current estimates of
the jet power set interesting contraints on the jet velocity (which is at least
mildly relativistic), the accretion efficiency (which is large in both spectral
states), and the nature of the X-ray emitting region (which is unlikely to be
the jet).Comment: 8 pages, 1 figure. Accepted for publication in Journal of Modern
Physics D, Proceedings of HEPRO II conference, Buenos Aires, Argentina,
October 26-30, 200
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
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