67 research outputs found
Simultaneous solution of Kompaneets equation and Radiative Transfer equation in the photon energy range 1 - 125 KeV
Radiative transfer equation in plane parallel geometry and Kompaneets
equation is solved simultaneously to obtain theoretical spectrum of 1-125 KeV
photon energy range. Diffuse radiation field is calculated using
time-independent radiative transfer equation in plane parallel geometry, which
is developed using discrete space theory (DST) of radiative transfer in a
homogeneous medium for different optical depths. We assumed free-free emission
and absorption and emission due to electron gas to be operating in the medium.
The three terms and where is photon phase density and , in Kompaneets equation and those due to
free-free emission are utilized to calculate the change in the photon phase
density in a hot electron gas. Two types of incident radiation are considered:
(1) isotropic radiation with the modified black body radiation [1] and
(2) anisotropic radiation which is angle dependent. The emergent radiation at
and reflected radiation are calculated by using the
diffuse radiation from the medium. The emergent and reflected radiation contain
the free-free emission and emission from the hot electron gas. Kompaneets
equation gives the changes in photon phase densities in different types of
media. Although the initial spectrum is angle dependent, the Kompaneets
equation gives a spectrum which is angle independent after several Compton
scattering times.Comment: 31 pages, 8 figures, Accepte
Effects of Dust Scattering in Expanding Spherical Nebulae
The mean intensity of planetary nebulae with an expanding atmosphere is
modeled by considering dusty and dust-free atmospheres. The bulk matter density
is determined from the adopted velocity field through the equation of
continuity. The gas is assumed to consist of hydrogen and helium and the
gas-to-dust mass ratio is taken to be . The Rayleigh phase
function is employed for atomic scattering while the full Mie theory of
scattering is incorporated for determining the dust scattering and absorption
cross-section as well as the phase function for the angular distribution of
photons after scattering. It is shown that in a dust free atmosphere, the mean
intensity increases with the increase in the expansion velocity that makes the
medium diluted. The mean intensity profile changes significantly when dust
scattering is incorporated. The increase in forward scattering of photons by
the dust particles yields into an increase in the mean intensity as compared to
that without dust. The mean intensity increases as the particle size is
increased. Thus it is shown that both the expansion of the medium and the
presence of dust play important role in determining the mean intensity of a
planetary nebulae.Comment: 18 pages, Elseveir style (cls file included), 5 postscript figures,
Accepted for publication in New Astronom
Radiative transfer in a spherical, emitting, absorbing and anisotropically scattering medium
The atmospheres of planets (including Earth) and the outer layers of stars
have often been treated in radiative transfer as plane-parallel media, instead
of spherical shells, which can lead to inaccuracy, e.g. limb darkening. We give
an exact solution of the radiative transfer specific intensity at all points
and directions in a finite spherical medium having arbitrary radial spectral
distribution of: source (temperature), absorption, emission and anisotropic
scattering. The power and efficiency of the method stems from the spherical
numerical gridding used to discretize the transfer equations prior to matrix
solution: the wanted ray and the rays which scatter into it both have the same
physico-geometric structure. Very good agreement is found with an isotropic
astrophysical benchmark (Avrett & Loeser, 1984). We introduce a specimen
arbitrary forward-back-side phase scattering function for future comparisons.
Our method directly and exactly addresses spherical symmetry with anisotropic
scattering, and could be used to study the Earth's climate, nuclear power
(neutron diffusion) and the astrophysics of stars and planets.Comment: 8 pages, 2 figures, spherical radiative transfer: stellar, planetary,
terrestia
Preconditioned Bi-Conjugate Gradient Method for Radiative Transfer in Spherical Media
A robust numerical method called the Preconditioned Bi-Conjugate Gradient
(Pre-BiCG)method is proposed for the solution of radiative transfer equation in
spherical geometry.A variant of this method called Stabilized Preconditioned
Bi-Conjugate Gradient (Pre-BiCG-STAB) is also presented. These are iterative
methods based on the construction of a set of bi-orthogonal vectors. The
application of Pre-BiCG method in some benchmark tests show that the method is
quite versatile, and can handle hard problems that may arise in astrophysical
radiative transfer theory.Comment: 19 pages, 12 figure
Sunyaev-Zel'dovich Effect by Multiple Sctattering : Numerical Solution of the Transfer Equations
The radiative transfer equations for multiple inverse Compton scattering of
the Cosmic Microwave Background Radiation (CMBR) by the hot intra-cluster
electrons are solved numerically. The spherical isothermal and inhomogeneous
model has been considered for the electron distribution. The anisotropy
of the CMBR caused by scattering, known as thermal Sunyaev-Zel'dovich effect,
along the radial axis of the medium is compared with the analytical solution of
Kompaneets equation. The X-ray data of several clusters of galaxies at low
redshifts provide an estimation of the central electron density to be of
the order . It is found that for this value of the effect of
multiple scattering is negligible. The numerically calculated anisotropy along
the radial axis matches well with the analytical solution that describes single
scattering. The result incorporating multiple scattering is fitted with the
recent observation of Sunyaev-Zel'dovich effect in the cluster Abell 2163. It
is shown that if is greater by an order of magnitude, which could be
possible for cluster of galaxies at comparatively higher redshift, multiple
scattering would play a significant role at the Wien region of the anisotropy
spectrum. A fitting formula for the correction to the Sunyaev-Zel'dovich effect
due to multiple scattering is provided.Comment: 9 pages, Latex, ws-ijmpa style (cls file included), 3 postscript
figures, Accepted for publication by International Journal of Modern Physics
A method to simulate inhomogeneously irradiated objects with a superposition of 1D models
In close binary systems the atmosphere of one or both components can be
significantly influenced by irradiation from the companion. Often the
irradiated atmosphere is simulated with a single-temperature approximation for
the entire half-sphere. We present a scheme to take the varying irradiation
angle into account by combining several separate 1D models. This is independent
of the actual code which provides the separate stellar spectra. We calculate
the projected area of zones with given irradiation angle and use this
geometrical factor to scale separate 1D models. As an example we calculate two
different irradiation scenarios with the PHOENIX code. The scheme to calculate
the projected area is applicable independent of the physical mechanism that
forms these zones. In the case of irradiation by a primary with T=125000 K, the
secondary forms ions at different ionisation states for different irradiation
angles. No single irradiation angle exists which provides an accurate
description of the spectrum. We show a similar simulation for weaker
irradiation, where the profile of the H line depends on the irradiation
angle.Comment: published in A&
The Maximal Runaway Temperature of Earth-like Planets
We generalize the problem of the semi-gray model to cases in which a
non-negligible fraction of the stellar radiation falls on the long-wavelength
range, and/or that the planetary long-wavelength emission penetrates into the
transparent short wavelength domain of the absorption.
Second, applying the most general assumptions and independently of any
particular properties of an absorber, we show that the greenhouse effect
saturates and any Earth-like planet has a maximal temperature which depends on
the type of and distance to its main-sequence star, its albedo and the primary
atmospheric components which determine the cutoff frequency below which the
atmosphere is optically thick. For example, a hypothetical convection-less
planet similar to Venus, that is optically thin in the visible, could have at
most a surface temperature of 1200-1300K irrespective of the nature of the
greenhouse gas.
We show that two primary mechanisms are responsible for the saturation of the
runaway greenhouse effect, depending on the value of the wavelength above which
the atmosphere becomes optically thick. Unless this wavelength is small and
resides in the optical region, saturation is achieved by radiating the thermal
flux of the planet through the short wavelength tail of the thermal
distribution. This has the observational implication, the radiation from such a
planet should be skewed towards the NIR. Otherwise, saturation takes place by
radiating through windows in the FIR.Comment: 13 pages 14 figure
Periodic variable stars in CoRoT field LRa02 observed with BEST II
The Berlin Exoplanet Search Telescope II (BEST II) is a small wide
field-of-view photometric survey telescope system located at the Observatorio
Cerro Armazones, Chile. The high duty cycle combined with excellent observing
conditions and millimagnitude photometric precision makes this instrument
suitable for ground based support observations for the CoRoT space mission.
Photometric data of the CoRoT LRa02 target field collected between November
2008 and March 2009 were analysed for stellar variability. The presented
results will help in the future analysis of the CoRoT data, particularly in
additional science programs related to variable stars. BEST II observes
selected CoRoT target fields ahead of the space mission. The photometric data
acquired are searched for stellar variability, periodic variable stars are
identified with time series analysis of the obtained stellar light curves. We
obtained the light curves of 104335 stars in the CoRoT LRa02 field over 41
nights. Variability was detected in light curves of 3726 stars of which 350
showed a regular period. These stars are, with the exception of 5 previously
known variable stars, new discoveries.Comment: The figures with light curves can be find in the A&A journal as
online onl
A circular polarimeter for the Cosmic Microwave Background
A primordial degree of circular polarization of the Cosmic Microwave
Background is not observationally excluded. The hypothesis of primordial
dichroism can be quantitatively falsified if the plasma is magnetized prior to
photon decoupling since the initial V-mode polarization affects the evolution
of the temperature fluctuations as well as the equations for the linear
polarization. The observed values of the temperature and polarization angular
power spectra are used to infer constraints on the amplitude and on the
spectral slope of the primordial V-mode. Prior to photon decoupling magnetic
fields play the role of polarimeters insofar as they unveil the circular
dichroism by coupling the V-mode power spectrum to the remaining brightness
perturbations. Conversely, for angular scales ranging between 4 deg and 10 deg
the joined bounds on the magnitude of circular polarization and on the magnetic
field intensity suggest that direct limits on the V-mode power spectrum in the
range of 0.01 mK could directly rule out pre-decoupling magnetic fields in the
range of 10-100 nG. The frequency dependence of the signal is located, for the
present purposes, in the GHz range.Comment: 28 pages, 12 included figures
Time-dependent radio emission from evolving jets
We investigated the time-dependent radiative and dynamical properties of
light supersonic jets launched into an external medium, using hydrodynamic
simulations and numerical radiative transfer calculations. These involved
various structural models for the ambient media, with density profiles
appropriate for galactic and extragalactic systems. The radiative transfer
formulation took full account of emission, absorption, re-emission, Faraday
rotation and Faraday conversion explicitly. High time-resolution intensity maps
were generated, frame-by-frame, to track the spatial hydrodynamical and
radiative properties of the evolving jets. Intensity light curves were computed
via integrating spatially over the emission maps. We apply the models to jets
in active galactic nuclei (AGN). From the jet simulations and the
time-dependent emission calculations we derived empirical relations for the
emission intensity and size for jets at various evolutionary stages. The
temporal properties of jet emission are not solely consequences of intrinsic
variations in the hydrodynamics and thermal properties of the jet. They also
depend on the interaction between the jet and the ambient medium. The
interpretation of radio jet morphology therefore needs to take account of
environmental factors. Our calculations have also shown that the environmental
interactions can affect specific emitting features, such as internal shocks and
hotspots. Quantification of the temporal evolution and spatial distribution of
these bright features, together with the derived relations between jet size and
emission, would enable us to set constraints on the hydrodynamics of AGN and
the structure of the ambient medium.Comment: 16 pages, 18 figures, MNRAS in press
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