4,846 research outputs found
HIPPARCOS Astrometric Orbit and Evolutionary Status of HR 6046
The previously known, 6-yr spectroscopic binary HR 6046 has been speculated
in the past to contain a compact object as the secondary. A recent study has
re-determined the orbit with great accuracy, and shown that the companion is an
evolved but otherwise normal star of nearly identical mass as the primary,
which is also a giant. The binary motion was detected by the Hipparcos mission
but was not properly accounted for in the published astrometric solution. Here
we use the Hipparcos intermediate data in combination with the spectroscopic
results to revise that solution and establish the orbital inclination angle for
the first time, and with it the absolute masses M(A) = 1.38 [-0.03,+0.09]
M(Sun) and M(B) = 1.36 [-0.02,+0.07] M(Sun). Aided by other constraints, we
investigate the evolutionary status and confirm that the primary star is
approaching the tip of the red-giant branch, while the secondary is beginning
its first ascent.Comment: To appear in The Astronomical Journal. 8 pages including tables and
figures, in emulateapj forma
The pressure confined wind of the massive and compact superstar cluster M82-A1
The observed parameters of the young superstar cluster M82-A1 and its
associated compact HII region are here shown to indicate a low heating
efficiency or immediate loss, through radiative cooling, of a large fraction of
the energy inserted by stellar winds and supernovae during the early evolution
of the cluster. This implies a bimodal hydrodynamic solution which leads to a
reduced mass deposition rate into the ISM, with a much reduced outflow
velocity. Furthermore, to match the observed parameters of the HII region
associated to M82-A1, the resultant star cluster wind is here shown to ought to
be confined by a high pressure interstellar medium. The cluster wind
parameters, as well as the location of the reverse shock, its cooling length
and the radius of the standing outer HII region are derived analytically. All
of these properties are then confirmed with a semi-analytical integration of
the flow equations, which provides us also with the run of the hydrodynamic
variables as a function of radius. The impact of the results is discussed and
extended to other massive and young superstar clusters surrounded by a compact
HII region.Comment: 19 pages, 4 figures, accepted for publication in Ap
Metallicity evolution of AGNs from UV emission-lines based on a new index
We analyzed the evolution of the metallicity of the gas with the redshift for
a sample of AGNs in a very wide redshift range (0<z<4) using ultraviolet
emission-lines from the narrow-line regions (NLRs) and photoionization models.
The new index C43=log(CIV+CIII])/HeII is suggested as a metallicity indicator
for AGNs. Based on this indicator, we confirmed the no metallicity evolution of
NLRs with the redshift pointed out by previous works. We found that metallicity
of AGNs shows similar evolution than the one predicted by cosmic semi-analytic
models of galaxy formation set within the Cold Dark Matter merging hierarchy
(for z < 3). Our results predict a mean metallicity for local objects in
agreement with the solar value (12+log(O/H)=8.69). This value is about the same
that the maximum oxygen abundance value derived for the central parts of local
spiral galaxies. Very low metallicity log(Z/Z_{\odot})~ -0.8 for some objects
in the range 1.5 < z <3 is derived.Comment: 25 pages, 10 figures, accepted MNRA
Phase and Charge reentrant phase transitions in two capacitively coupled Josephson arrays with ultra-small junction
We have studied the phase diagram of two capacitively coupled Josephson
junction arrays with charging energy, , and Josephson coupling energy,
. Our results are obtained using a path integral Quantum Monte Carlo
algorithm. The parameter that quantifies the quantum fluctuations in the i-th
array is defined by . Depending on
the value of , each independent array may be in the semiclassical or
in the quantum regime: We find that thermal fluctuations are important when
and the quantum fluctuations dominate when . We have extensively studied the interplay between vortex and charge
dominated individual array phases. The two arrays are coupled via the
capacitance at each site of the lattices. We find a {\it
reentrant transition} in , at low temperatures, when one of
the arrays is in the semiclassical limit (i.e. ) and the
quantum array has , for the values considered for
the interlayer capacitance. In addition, when , and
for all the inter-layer couplings considered above, a {\it novel} reentrant
phase transition occurs in the charge degrees of freedom, i.e. there is a
reentrant insulating-conducting transition at low temperatures. We obtain the
corresponding phase diagrams and found some features that resemble those seen
in experiments with 2D JJA.Comment: 25 Latex pages including 8 encapsulated poscript figures. Accepted
for publication in Phys. Rev B (Nov. 2004 Issue
A Nanoscale Parametric Feedback Oscillator
We describe and demonstrate a new oscillator topology, the parametric feedback oscillator (PFO). The PFO paradigm is applicable to a wide variety of nanoscale devices and opens the possibility of new classes of oscillators employing innovative frequency-determining elements, such as nanoelectromechanical systems (NEMS), facilitating integration with circuitry and system-size reduction. We show that the PFO topology can also improve nanoscale oscillator performance by circumventing detrimental effects that are otherwise imposed by the strong device nonlinearity in this size regime
On the Extreme Positive Feedback Star-Forming Mode from Massive and Compact Superstar Clusters
The force of gravity acting within the volume occupied by young, compact and
massive superstar clusters, is here shown to drive in situ all the matter
deposited by winds and supernovae into several generations of star formation.
These events are promoted by radiative cooling which drains the thermal energy
of the ejected gas causing its accumulation to then rapidly exceed the
gravitational instability criterion. A detailed account of the integrated
ionizing radiation and mechanical luminosity as a function of time is here
shown to lead to a new stationary solution. In this, the mass deposition rate
, instead of causing a wind as in the adiabatic solution, turns into a
positive feedback star-forming mode equal to the star formation rate. Some of
the implications of this extreme positive feedback mode are discussed.Comment: 4 pages, 4 figures, accepted for publication in The Astrophysical
Journal Letter
TUMORES RAROS EN NIÑOS Y ADOLESCENTES
ResumenLos tumores infrecuentes están definidos como cánceres pediátricos con una incidencia anual <2 casos por millón. Aunque son percibidos como raros, constituyen el 15% de todos los cánceres en menores de 20 años y 30% de todos los tumores de pacientes entre 15 y 19 años.Se han desarrollado proyectos cooperativos nacionales e internacionales pediátricos con el fin de mejorar el manejo clínico y la investigación básica en estos tumores. Revisamos los procesos desarrollados y las dificultades que se han enfrentado, como bajas tasas de registro y participación en bancos de tumores y estudios clínicos. Esta experiencia inicial ha permitido desarrollar estrategias alternativas que permitirían implementar una iniciativa similar para América Latina.La experiencia demuestra la factibilidad de cooperación multidisciplinaria a nivel nacional y sugiere que se pueden realizar estudios internacionales, que aumenten nuestro entendimiento de la biología de estos tumores, mejorando los resultados de tratamiento de niños y adolescentes con cánceres infrecuentes.SummaryAlthough perceived as rare, infrequent tumors, defined as childhood solid malignancies with an annual incidence < 2/million and not considered in other clinical trials, account for 15% of all cancers in patients younger than age 20 and for 30% of all tumors in patients ages 15 to 19.National and international cooperative projects on rare paediatric tumours have been developed to improve the clinical management and basic research on these tumors. We reviewed the process developed and the problems it had to face, as low rates of registration, low levels of participation in tumor banking, and clinical trials. This initial experience has allowed to develop alternative strategies that could help to launch a latinamerican initiative.Experience demonstrates the feasibility of a national multidisciplinary cooperation and suggests that international studies can be performed, increasing our knowledge to understand the biology and improving the treatment results of young patients with rare cancers
On the X-ray Emission from Massive Star Clusters and their Evolving Superbubbles
The X-ray emission properties from the hot thermalized plasma that results
from the collisions of individual stellar winds and supernovae ejecta within
rich and compact star clusters are discussed. We propose a simple analytical
way of estimating the X-ray emission generated by super star clusters and
derive an expression that indicates how this X-ray emission depends on the main
cluster parameters. Our model predicts that the X-ray luminosity from the star
cluster region is highly dependent on the star cluster wind terminal speed, a
quantity related to the temperature of the thermalized ejecta.We have also
compared the X-ray luminosity from the SSC plasma with the luminosity of the
interstellar bubbles generated from the mechanical interaction of the high
velocity star cluster winds with the ISM.We found that the hard (2.0 keV - 8.0
keV) X-ray emission is usually dominated by the hotter SSC plasma whereas the
soft (0.3 keV - 2.0 keV) component is dominated by the bubble plasma. This
implies that compact and massive star clusters should be detected as point-like
hard X-ray sources embedded into extended regions of soft diffuse X-ray
emission. We also compared our results with predictions from the population
synthesis models that take into consideration binary systems and found that in
the case of young,massive and compact super star clusters the X-ray emission
from the thermalized star cluster plasma may be comparable or even larger than
that expected from the HMXB population.Comment: 24 pages, 8 figures, Accepted for publication in The Astrophysical
Journa
Chemical Compositions of Four Metal-poor Giants
We present the chemical compositions of four K giants CS 22877-1, CS
22166-16, CS22169-35 and BS 16085 - 0050 that have [Fe/H] in the range -2.4 to
-3.1. Metal-poor stars with [Fe/H] < -2.5 are known to exhibit considerable
star - to - star variations of many elements. This quartet confirms this
conclusion. CS 22877-1 and CS 22166-16 are carbon-rich. There is significant
spread for [/Fe] within our sample where [/Fe] is computed from
the mean of the [Mg/Fe], and [Ca/Fe] ratios. BS 16085 - 0050 is remarkably
enriched with a mean [/Fe] of 0.7 but CS 22169-35 is
-poor. The aluminium abundance also shows a significant variation over
the sample. A parallel and unsuccessful search among high-velocity late-type
stars for metal-poor stars is described.Comment: 14 pages (text), 4 tables, 3 figures, Accepted for publication in
PAS
Five New Transits of the Super-Neptune HD 149026
We present new photometry of HD 149026 spanning five transits of its
"super-Neptune" planet. In combination with previous data, we improve upon the
determination of the planet-to-star radius ratio: R_p/R_star =
0.0491^{+0.0018}_{-0.0005}. We find the planetary radius to be 0.71 +/- 0.05
R_Jup, in accordance with previous theoretical models invoking a high metal
abundance for the planet. The limiting error is the uncertainty in the stellar
radius. Although we find agreement among four different ways of estimating the
stellar radius, the uncertainty remains at 7%. We also present a refined
transit ephemeris and a constraint on the orbital eccentricity and argument of
pericenter, e cos(omega) = -0.0014 +/- 0.0012, based on the measured interval
between primary and secondary transits.Comment: To appear in ApJ [19 pages
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