1,606 research outputs found
Superbubble evolution including the star-forming clouds: Is it possible to reconcile LMC observations with model predictions?
Here we present a possible solution to the apparent discrepancy between the
observed properties of LMC bubbles and the standard, constant density bubble
model. A two-dimensional model of a wind-driven bubble expanding from a
flattened giant molecular cloud is examined. We conclude that the expansion
velocities derived from spherically symmetric models are not always applicable
to elongated young bubbles seen almost face-on due to the LMC orientation. In
addition, an observational test to differentiate between spherical and
elongated bubbles seen face-on is discussed.Comment: 25 pages, 7 figures, accepted to ApJ (September, 1999 issue
New Results of Observations of the Only Supernova Remnant in the IC1613 Galaxy
The new results of a study of the kinematics of the supernova remnant S8 in
the IC1613 galaxy are reported. The expansion velocity of the bright optical
nebula is determined based on observations made with the 6-m telescope of the
Special Astrophysical Observatory of the Russian Academy of Sciences using MPSF
field spectrograph and SCORPIO focal reducer operating in the scanning
Fabry--Perot interferometer mode. An analysis of 21-cm line VLA observations of
the galaxy corroborates our earlier proposed model of a SN exploding inside a
cavern surrounded by a dense shell and S8 colliding with the wall of the HI
shell.Comment: 8 pages, 7 figures; accepted for publication in Astronomy Letter
Fluorescence In Situ Hybridization: a potentially useful technique for detection of microorganisms on mortars
This paper discusses the possibilities of applying Fluorescence In Situ Hybridization (FISH) to detect microorganisms on mortars, as this analytical technique has been used in different fields for the detection and identification of individual microbial cells in situ. FISH technique was applied for microbial detection on test and real mortars inoculated with fungal suspensions of S. cerevisae 396 and Nectria sp. A universal eukaryotic probe (EUK516) labelled with fluorescent dye (Cy3) was tested with different cell fixation procedures (4% (w / v) paraformaldehyde or 50% (v / v) ethanol in PBS). Positive results were obtained with FISH detection of Nectria on testing/artificial as well as authentic/historical mortars, which confirms successful application of FISH technique to a new on mortars
Gravitational wave background from rotating neutron stars
The background of gravitational waves produced by the ensemble of rotating
neutron stars (which includes pulsars, magnetars and gravitars) is
investigated. A formula for \Omega(f) (commonly used to quantify the
background) is derived, properly taking into account the time evolution of the
systems since their formation until the present day. Moreover, the formula
allows one to distinguish the different parts of the background: the
unresolvable (which forms a stochastic background) and the resolvable. Several
estimations of the background are obtained, for different assumptions on the
parameters that characterize neutron stars and their population. In particular,
different initial spin period distributions lead to very different results. For
one of the models, with slow initial spins, the detection of the background can
be rejected. However, other models do predict the detection of the background
by the future ground-based gravitational wave detector ET. A robust upper limit
for the background of rotating neutron stars is obtained; it does not exceed
the detection threshold of two cross-correlated Advanced LIGO interferometers.
If gravitars exist and constitute more than a few percent of the neutron star
population, then they produce an unresolvable background that could be detected
by ET. Under the most reasonable assumptions on the parameters characterizing a
neutron star, the background is too faint. Previous papers have suggested
neutron star models in which large magnetic fields (like the ones that
characterize magnetars) induce big deformations in the star, which produce a
stronger emission of gravitational radiation. Considering the most optimistic
(in terms of the detection of gravitational waves) of these models, an upper
limit for the background produced by magnetars is obtained; it could be
detected by ET, but not by BBO or DECIGO.Comment: 25 pages, 15 figure
Molecular structure and polymorphism of a cyclohexanediol: trans-1,4-cyclohexanedimethanol
This study aims to investigate the molecular structure and polymorphism of trans-1,4-cyclohexanedimethanol,
including the bi-axial/bi-equatorial equilibrium and the nature of the intermolecular H-bond networks in
condensed phases created by the hydroxyl group torsions. The full conformational space of the single
molecule was explored by MP2 calculations, showing that the optimized bi-equatorial conformers have
similar stability and the bi-axial ones have much higher energies. The hydroxymethyl substituents have
preference for gauche/anti or gauche+/gauche− conformations. Polymorphic forms were generated by
crystallization from solutions and by cooling the melt, which were characterized by a combination of
techniques: DSC, PLTM and XRD. Two polymorphs were isolated and their crystal structures were solved
by direct methods based on single-crystal X-ray analysis. Both were found to contain two of the most
stable conformers found in the computational calculations. The influence of H-bonding in the polymorphic
structures was verified by analysis of the structural differences between the geometries present in
the polymorphs determined by XRD and their single molecule counterparts resulting from the theoretical
calculations. The bi-axial conformations are destabilized over the bi-equatorial ones in isolated and
crystalline forms of trans-1,4-cyclohexanedimethanol
Gravitational wave astronomy with the SKA
On a time scale of years to decades, gravitational wave (GW) astronomy will
become a reality. Low frequency (nanoHz) GWs are detectable through long-term
timing observations of the most stable pulsars. Radio observatories worldwide
are currently carrying out observing programmes to detect GWs, with data sets
being shared through the International Pulsar Timing Array project. One of the
most likely sources of low frequency GWs are supermassive black hole binaries
(SMBHBs), detectable as a background due to a large number of binaries, or as
continuous or burst emission from individual sources. No GW signal has yet been
detected, but stringent constraints are already being placed on galaxy
evolution models. The SKA will bring this research to fruition.
In this chapter, we describe how timing observations using SKA1 will
contribute to detecting GWs, or can confirm a detection if a first signal
already has been identified when SKA1 commences observations. We describe how
SKA observations will identify the source(s) of a GW signal, search for
anisotropies in the background, improve models of galaxy evolution, test
theories of gravity, and characterise the early inspiral phase of a SMBHB
system.
We describe the impact of the large number of millisecond pulsars to be
discovered by the SKA; and the observing cadence, observation durations, and
instrumentation required to reach the necessary sensitivity. We describe the
noise processes that will influence the achievable precision with the SKA. We
assume a long-term timing programme using the SKA1-MID array and consider the
implications of modifications to the current design. We describe the possible
benefits from observations using SKA1-LOW. Finally, we describe GW detection
prospects with SKA1 and SKA2, and end with a description of the expectations of
GW astronomy.Comment: 19 pages, 3 figures, to be published in: "Advancing Astrophysics with
the Square Kilometre Array", Proceedings of Science, PoS(AASKA14)03
The UTMOST pulsar timing programme I: overview and first results
We present an overview and the first results from a large-scale pulsar timing
programme that is part of the UTMOST project at the refurbished Molonglo
Observatory Synthesis Radio Telescope (MOST) near Canberra, Australia. We
currently observe more than 400 mainly bright southern radio pulsars with up to
daily cadences. For 205 (8 in binaries, 4 millisecond pulsars) we publish
updated timing models, together with their flux densities, flux density
variability, and pulse widths at 843 MHz, derived from observations spanning
between 1.4 and 3 yr. In comparison with the ATNF pulsar catalogue, we improve
the precision of the rotational and astrometric parameters for 123 pulsars, for
47 by at least an order of magnitude. The time spans between our measurements
and those in the literature are up to 48 yr, which allows us to investigate
their long-term spin-down history and to estimate proper motions for 60
pulsars, of which 24 are newly determined and most are major improvements. The
results are consistent with interferometric measurements from the literature. A
model with two Gaussian components centred at 139 and fits the transverse velocity distribution best. The pulse duty
cycle distributions at 50 and 10 per cent maximum are best described by
log-normal distributions with medians of 2.3 and 4.4 per cent, respectively. We
discuss two pulsars that exhibit spin-down rate changes and drifting subpulses.
Finally, we describe the autonomous observing system and the dynamic scheduler
that has increased the observing efficiency by a factor of 2-3 in comparison
with static scheduling.Comment: 31 pages, 14 figures, 6 tables, accepted for publication in MNRA
The UTMOST: A hybrid digital signal processor transforms the MOST
The Molonglo Observatory Synthesis Telescope (MOST) is an 18,000 square meter
radio telescope situated some 40 km from the city of Canberra, Australia. Its
operating band (820-850 MHz) is now partly allocated to mobile phone
communications, making radio astronomy challenging. We describe how the
deployment of new digital receivers (RX boxes), Field Programmable Gate Array
(FPGA) based filterbanks and server-class computers equipped with 43 GPUs
(Graphics Processing Units) has transformed MOST into a versatile new
instrument (the UTMOST) for studying the dynamic radio sky on millisecond
timescales, ideal for work on pulsars and Fast Radio Bursts (FRBs). The
filterbanks, servers and their high-speed, low-latency network form part of a
hybrid solution to the observatory's signal processing requirements. The
emphasis on software and commodity off-the-shelf hardware has enabled rapid
deployment through the re-use of proven 'software backends' for its signal
processing. The new receivers have ten times the bandwidth of the original MOST
and double the sampling of the line feed, which doubles the field of view. The
UTMOST can simultaneously excise interference, make maps, coherently dedisperse
pulsars, and perform real-time searches of coherent fan beams for dispersed
single pulses. Although system performance is still sub-optimal, a pulsar
timing and FRB search programme has commenced and the first UTMOST maps have
been made. The telescope operates as a robotic facility, deciding how to
efficiently target pulsars and how long to stay on source, via feedback from
real-time pulsar folding. The regular timing of over 300 pulsars has resulted
in the discovery of 7 pulsar glitches and 3 FRBs. The UTMOST demonstrates that
if sufficient signal processing can be applied to the voltage streams it is
possible to perform innovative radio science in hostile radio frequency
environments.Comment: 12 pages, 6 figure
Risk Factors for Active Asthma at School Age: an 8-Year Prospective Study
A sibilância recorrente na infância é uma entidade clÃnica prevalente e heterogénea do pontode vista da história natural e do prognóstico. Efectuou-se um estudo prospectivo com 8 anos de duração, com o objectivo de relacionar a evolução clÃnica da sibilância recorrente nos primeiros
anos de vida, com factores de prognóstico associados com a persistência da sintomatologia. Uma coorte de 308 crianças com sibilância recorrente, com idade ≤6 anos, foi incluÃda no estudo em
1993. Foi aplicado um questionário clÃnico, realizados testes cutâneos por prick e efectuado doseamento sérico de IgE total. Em 1996 procedeu-se a uma primeira reavaliação sistemática destas crianças. Em 2001 foi efectuada nova reavaliação sistemática, possÃvel em 81% destas crianças (n=249), com repetição dos testes cutâneos e realização de avaliação funcional respiratória,em perÃodo intercrise, com espirometria com prova de broncodilatação (BD). As crianças reavaliadas apresentavam média etária de 11 anos (8-14 anos) e relação sexo M/F de 1.7/1. Permaneciam sintomáticas em 61% dos casos. A prevalência de atopia foi de 48% em 1993, 65% em 1996 e 75% em 2001. Pela realização de um modelo de regressão logÃstica múltiplo foram identificados
como factores de risco para asma activa em idade escolar: história pessoal de rinite alérgica (OR=15.8, IC95%=6.1-40.8; p<0.001), asma paterna (OR=7.2, IC95%=1.7-29.7; p=0.007), história pessoal de eczema atópico (OR=5.9, IC95%=2.2-15.7; p<0.001), asma materna (OR=5.4, IC95%=1.7-17.1; p=0.004), evidência de sensibilização alergénica (OR=3.4, IC95%=1.2-10.4;p=0.03) e inÃcio dos sintomas ≥2 anos de idade (OR=2.1, IC95%=1.1-4.8; p=0.04); a frequência de infantário antes dos 12 meses de idade foi identificada como factor protector (OR=0.4, IC95%=0.2-
0.9; p=0.04). Desenvolveram sensibilização alergénica de novo (ácaros do pó >80%) 66 das 128 crianças não atópicas em 1993 (52%). Apresentavam obstrução brônquica 36% das crianças: 47% das sintomáticas e 18% das assintomáticas (p<0.001). A prova de BD foi positiva em 35%: 47% nos sintomáticos e 13% nos assintomáticos (p<0.001). Concluindo, foram identificados como factores de mau prognóstico, antecedentes pessoais de doença alérgica, história parental de asma,
presença de sensibilização alergénica e inÃcio dos sintomas na segunda infância. Os sintomas clÃnicos podem preceder em anos a sensibilização alergénica, realçando a importância da instituição precoce de medidas de controlo ambiental. Alterações nas provas funcionais respiratórias, mais
frequentes nas asmas activas, estavam também presentes em crianças actualmente sem clÃnica, reforçando a necessidade de valorizar marcadores objectivos nesta cada vez mais prevalente doença respiratória crónica
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