11,007 research outputs found
The nearby Galaxy structure toward the Vela Gum nebula
We report on photometry and spectroscopy for MK classification
purposes carried out in the fields of five open clusters projected against the
Vela Gum in the Third Galactic Quadrant of the Galaxy. They are Ruprecht 20,
Ruprecht 47, Ruprecht 60, NGC 2660 and NGC 2910. We could improve/confirm the
parameters of these objects derived before. The spectroscopic parallax method
has been applied to several stars located in the fields of four out of the five
clusters to get their distances and reddenings. With this method we found two
blue stars in the field of NGC 2910 at distances that make them likely members
of Vela OB1 too. Also, projected against the fields of Ruprecht 20 and Ruprecht
47 we have detected other young stars favoring not only the existence of Puppis
OB1 and OB2 but conforming a young stellar group at kpc from the Sun
and extending for more than 6 kpc outward the Galaxy. If this is the case,
there is a thickening of the thin Galactic disk of more than 300 pc at just 2-3
kpc from the Sun. Ruprecht 60 and NGC 2660 are too old objects that have no
physical relation with the associations under discussion. An astonishing result
has been the detection in the background of Ruprecht 47 of a young star at the
impressive distance of 9.5 kpc from the Sun that could be a member of the
innermost part of the Outer Arm. Another far young star in the field of NGC
2660, at near 6.0 kpc, may become a probable member of the Perseus Arm or of
the inner part of the Local Arm. The distribution of young clusters and stars
onto the Third Galactic Quadrant agrees with recent findings concerning the
extension of the Local Arm as revealed by parallaxes of regions of star
formation. We show evidences too that added to previous ones found by our group
explain the thickening of the thin disk as a combination of flare and warp.Comment: Accepted for publication in New Astronom
Pressure-induced structural, electronic, and magnetic effects in BiFeO3
We present a first-principles study of multiferroic BiFeO3 at high pressures.
Our work reveals the main structural (change in Bi's coordination and loss of
ferroelectricity), electronic (spin crossover and metallization), and magnetic
(loss of order) effects favored by compression and how they are connected. Our
results are consistent with the striking manifold transition observed
experimentally by Gavriliuk et al. [Phys. Rev. B 77, 155112 (2008)] and provide
an explanation for it.Comment: 4 pages with 4 figures embedded. More information at
http://www.icmab.es/dmmis/leem/jorg
Numerical analysis of the stability of the Electrohydrodynamic (EHD) electroconvection between two plates
The time evolution of the problem of Electrohydrodynamic (EHD)
convection in a liquid between two plates is analysed numerically. The equations are
nondimensionalized using the ion drift velocity and the viscous time scales. Following
the non-dimensionalisation of the respective model, two different techniques have been
used to describe the charge evolution, namely the Finite-Element Flux-Corrected
Transport Method and the Particle-In-Cell technique. The results obtained with the
two schemes, apart from showing good agreement, have revealed the appearance of a
two-roll structure not described in previous works. This is investigated in detail for
both strong and weak injection.Ministerio de ciencia y tecnología FQM-42
Examples of signature (2,2) manifolds with commuting curvature operators
We exhibit Walker manifolds of signature (2,2) with various commutativity
properties for the Ricci operator, the skew-symmetric curvature operator, and
the Jacobi operator. If the Walker metric is a Riemannian extension of an
underlying affine structure A, these properties are related to the Ricci tensor
of A
Photometric study of the young open cluster NGC 3293
Deep and extensive CCD photometric observations were
carried out in the area of the open cluster NGC 3293. The new data set allows
to see the entire cluster sequence down to , revealing that
stars with are evolving off the main sequence; stars with are
placed above it. According to our analysis, the cluster distance is () and its nuclear age is . NGC 3293 contains an important fraction of pre--main sequence (PMS) stars
distributed along a parallel band to the ZAMS with masses from 1 to 2.5 \cal
M_{\sun} and a mean contraction age of . This last value does not
differ too much from the nuclear age estimate. Actually, if we take into
account the many factors that may affect the PMS star positions onto the
colour--magnitude diagram, both ages can be perfectly reconciled. The star
formation rate, on the other hand, suggests that NGC 3293 stars formed surely
in one single event, therefore favouring a coeval process of star formation.
Besides, using the data, we detected nineteen stars with signs of
having emission in the region of NGC 3293, giving another
indication that the star formation process is still active in the region. The
computed initial mass function for the cluster has a slope value , a bit flatter than the typical slope for field stars and similar to the
values found for other young open clusters.Comment: 17 pages, 13 eps figures, in press in Astronomy and Astrophysic
The inhomogeneous evolution of subgraphs and cycles in complex networks
Subgraphs and cycles are often used to characterize the local properties of
complex networks. Here we show that the subgraph structure of real networks is
highly time dependent: as the network grows, the density of some subgraphs
remains unchanged, while the density of others increase at a rate that is
determined by the network's degree distribution and clustering properties. This
inhomogeneous evolution process, supported by direct measurements on several
real networks, leads to systematic shifts in the overall subgraph spectrum and
to an inevitable overrepresentation of some subgraphs and cycles.Comment: 4 pages, 4 figures, submitted to Phys. Rev.
Searching for spiral features in the outer Galactic disk. The field towards WR38 and WR38a
The detailed spiral structure in the outer Galactic disk is still poorly
known, and for several Galactic directions we rely on model extrapolations. One
of these regions is the fourth Galactic quadrant, in the sector comprised
between Vela and Carina (270 <l< 300) where no spiral arms have been detected
so far in the optical beyond 270. By means of deep UBVI photometry, we search
for spiral features in known low absorption windows.U photometry, although
demanding, constitutes a powerful tool to detect and characterize distant
aggregates, and allows to derive firmer distance estimates. We studied a
direction close to the tangent (l=290) to the Carina arm, in an attempt to
detect optical spiral tracers beyond the Carina branch, where radio
observations and models predictions indicate the presence of the extension of
the Perseus and Norma-Cygnus spiral arms in the fourth quadrant.Along this line
of sight, we detect three distinct groups of young stars. Two of them, at 2.5
and 6.0 kpc, belong to the Carina spiral arm (which is crossed twice in this
particular direction).The latter is here detected for the first time. The third
group, at a distance of 12.7 kpc, is part of the Perseus arm which lies beyond
the Carina arm, and constitutes the first optical detection of this arm in the
fourth Galactic quadrant. The position of this feature is compatible with HI
observations and model predictions. We furthermore present evidence that this
extremely distant group, formerly thought to be a star cluster (Shorlin 1), is
in fact a diffuse young population. In addition, our data-set does not support
the possible presence of the Monoceros Ring toward this direction. This study
highlights how multicolor optical studies can be effective to probe the spiral
structure in the outer Galactic disk.Comment: 9 pages, 13 eps figure, in press in A&A, abstract rephrased and a few
figures degraded in resolution to fit i
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