103 research outputs found
The Early Evolution of Massive Stars: Radio Recombination Line Spectra
Velocity shifts and differential broadening of radio recombination lines are
used to estimate the densities and velocities of the ionized gas in several
hypercompact and ultracompact HII regions. These small HII regions are thought
to be at their earliest evolutionary phase and associated with the youngest
massive stars. The observations suggest that these HII regions are
characterized by high densities, supersonic flows and steep density gradients,
consistent with accretion and outflows that would be associated with the
formation of massive stars.Comment: ApJ in pres
A Search for Small-Scale Clumpiness in Dense Cores of Molecular Clouds
We have analyzed HCN(1-0) and CS(2-1) line profiles obtained with high
signal-to-noise ratios toward distinct positions in three selected objects in
order to search for small-scale structure in molecular cloud cores associated
with regions of high-mass star formation. In some cases, ripples were detected
in the line profiles, which could be due to the presence of a large number of
unresolved small clumps in the telescope beam. The number of clumps for regions
with linear scales of ~0.2-0.5 pc is determined using an analytical model and
detailed calculations for a clumpy cloud model; this number varies in the
range: ~2 10^4-3 10^5, depending on the source. The clump densities range from
~3 10^5-10^6 cm^{-3}, and the sizes and volume filling factors of the clumps
are ~(1-3) 10^{-3} pc and ~0.03-0.12. The clumps are surrounded by inter-clump
gas with densities not lower than ~(2-7) 10^4 cm^{-3}. The internal thermal
energy of the gas in the model clumps is much higher than their gravitational
energy. Their mean lifetimes can depend on the inter-clump collisional rates,
and vary in the range ~10^4-10^5 yr. These structures are probably connected
with density fluctuations due to turbulence in high-mass star-forming regions.Comment: 23 pages including 4 figures and 4 table
Chemical modeling of Infrared Dark Clouds: the Role of Surface Chemistry
We simulate the chemistry of infrared dark clouds (IRDCs) with a model in
which the physical conditions are homogeneous and time-independent. The
chemistry is solved as a function of time with three networks: one purely
gas-phase, one that includes accretion and desorption, and one, the complete
gas-grain network, that includes surface chemistry in addition. We compare our
results with observed molecular abundances for two representative IRDCs --
IRDC013.90-1 and IRDC321.73-1 -- using the molecular species NH,
HCN, HNC, HCO, HCN, CH, NH and CS. IRDC013.90-1 is a cold IRDC,
with a temperature below 20 K, while IRDC321.73-1 is somewhat warmer, in the
range 20 - 30 K. We find that the complete gas-grain model fits the data very
well, but that the goodness-of-fit is not sharply peaked at a particular
temperature. Surface processes are important for the explanation of the high
gas-phase abundance of NH in IRDC321.73-1. The general success of the
0-D model in reproducing single-dish observations of our limited sample of 8
species shows that it is probably sufficient for an explanation of this type of
data. To build and justify more complicated models, including spatial
temperature and density structure, contraction, and heating, we require
high-resolution interferometric data.Comment: accepted for publication in Ap
Observations and radiative transfer modelling of a massive dense cold core in G333
Cold massive cores are one of the earliest manifestations of high mass star
formation. Following the detection of SiO emission from G333.125-0.562, a cold
massive core, further investigations of the physics, chemistry and dynamics of
this object has been carried out. Mopra and NANTEN2 molecular line profile
observations, Australia Telescope Compact Array (ATCA) line and continuum
emission maps, and Spitzer 24 and 70 \mum images were obtained. These new data
further constrain the properties of this prime example of the very early stages
of high mass star formation. A model for the source was constructed and
compared directly with the molecular line data using a 3D molecular line
transfer code - MOLLIE. The ATCA data reveal that G333.125-0.562 is composed of
two sources. One of the sources is responsible for the previously detected
molecular outflow and is detected in the Spitzer 24 and 70 \mum band data.
Turbulent velocity widths are lower than other more active regions of G333
which reflects the younger evolutionary stage and/or lower mass of this core.
The molecular line modelling requires abundances of the CO isotopes that
strongly imply heavy depletion due to freeze-out of this species onto dust
grains. The principal cloud is cold, moderately turbulent and possesses an
outflow which indicates the presence of a central driving source. The secondary
source could be an even less evolved object as no apparent associations with
continuum emissions at (far-)infrared wavelengths.Comment: 10 pages, accepted to MNRA
Modeling of Protostellar Clouds and their Observational Properties
A physical model and two-dimensional numerical method for computing the
evolution and spectra of protostellar clouds are described. The physical model
is based on a system of magneto-gasdynamical equations, including ohmic and
ambipolar diffusion, and a scheme for calculating the thermal and ionization
structure of a cloud. The dust and gas temperatures are determined during the
calculations of the thermal structure of the cloud. The results of computing
the dynamical and thermal structure of the cloud are used to model the
radiative transfer in continuum and in molecular lines. We presented the
results for clouds in hydrostatic and thermal equilibrium. The evolution of a
rotating magnetic protostellar cloud starting from a quasi-static state is also
considered. Spectral maps for optically thick lines of linear molecules are
analyzed. We have shown that the influence of the magnetic field and rotation
can lead to a redistribution of angular momentum in the cloud and the formation
of a characteristic rotational velocity structure. As a result, the
distribution of the velocity centroid of the molecular lines can acquire an
hourglass shape. We plan to use the developed program package together with a
model for the chemical evolution to interpret and model observed starless and
protostellar cores.Comment: Accepted to Astronomy Report
Molecular excitation in the Interstellar Medium: recent advances in collisional, radiative and chemical processes
We review the different excitation processes in the interstellar mediumComment: Accepted in Chem. Re
Control of star formation by supersonic turbulence
Understanding the formation of stars in galaxies is central to much of modern
astrophysics. For several decades it has been thought that stellar birth is
primarily controlled by the interplay between gravity and magnetostatic
support, modulated by ambipolar diffusion. Recently, however, both
observational and numerical work has begun to suggest that support by
supersonic turbulence rather than magnetic fields controls star formation. In
this review we outline a new theory of star formation relying on the control by
turbulence. We demonstrate that although supersonic turbulence can provide
global support, it nevertheless produces density enhancements that allow local
collapse. Inefficient, isolated star formation is a hallmark of turbulent
support, while efficient, clustered star formation occurs in its absence. The
consequences of this theory are then explored for both local star formation and
galactic scale star formation. (ABSTRACT ABBREVIATED)Comment: Invited review for "Reviews of Modern Physics", 87 pages including 28
figures, in pres
Effects of Nitrogen contamination in liquid Argon
A dedicated test of the effects of Nitrogen contamination in liquid Argon has
been performed at the INFN-Gran Sasso Laboratory (LNGS, Italy) within the WArP
R&D program. A detector has been designed and assembled for this specific task
and connected to a system for the injection of controlled amounts of gaseous
Nitrogen into the liquid Argon. Purpose of the test is to detect the reduction
of the Ar scintillation light emission as a function of the amount of the
Nitrogen contaminant injected in the Argon volume. A wide concentration range,
spanning from about 10^-1 ppm up to about 10^3 ppm, has been explored.
Measurements have been done with electrons in the energy range of minimum
ionizing particles (gamma-conversion from radioactive sources). Source spectra
at different Nitrogen contaminations are analyzed, showing sensitive reduction
of the scintillation yield at increasing concentrations. The rate constant of
the light quenching process induced by Nitrogen in liquid Ar has been found to
be k(N2)=0.11 micros^-1 ppm^-1. Direct PMT signals acquisition at high time
resolution by fast Waveform recording allowed to extract with high precision
the main characteristics of the scintillation light emission in pure and
contaminated LAr. In particular, the decreasing behavior in lifetime and
relative amplitude of the slow component is found to be appreciable from O(1
ppm) of Nitrogen concentrations
Analysis of the unexplored features of rrs (16S rDNA) of the Genus Clostridium
<p>Abstract</p> <p>Background</p> <p>Bacterial taxonomy and phylogeny based on <it>rrs </it>(16S rDNA) sequencing is being vigorously pursued. In fact, it has been stated that novel biological findings are driven by comparison and integration of massive data sets. In spite of a large reservoir of <it>rrs </it>sequencing data of 1,237,963 entries, this analysis invariably needs supplementation with other genes. The need is to divide the genetic variability within a taxa or genus at their <it>rrs </it>phylogenetic boundaries and to discover those fundamental features, which will enable the bacteria to naturally fall within them. Within the large bacterial community, <it>Clostridium </it>represents a large genus of around 110 species of significant biotechnological and medical importance. Certain <it>Clostridium </it>strains produce some of the deadliest toxins, which cause heavy economic losses. We have targeted this genus because of its high genetic diversity, which does not allow accurate typing with the available molecular methods.</p> <p>Results</p> <p>Seven hundred sixty five <it>rrs </it>sequences (> 1200 nucleotides, nts) belonging to 110 <it>Clostridium </it>species were analyzed. On the basis of 404 <it>rrs </it>sequences belonging to 15 <it>Clostridium </it>species, we have developed species specific: (i) phylogenetic framework, (ii) signatures (30 nts) and (iii) <it>in silico </it>restriction enzyme (14 Type II REs) digestion patterns. These tools allowed: (i) species level identification of 95 <it>Clostridium </it>sp. which are presently classified up to genus level, (ii) identification of 84 novel <it>Clostridium </it>spp. and (iii) potential reduction in the number of <it>Clostridium </it>species represented by small populations.</p> <p>Conclusions</p> <p>This integrated approach is quite sensitive and can be easily extended as a molecular tool for diagnostic and taxonomic identification of any microbe of importance to food industries and health services. Since rapid and correct identification allows quicker diagnosis and consequently treatment as well, it is likely to lead to reduction in economic losses and mortality rates.</p
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