40,512 research outputs found
Spectral Models of Convection-Dominated Accretion Flows
For small values of the dimensionless viscosity parameter, namely
, the dynamics of non-radiating accretion flows is
dominated by convection; convection strongly suppresses the accretion of matter
onto the central object and transports a luminosity from small to large radii in the flow. A fraction of this convective
luminosity is likely to be radiated at large radii via thermal bremsstrahlung
emission. We show that this leads to a correlation between the frequency of
maximal bremsstrahlung emission and the luminosity of the source, . Accreting black holes with X-ray luminosities are expected to
have hard X-ray spectra, with photon indices , and sources with
are expected to have soft spectra, with
. This is testable with {\it Chandra} and {\it XMM}.Comment: final version accepted by ApJ; significant modifications from
previous versio
Properties of Intercalated 2H-NbSe2, 4Hb-TaS2 and 1T-TaS2
The layered compounds 2H-NbSe, 24Hb-TaS, 2and 1T-TaS2 have been intercalated with organic molecules; and the resulting crystal structure, heat capacity, conductivity, and superconductivity have been studied. The coordination in the disulfide layers was found to be unchanged in the product phase. Resistance minima appear and the superconducting transition temperature is reduced in the NbSe2 complex. Conversely, superconductivity is induced in the 4Hb-TaS2 complex. Corresponding evidence of a large change of the density of states, negative for 2H-NbSe2 and positive for 4Hb-TaS2, was also observed upon intercalation. The transport properties of all the intercalation complexes show a pronounced dependence upon the coordination of the transition metal
A Comparison and Strategy of Semantic Segmentation on Remote Sensing Images
In recent years, with the development of aerospace technology, we use more
and more images captured by satellites to obtain information. But a large
number of useless raw images, limited data storage resource and poor
transmission capability on satellites hinder our use of valuable images.
Therefore, it is necessary to deploy an on-orbit semantic segmentation model to
filter out useless images before data transmission. In this paper, we present a
detailed comparison on the recent deep learning models. Considering the
computing environment of satellites, we compare methods from accuracy,
parameters and resource consumption on the same public dataset. And we also
analyze the relation between them. Based on experimental results, we further
propose a viable on-orbit semantic segmentation strategy. It will be deployed
on the TianZhi-2 satellite which supports deep learning methods and will be
lunched soon.Comment: 8 pages, 3 figures, ICNC-FSKD 201
Low heat conduction in white dwarf boundary layers?
X-ray spectra of dwarf novae in quiescence observed by Chandra and XMM-Newton
provide new information on the boundary layers of their accreting white dwarfs.
Comparison of observations and models allows us to extract estimates for the
thermal conductivity in the accretion layer and reach conclusions on the
relevant physical processes. We calculate the structure of the dense thermal
boundary layer that forms under gravity and cooling at the white dwarf surface
on accretion of gas from a hot tenuous ADAF-type coronal inflow. The
distribution of density and temperature obtained allows us to calculate the
strength and spectrum of the emitted X-ray radiation. They depend strongly on
the values of thermal conductivity and mass accretion rate. We apply our model
to the dwarf nova system VW Hyi and compare the spectra predicted for different
values of the thermal conductivity with the observed spectrum. We find a
significant deviation for all values of thermal conductivity that are a sizable
fraction of the Spitzer conductivity. A good fit arises however for a
conductivity of about 1% of the Spitzer value. This also seems to hold for
other dwarf nova systems in quiescence. We compare this result with thermal
conduction in other astrophysical situations. The highly reduced thermal
conductivity in the boundary layer requires magnetic fields perpendicular to
the temperature gradient. Locating their origin in the accretion of magnetic
fields from the hot ADAF-type coronal flow we find that dynamical effects of
these fields will lead to a spatially intermittent, localized accretion
geometry at the white dwarf surface.Comment: 8 pages, 5 figs, to appear in Astronomy & Astrophysic
Radioactivity and Electron Acceleration in Supernova Remnants
We argue that the decays of radioactive nuclei related to Ti and
Ni ejected during supernova explosions can provide a vast pool of mildly
relativistic positrons and electrons which are further accelerated to
ultrarelativistic energies by reverse and forward shocks. This interesting link
between two independent processes - the radioactivity and the particle
acceleration - can be a clue for solution of the well known theoretical problem
of electron injection in supernova remnants. In the case of the brightest radio
source Cas A, we demonstrate that the radioactivity can supply adequate number
of energetic electrons and positrons for interpretation of observational data
provided that they are stochastically pre-accelerated in the upstream regions
of the forward and reverse shocks.Comment: 6 pages, 1 figure, revised version accepted to Phys.Rev.
Measurement of Partial-Wave Contributions in pp --> pp pi^0
We report a measurement of the spin-dependent total cross section ratios
delta_sigma_T/sigma_tot and delta_sigma_L/sigma_tot of the pp --> pp pi^0
reaction between 325 MeV and 400 MeV. The experiment was carried out with a
polarized internal target in a storage ring. Non-vertical beam polarization was
obtained by the use of solenoidal spin rotators. Near threshold, the knowledge
of both spin-dependent total cross sections is sufficient to deduce the
strength of certain participating partial waves, free of any model.Comment: 6 pages, 4 figure
High efficiency of soft X-ray radiation reprocessing in supersoft X-ray sources due to multiple scattering
Detailed analysis of the lightcurve of CAL 87 clearly has shown that the high
optical luminosity comes from the accretion disc rim and can only be explained
by a severe thickening of the disc rim near the location where the accretion
stream impinges. This area is irradiated by the X-rays where it faces the white
dwarf. Only if the reprocessing rate of X-rays to optical light is high a
luminosity as high as observed can be understood. But a recent detailed study
of the soft X-ray radiation reprocessing in supersoft X-ray sources has shown
that the efficiency is not high enough. We here propose a solution for this
problem. As already discussed in the earlier lightcurve analysis the impact of
the accretion stream at the outer disc rim produces a ``spray'', consisting of
a large number of individual gas blobs imbedded in a surrounding corona. For
the high mass flow rate this constitutes an optically thick vertically extended
screen at the rim of the accretion disc. We analyse the optical properties of
this irradiated spray and find that the multiple scattering between these gas
blobs leads to an effective reprocessing of soft X-rays to optical light as
required by the observations.Comment: 7 pages, 6 figures, accepted for publication in A&
The Formation of the First Stars II. Radiative Feedback Processes and Implications for the Initial Mass Function
We consider the radiative feedback processes that operate during the
formation of the first stars, including the photodissociation of H_2, Ly-alpha
radiation pressure, formation and expansion of an HII region, and disk
photoevaporation. These processes may inhibit continued accretion once the
stellar mass has reached a critical value, and we evaluate this mass separately
for each process. Photodissociation of H_2 in the local dark matter minihalo
occurs relatively early in the growth of the protostar, but we argue this does
not affect subsequent accretion since by this time the depth of the potential
is large enough for accretion to be mediated by atomic cooling. However,
neighboring starless minihalos can be affected. Ionization creates an HII
region in the infalling envelope above and below the accretion disk. Ly-alpha
radiation pressure acting at the boundary of the HII region is effective at
reversing infall from narrow polar directions when the star reaches ~20-30Msun,
but cannot prevent infall from other directions. Expansion of the HII region
beyond the gravitational escape radius for ionized gas occurs at masses
~50-100Msun, depending on the accretion rate and angular momentum of the
inflow. However, again, accretion from the equatorial regions can continue
since the neutral accretion disk has a finite thickness and shields a
substantial fraction of the accretion envelope from direct ionizing flux. At
higher stellar masses, ~140Msun in the fiducial case, the combination of
declining accretion rates and increasing photoevaporation-driven mass loss from
the disk act to effectively halt the increase in the protostellar mass. We
identify this process as the mechanism that terminates the growth of Population
III stars... (abridged)Comment: 31 pages, including 10 figures, accepted to Ap
Electronic correlations in vanadium chalcogenides: BaVSe3 versus BaVS3
Albeit structurally and electronically very similar, at low temperature the
quasi-one-dimensional vanadium sulfide BaVS3 shows a metal-to-insulator
transition via the appearance of a charge-density-wave state, while BaVSe3
apparently remains metallic down to zero temperature. This different behavior
upon cooling is studied by means of density functional theory and its
combination with the dynamical mean-field theory and the rotationally-invariant
slave-boson method. We reveal several subtle differences between these
chalcogenides that provide indications for the deviant behavior of BaVSe3 at
low temperature. In this regard, a smaller Hubbard U in line with an increased
relevance of the Hund's exchange J plays a vital role.Comment: 16 pages, 11 figures, published versio
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