139 research outputs found
A Synthesis of Research on Family Preservation and Family Reunification Programs
How effective are current efforts to preserve and reunify families in child welfare? In this paper we review research on programs aimed at preventing out-of-home placement of children, broader family preservation programs, and programs designed to reunify families with children in foster care.1 We examine what is known about the outcomes of these programs, relationships between service characteristics and outcomes, and the response of subgroups of clients to services.
Claims that family preservation programs result in substantial reductions in the placement of children are based largely on non-experimental studies. Such studies do not provide solid evidence of program effects. Evidence from controlled studies of placement prevention effects is much weaker. The results of controlled studies suggest that difficulties in targeting services to families at risk of placement contribute to the lack of effects on likelihood of placement. The small amount of evidence on outcomes other than placement suggests that these programs have little effect on the recurrence of child maltreatment, although they may produce modest, short term improvements in some aspects of child and family functioning.
Research on family reunification programs is in its infancy and there are very few controlled studies in this area. Available evidence is mixed. While some studies suggest that intensive, in-home services can speed the process of family reunification, the long-term effects of these programs are largely unknown. In particular, it is not clear whether intensive service programs increase the rates at which children return home, reduce the risk of foster care reentry, or lessen the chance of subsequent child maltreatment.
We conclude our review with a discussion of directions for further research in this area
Linear Stability of Triangular Equilibrium Points in the Generalized Photogravitational Restricted Three Body Problem with Poynting-Robertson Drag
In this paper we have examined the linear stability of triangular equilibrium
points in the generalised photogravitational restricted three body problem with
Poynting-Robertson drag. We have found the position of triangular equilibrium
points of our problem. The problem is generalised in the sense that smaller
primary is supposed to be an oblate spheroid. The bigger primary is considered
as radiating. The equations of motion are affected by radiation pressure force,
oblateness and P-R drag. All classical results involving photogravitational and
oblateness in restricted three body problem may be verified from this result.
With the help of characteristic equation, we discussed the stability. Finally
we conclude that triangular equilibrium points are unstable.Comment: accepted for publication in Journal of Dynamical Systems & Geometric
Theories Vol. 4, Number 1 (2006
Soft-x-ray fluorescence study of the quasi-one-dimensional Heisenberg antiferromagnet tetraphenylverdazyl
Soft-x-ray fluorescence measurements have been performed on a single crystal of the organic antiferromagnet 2,4,6-triphenylverdazyl. Resonant and nonresonant C Kα and N Kα (2p â 1s transition) x-ray emission spectra (XES) were measured and compared with x-ray photoelectron valence band spectra and deMon density-functional theory calculations. It is shown that intramolecular interactions are much stronger than intermolecular ones and give the main contribution to the formation of C 2p density of states. We present evidence of a delocalization of unpaired N 2p electrons over the verdazyl ring. The excitation energy dependence of C Kα and N Kα XES observed below the C 1s and N 1s thresholds, respectively, is discussed in terms of symmetry selective resonant inelastic x-ray scattering
Mass Transfer by Stellar Wind
I review the process of mass transfer in a binary system through a stellar
wind, with an emphasis on systems containing a red giant. I show how wind
accretion in a binary system is different from the usually assumed Bondi-Hoyle
approximation, first as far as the flow's structure is concerned, but most
importantly, also for the mass accretion and specific angular momentum loss.
This has important implications on the evolution of the orbital parameters. I
also discuss the impact of wind accretion, on the chemical pollution and change
in spin of the accreting star. The last section deals with observations and
covers systems that most likely went through wind mass transfer: barium and
related stars, symbiotic stars and central stars of planetary nebulae (CSPN).
The most recent observations of cool CSPN progenitors of barium stars, as well
as of carbon-rich post-common envelope systems, are providing unique
constraints on the mass transfer processes.Comment: Chapter 7, in Ecology of Blue Straggler Stars, H.M.J. Boffin, G.
Carraro & G. Beccari (Eds), Astrophysics and Space Science Library, Springe
The Effect of Radiation Pressure on the Equilibrium Points in the Generalised Photogravitational Restricted Three Body Problem
The existence of equilibrium points and the effect of radiation pressure have
been discussed numerically. The problem is generalized by considering bigger
primary as a source of radiation and small primary as an oblate spheroid. We
have also discussed the Poynting-Robertson(P-R) effect which is caused due to
radiation pressure. It is found that the collinear points deviate
from the axis joining the two primaries, while the triangular points
are not symmetrical due to radiation pressure. We have seen that
are linearly unstable while are conditionally stable in the sense of
Lyapunov when P-R effect is not considered. We have found that the effect of
radiation pressure reduces the linear stability zones while P-R effect induces
an instability in the sense of Lyapunov
Vaccine eïŹectiveness of the pneumococcal Haemophilus inïŹuenzae protein D conjugate vaccine (PHiD-CV10) against clinically suspected invasive pneumococcal disease: a cluster-randomised trial
Post-AGB stars with hot circumstellar dust: binarity of the low-amplitude pulsators
While the first binary post-AGB stars were serendipitously discovered, the
distinct characteristics of their Spectral Energy Distribution (SED) allowed us
to launch a more systematic search for binaries. We selected post-AGB objects
which show a broad dust excess often starting already at H or K, pointing to
the presence of a gravitationally bound dusty disc in the system. We started a
very extensive multi-wavelength study of those systems and here we report on
our radial velocity and photometric monitoring results for six stars of early F
type, which are pulsators of small amplitude. To determine the radial velocity
of low signal-to-noise time-series, we constructed dedicated auto-correlation
masks. The radial velocity variations were subjected to detailed analysis to
differentiate between pulsational variability and variability due to orbital
motion. Finally orbital minimalisation was performed to constrain the orbital
elements. All of the six objects are binaries, with orbital periods ranging
from 120 to 1800 days. Five systems have non-circular orbits. The mass
functions range from 0.004 to 0.57 solar mass and the companions are likely
unevolved objects of (very) low initial mass. We argue that these binaries must
have been subject to severe binary interaction when the primary was a cool
supergiant. Although the origin of the circumstellar disc is not well
understood, the disc is generally believed to be formed during this strong
interaction phase. The eccentric orbits of these highly evolved objects remain
poorly understood. With the measured orbits and mass functions we conclude that
the circumbinary discs seem to have a major impact on the evolution of a
significant fraction of binary systems.Comment: 13 pages, 15 figures, accepted for Astronomy and Astrophysic
The decline and rise of neighbourhoods: the importance of neighbourhood governance
There is a substantial literature on the explanation of neighbourhood change. Most of this literature concentrates on identifying factors and developments behind processes of decline. This paper reviews the literature, focusing on the identification of patterns of neighbourhood change, and argues that the concept of neighbourhood governance is a missing link in attempts to explain these patterns. Including neighbourhood governance in the explanations of neighbourhood change and decline will produce better explanatory models and, finally, a better view about what is actually steering neighbourhood change
An incisive look at the symbiotic star SS Leporis -- Milli-arcsecond imaging with PIONIER/VLTI
Context. Determining the mass transfer in a close binary system is of prime
importance for understanding its evolution. SS Leporis, a symbiotic star
showing the Algol paradox and presenting clear evidence of ongoing mass
transfer, in which the donor has been thought to fill its Roche lobe, is a
target particularly suited to this kind of study. Aims. Since previous
spectroscopic and interferometric observations have not been able to fully
constrain the system morphology and characteristics, we go one step further to
determine its orbital parameters, for which we need new interferometric
observations directly probing the inner parts of the system with a much higher
number of spatial frequencies. Methods. We use data obtained at eight different
epochs with the VLTI instruments AMBER and PIONIER in the H- and K-bands. We
performed aperture synthesis imaging to obtain the first model-independent view
of this system. We then modelled it as a binary (whose giant is spatially
resolved) that is surrounded by a circumbinary disc. Results. Combining these
interferometric measurements with previous radial velocities, we fully
constrain the orbit of the system. We then determine the mass of each star and
significantly revise the mass ratio. The M giant also appears to be almost
twice smaller than previously thought. Additionally, the low spectral
resolution of the data allows the flux of both stars and of the dusty disc to
be determined along the H and K bands, and thereby extracting their
temperatures. Conclusions. We find that the M giant actually does not stricto
sensus fill its Roche lobe. The mass transfer is more likely to occur through
the accretion of an important part of the giant wind. We finally rise the
possibility for an enhanced mass loss from the giant, and we show that an
accretion disc should have formed around the A star.Comment: 11 pages, 5 figures, published in A&A Appendix presenting reduced
data and extracted parameters Reduced data can be found on the CD
Formation of contact in massive close binaries
We present evolutionary calculations for 74 close binaries systems with
initial primary masses in the range 12...25 M_sun, and initial secondary masses
between 6 and 24 M_sun. The initial periods were chosen such that mass overflow
starts during the core hydrogen burning phase of the primary (Case A), or
shortly thereafter (Case B). We assume conservative evolution for contact-free
systems, i.e., no mass or angular momentum loss from those system except due to
stellar winds. We investigate the borderline between contact-free evolution and
contact, as a function of the initial system parameters. We also investigate
the effect of the treatment of convection, and found it relevant for contact
and supernova order in Case A systems, particularly for the highest considered
masses. For Case B systems we find contact for initial periods above
approximate 10 days and below. However, in that case (and for not too large
periods) contact occurs only after the mass ratio has been reversed, due to the
increased fraction of the donor's convective envelope. As most In all Cases we
find contact for mass ratios below approximate 0.65. We derive the observable
properties of our systems after the major mass transfer event, where the mass
gainer is a main sequence or supergiant O or early B type star, and the mass
loser is a helium star. We point out that the assumption of conservative
evolution for contact-free systems could be tested by finding helium star
companions to O stars.Comment: 19 pages, 14 figures, accepted by A&
- âŠ