4,558 research outputs found
Radio polarization maps of shell-type SNRs II. Sedov models with evolution of turbulent magnetic field
Polarized radio emission has been mapped with great detail in several
Galactic supernova remnants (SNRs), but has not yet been exploited to the
extent it deserves. We have developed a method to model maps of the Stokes
parameters for shell-like SNRs during their Sedov evolution phase. At first,
3-dimensional structure of a SNR has been computed, by modeling the
distribution of the magnetohydrodynamic parameters and of the accelerated
particles. The generation and dissipation of the turbulent component of
magnetic field everywhere in SNR are also considered taking into account its
interaction with accelerated particles. Then, in order to model the emission,
we have used a generalization of the classical synchrotron theory, valid for
the case in which the magnetic field has ordered and disordered components.
Finally, 2-dimensional projected maps have been derived, for different
orientations of SNR and of interstellar magnetic field with respect to the
observer. An important effect to consider is the Faraday rotation of the
polarization planes inside the SNR interior. In this paper we present details
of the model, and describe general properties of the images.Comment: accepted in MNRA
Repair Expenses, Selling Contracts, and House Prices
This paper examines the impact of repair expenses on the selling price of a house. Using data from settlement statements, we investigate the frequency and extent to which performance of major repairs is part of the sales contract. We find that most homes are restored to a "normally maintained" state each time the home changes hands, and that the cost of bringing the home to this condition is included as part of house selling price. This implies it may be unnecessary to measure maintenance levels when using transaction data to study components of house price or to construct house price indexes.
Designing a sustainable university recharge area for electric vehicles: Technical and economic analysis
This article addresses the technical and economic challenges regarding the design of a "green" recharge area for electric vehicles at the University of Palermo in order to reduce costs and pollution connected to the charging process. Based on the behaviour of the student population, the electrical load is identified and two possible solutions are evaluated to manage the peak load: an orientation of the panels increasing the power at defined time and the use of a storage system. The main strength and weakness points of two systems are investigated by taking into account the Levelized Cost of Energy (LCOE), which reaches 75.3 \u20ac/MWh for the orientation of panel and 103 \u20ac/MWh for the storage system. Furthermore, the cost of the topologies of power plant and the cost of energy are discussed in depth
Modeling non-thermal emission from stellar bow shocks
Runaway O- and early B-type stars passing throughout the interstellar medium
at supersonic velocities and characterized by strong stellar winds may produce
bow shocks that can serve as particle acceleration sites. Previous theoretical
models predict the production of high energy photons by non-thermal radiative
processes, but their efficiency is still debated. We aim to test and explain
the possibility of emission from the bow shocks formed by runaway stars
traveling through the interstellar medium by using previous theoretical models.
We apply our model to AE Aurigae, the first reported star with an X-ray
detected bow shock, to BD+43 3654, in which the observations failed in
detecting high energy emission, and to the transition phase of a supergiant
star in the late stages of its life.From our analysis, we confirm that the
X-ray emission from the bow shock produced by AE Aurigae can be explained by
inverse Compton processes involving the infrared photons of the heated dust. We
also predict low high energy flux emission from the bow shock produced by BD+43
3654, and the possibility of high energy emission from the bow shock formed by
a supergiant star during the transition phase from blue to red supergiant.Bow
shock formed by different type of runaway stars are revealed as a new possible
source of high energy photons in our neighbourhood
Redshifted X-rays from the material accreting onto TW Hya: evidence of a low-latitude accretion spot
High resolution spectroscopy, providing constraints on plasma motions and
temperatures, is a powerful means to investigate the structure of accretion
streams in CTTS. In particular, the accretion shock region, where the accreting
material is heated to temperatures of a few MK as it continues its inward bulk
motion, can be probed by X-ray spectroscopy. To attempt to detect for the first
time the motion of this X-ray-emitting post-shock material, we searched for a
Doppler shift in the deep Chandra/HETGS observation of the CTTS TW Hya. This
test should unveil the nature of this X-ray emitting plasma component in CTTS,
and constrain the accretion stream geometry. We searched for a Doppler shift in
the X-ray emission from TW Hya with two different methods, by measuring the
position of a selected sample of emission lines, and by fitting the whole TW
Hya X-ray spectrum, allowing the line-of-sight velocity to vary. We found that
the plasma at T~2-4 MK has a line-of-sight velocity of 38.3+/-5.1 km/s with
respect to the stellar photosphere. This result definitively confirms that this
X-ray-emitting material originates in the post-shock region, at the base of the
accretion stream, and not in coronal structures. The comparison of the observed
velocity along the line of sight, 38.3+/-5.1 km/s, with the inferred intrinsic
velocity of the post shock of TW Hya, v_post~110-120 km/s, indicates that the
footpoints of the accretion streams on TW Hya are located at low latitudes on
the stellar surface. Our results indicate that complex magnetic field
geometries, such as that of TW Hya, permit low-latitude accretion spots.
Moreover, since on TW Hya the redshift of the soft X-ray emission is very
similar to that of the narrow component of the CIV resonance doublet at 1550
Ang, as found by Ardila et al. (2013), then the plasma at 2-4 MK and that at
0.1 MK likely originate in the same post-shock regions.Comment: Accepted for publication in Astronomy & Astrophysics; 2nd version
after language editor corrections; 16 pages, 8 figures, 6 table
Nanoflare Evidence from Analysis of the X-Ray Variability of an Active Region Observed with Hinode/XRT
The heating of the solar corona is one of the big questions in astrophysics.
Rapid pulses called nanoflares are among the best candidate mechanisms. The
analysis of the time variability of coronal X-ray emission is potentially a
very useful tool to detect impulsive events. We analyze the small-scale
variability of a solar active region in a high cadence Hinode/XRT observation.
The dataset allows us to detect very small deviations of emission fluctuations
from the distribution expected for a constant rate. We discuss the deviations
in the light of the pulsed-heating scenario.Comment: 6 pages, 4 figure
A General Mathematical Formulation for the Determination of Differential Leakage Factors in Electrical Machines with Symmetrical and Asymmetrical Full or Dead-Coil Multiphase Windings
This paper presents a simple and general mathematical formulation for the determination of the differential leakage factor for both symmetrical and asymmetrical full and dead-coil windings of electrical machines. The method can be applied to all multiphase windings and considers Görges polygons in conjunction with masses geometry in order to find an easy and affordable way to compute the differential leakage factor, avoiding the adoption of traditional methods that refer to the Ossanna's infinite series, which has to be obviously truncated under the bound of a predetermined accuracy. Moreover, the method described in this paper allows the easy determination of both the minimum and maximum values of the differential leakage factor, as well as its average value and the time trend. The proposed method, which does not require infinite series, is validated by means of several examples in order to practically demonstrate the effectiveness and the easiness of application of this procedure
Formation of X-ray emitting stationary shocks in magnetized protostellar jets
X-ray observations of protostellar jets show evidence of strong shocks
heating the plasma up to temperatures of a few million degrees. In some cases,
the shocked features appear to be stationary. They are interpreted as shock
diamonds. We aim at investigating the physics that guides the formation of
X-ray emitting stationary shocks in protostellar jets, the role of the magnetic
field in determining the location, stability, and detectability in X-rays of
these shocks, and the physical properties of the shocked plasma. We performed a
set of 2.5-dimensional magnetohydrodynamic numerical simulations modelling
supersonic jets ramming into a magnetized medium and explored different
configurations of the magnetic field. The model takes into account the most
relevant physical effects, namely thermal conduction and radiative losses. We
compared the model results with observations, via the emission measure and the
X-ray luminosity synthesized from the simulations. Our model explains the
formation of X-ray emitting stationary shocks in a natural way. The magnetic
field collimates the plasma at the base of the jet and forms there a magnetic
nozzle. After an initial transient, the nozzle leads to the formation of a
shock diamond at its exit which is stationary over the time covered by the
simulations (~ 40 - 60 yr; comparable with time scales of the observations).
The shock generates a point-like X-ray source located close to the base of the
jet with luminosity comparable with that inferred from X-ray observations of
protostellar jets. For the range of parameters explored, the evolution of the
post-shock plasma is dominated by the radiative cooling, whereas the thermal
conduction slightly affects the structure of the shock.Comment: Accepted for publication in Astronomy and Astrophysic
A physical interpretation of the jet-like X-ray emission from supernova remnant W49B
In the framework of the study of supernova remnants and their complex
interaction with the interstellar medium and the circumstellar material, we
focus on the galactic supernova remnant W49B. Its morphology exhibits an X-ray
bright elongated nebula, terminated on its eastern end by a sharp perpendicular
structure aligned with the radio shell. The X-ray spectrum of W49B is
characterized by strong K emission lines from Si, S, Ar, Ca, and Fe. There is a
variation of the temperature in the remnant with the highest temperature found
in the eastern side and the lowest one in the western side. The analysis of the
recent observations of W49B indicates that the remnant may be the result of an
asymmetric bipolar explosion where the ejecta are collimated along a jet-like
structure and the eastern jet is hotter and more Fe-rich than the western one.
Another possible scenario associates the X-ray emission with a spherical
explosion where parts of the ejecta are interacting with a dense belt of
ambient material. To overcome this ambiguity we present new results of the
analysis of an XMM-Newton observation and we perform estimates of the mass and
energy of the remnant. We conclude that the scenario of an anisotropic jet-like
explosion explains quite naturally our observation results, but the association
of W49B with a hypernova and a gamma-ray burst, although still possible, is not
directly supported by any evidence.Comment: 7 pages, 5 figures, accepted for publication in Advances in Space
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