330 research outputs found
Semilogarithmic Nonuniform Vector Quantization of Two-Dimensional Laplacean Source for Small Variance Dynamics
In this paper high dynamic range nonuniform two-dimensional vector quantization model for Laplacean source was provided. Semilogarithmic A-law compression characteristic was used as radial scalar compression characteristic of two-dimensional vector quantization. Optimal number value of concentric quantization domains (amplitude levels) is expressed in the function of parameter A. Exact distortion analysis with obtained closed form expressions is provided. It has been shown that proposed model provides high SQNR values in wide range of variances, and overachieves quality obtained by scalar A-law quantization at same bit rate, so it can be used in various switching and adaptation implementations for realization of high quality signal compression
Effects of disc midplane evolution on CO snowline location
Temperature changes in the planet forming disc midplanes carry important physico-chemical consequences, such as the effect on the locations of the condensation fronts of molecules - the snowlines. Snowlines impose major chemical gradients and possibly foster grain growth. The aim of this paper is to understand how disc midplane temperature changes with gas and dust evolution, and identify trends that may influence planet formation or allow to constrain disc evolution observationally. We calculate disc temperature, hydrostatic equilibrium and dust settling in a mutually consistent way from a grid of disc models at different stages of gas loss, grain growth and hole opening. We find that the CO snowline location depends very strongly on disc properties. The CO snowline location migrates closer to the star for increasing degrees of gas dispersal and dust growth. Around a typical A type star, the snowline can be anywhere between several tens and a few hundred au, depending on the disc properties such as gas mass and grain size. In fact, gas loss is as efficient as dust evolution in settling discs, and flat discs may be gas-poor counterparts of flared discs. Our results, in the context of different pre-main sequence evolution of the luminosity in low- and intermediate-mass stars suggests very different thermal (and hence chemical) histories in these two types of discs. Discs of T Tauri stars settle and cool down while discs of Herbig Ae stars may remain rather warm throughout the pre-main sequence
Probing the radial temperature structure of protoplanetary disks with Herschel/HIFI
Herschel/HIFI spectroscopic observations of CO J=10-9, CO J=16-15 and [CII]
towards HD 100546 are presented. The objective is to resolve the velocity
profile of the lines to address the emitting region of the transitions and
directly probe the distribution of warm gas in the disk. The spectra reveal
double-peaked CO line profiles centered on the systemic velocity, consistent
with a disk origin. The J=16-15 line profile is broader than that of the J=10-9
line, which in turn is broader than those of lower J transitions (6-5, 3-2,
observed with APEX), thus showing a clear temperature gradient of the gas with
radius. A power-law flat disk model is used to fit the CO line profiles and the
CO rotational ladder simultaneously, yielding a temperature of T_0=1100 \pm 350
K (at r_0 = 13 AU) and an index of q=0.85 \pm 0.1 for the temperature radial
gradient. This indicates that the gas has a steeper radial temperature gradient
than the dust (mean q_{dust} ~ 0.5), providing further proof of the thermal
decoupling of gas and dust at the disk heights where the CO lines form. The
[CII] line profile shows a strong single-peaked profile red-shifted by 0.5 km
s-1 compared to the systemic velocity. We conclude that the bulk of the [CII]
emission has a non-disk origin (e.g., remnant envelope or diffuse cloud).Comment: Accepted for publication in ApJ
Acute coronary syndrome in diclofenac sodium-induced type I hypersensitivity reaction : Kounis syndrome
Drug-induced type I hypersensitivity reactions are frequent. Sometimes, acute coronary syndrome (ACS) can be registered in such patients, which may have a serious impact on the course and management of the allergic reaction. Because of potentially atypical ACS clinical presentations, the ECG is an obligatory diagnostic tool in any allergic reaction. Coronary artery spasm is the pathophysiological basis of ACS, triggered by the action of potent vasoactive mediators (histamine, neutral proteases, arachidonic acid products) released from the cells involved in type I hypersensitivity. Allergic angina and allergic myocardial infarction are referred to as Kounis Syndrome. We describe herein a case of ACS in a patient with registered systemic immediate hypersensitivity reaction which developed following the muscular administration of diclofenac sodium.peer-reviewe
Resolving HD 100546 disc in the mid-infrared: Small inner disc and asymmetry near the gap
A region of roughly half of the solar system scale around the star HD 100546
is largely cleared of gas and dust, in contrast to the bright outer disc.
However, some material is observed in the immediate vicinity of the star. We
investigate how the dust is distributed within and outside the gap, and
constrain the disc geometry with mid-infrared interferometric observations
using VLTI/MIDI. With baseline lengths of 40m, our long baseline observations
are sensitive to the inner few AU from the star, and we combined them with
observations at shorter, 15m baselines, to probe emission beyond the gap at up
to 20AU from the star. We modelled the mid-infrared emission using radial
temperature profiles. Our model is composed of infinitesimal concentric annuli
emitting as black bodies, and it has distinct inner and outer disc components.
We derived an upper limit of 0.7AU for the radial size of the inner disc, from
our longest baseline data. This small dusty disc is separated from the edge of
the outer disc by a large, roughly 10AU wide gap. Our short baseline data place
a bright ring of emission at 11+-1AU, consistent with prior observations of the
transition region between the gap and the outer disc, known as the disc wall.
The inclination and position angle are constrained by our data to i=53+-8deg
and PA=145+-5deg. Compared to the rim and outer disc geometry this suggests
co-planarity. Brightness asymmetry is evident in both short and long baseline
data, and it is unequivocally discernible from any atmospheric or instrumental
effects. The origin of the asymmetry is consistent with the bright disc wall,
which we find to be 1-2AU wide. The gap is cleared of micron-sized dust, but we
cannot rule out the presence of larger particles and/or perturbing bodies.Comment: 12 pages, 9 figures, accepted for publication in A&
Radioactivity Concentrations in Spa Waters - Dose Assessment
In this study 6 different spa water samples from Serbia, Hungary and Czech Republic were investigated in order to determine their radioactivity concentrations. These waters have been used on a large scale for medical and bathing purposes; for therapy, rehabilitation and recreation and also used for drinking, which is the most important. The obtained results showed that natural activity concentrations of alpha emitting radionuclides was within World Health Organization recommended levels and Serbian applicable regulations, but the gross beta activity exceed 1 Bq L-1 for some of the samples. Considering the fact that gross beta activity in four samples was higher than recommended levels, gamma spectrometric measurements were performed, in order to identify radionuclides which caused increase of the gross beta activity. It was found that K-40 was responsible for the elevated gross beta activity. Based on the obtained results the annual effective dose was calculated.3rd International Conference on Radiation and Applications in Various Fields of Research (RAD), Jun 08-12, 2015, Budva, Montenegr
Determining the mid-plane conditions of circumstellar discs using gas and dust modelling: a study of HD 163296
The mass of gas in protoplanetary discs is a quantity of great interest for
assessing their planet formation potential. Disc gas masses are, however,
traditionally inferred from measured dust masses by applying an assumed
standard gas-to-dust ratio of . Furthermore, measuring gas masses
based on CO observations has been hindered by the effects of CO freeze-out.
Here we present a novel approach to study the mid-plane gas by combining
CO line modelling, CO snowline observations and the spectral energy
distribution (SED) and selectively study the inner tens of au where freeze-out
is not relevant. We apply the modelling technique to the disc around the Herbig
Ae star HD 163296 with particular focus on the regions within the CO snowline
radius, measured to be at 90 au in this disc. Our models yield the mass of
CO in this inner disc region of
M. We
find that most of our models yield a notably low , especially in the
disc mid-plane (). Our only models with a more interstellar medium
(ISM)-like require CO to be underabundant with respect to the ISM
abundances and a significant depletion of sub-micron grains, which is not
supported by scattered light observations. Our technique can be applied to a
range of discs and opens up a possibility of measuring gas and dust masses in
discs within the CO snowline location without making assumptions about the
gas-to-dust ratio.This work has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG. DMB is funded by this ERC grant and an STFC studentship. OP is supported by the Royal Society Dorothy Hodgkin Fellowship. During a part of this project OP was supported by the European Union through ERC grant number 279973. TJH is funded by the STFC consolidated grant ST/K000985/1.This is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnras/stw132
Warm molecular gas and kinematics in the disc around HD 100546
The disc around the Herbig Ae/Be star HD 100546 is one of the most
extensively studied discs in the southern sky. Although there is a wealth of
information about its dust content and composition, not much is known about its
gas and large scale kinematics. We detect and study the molecular gas in the
disc at spatial resolution from 7.7" to 18.9" using the APEX telescope. The
lines 12CO J=7-6, J=6-5, J=3-2, 13CO J=3-2 and [C I] 3P2-3P1 are observed,
diagnostic of disc temperature, size, chemistry, and kinematics. We use
parametric disc models that reproduce the low-J 12CO emission from Herbig~Ae
stars and vary the basic disc parameters - temperature, mass and size. Using
the molecular excitation and radiative transfer code RATRAN we fit the observed
spectral line profiles. Our observations are consistent with more than 0.001
Msun of molecular gas in a disc of approximately 400 AU radius in Keplerian
rotation around a 2.5 Msun star, seen at an inclination of 50 degrees. The
detected 12CO lines are dominated by gas at 30-70~K. The non-detection of the
[C I] line indicates excess ultraviolet emission above that of a B9 type model
stellar atmosphere. Asymmetry in the 12CO line emission suggests that one side
of the outer disc is colder by 10-20~K than the other, possibly due to a shadow
by a warped geometry of the inner disc. Pointing offsets, foreground cloud
absorption and asymmetry in the disc extent are excluded scenarios. Efficient
heating of the outer disc ensures that low- and high-J 12CO lines are dominated
by the outermost disc regions, indicating a 400 AU radius. The 12CO J=6--5 line
arises from a disc layer higher above disc midplane, and warmer by 15-20~K than
the layer emitting the J=3--2 line. The existing models of discs around Herbig
Ae stars, assuming a B9.5 type model stellar atmosphere overproduce the [CI]
3P2--3P1 line intensity from HD 100546 by an order of magnitude.Comment: 9pages, 3figures, Accepted for publication in Astronomy &
Astrophysic
Radiation thermo-chemical models of protoplanetary disks II. Line diagnostics
Methods. We use the recently developed disk code ProDiMo to calculate the
physico-chemical structure of protoplanetary disks and apply the Monte-Carlo
line radiative transfer code RATRAN to predict observable line profiles and
fluxes. We consider a series of Herbig Ae type disk models ranging from 10^-6
M_Sun to 2.2 10^-2 M_Sun (between 0.5 and 700 AU) to discuss the dependency of
the line fluxes and ratios on disk mass for otherwise fixed disk parameters.
Results. We find the [CII] 157.7 mum line to originate in LTE from the surface
layers of the disk, where Tg > Td . The total emission is dominated by surface
area and hence depends strongly on disk outer radius. The [OI] lines can be
very bright (> 10^-16 W/m^2) and form in slightly deeper and closer regions
under non-LTE conditions. The high-excitation [OI] 145.5 mum line, which has a
larger critical density, decreases more rapidly with disk mass than the 63.2
mum line. Therefore, the [OI] 63.2 mum/145.5 mum ratio is a promising disk mass
indicator, especially as it is independent of disk outer radius for Rout > 200
AU. CO is abundant only in deeper layers A_V >~ 0.05. For too low disk masses
(M_disk <~10^-4 M_Sun) the dust starts to become transparent, and CO is almost
completely photo-dissociated. For masses larger than that the lines are an
excellent independent tracer of disk outer radius and can break the outer
radius degeneracy in the [OI] 63.2 mum/[CII]157.7 mum line ratio. Conclusions.
The far-IR fine-structure lines of [CII] and [OI] observable with Herschel
provide a promising tool to measure the disk gas mass, although they are mainly
generated in the atomic surface layers. In spatially unresolved observations,
none of these lines carry much information about the inner, possibly hot
regions < 30 AU.Comment: accepted for publication in A&
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