971 research outputs found
Atmospheres and Winds of PN Central Stars
The progress over the last years in modelling the atmospheres and winds of PN
central stars is reviewed. We discuss the effect of the inclusion of the
blanketing by millions of metal lines in NLTE on the diagnostics of
photospheric and stellar wind lines, which can be used to determine stellar
parameters such as effective temperature, gravity, radius, mass loss rate and
distance. We also refer to recent work on the winds of massive O-type stars,
which indicates that their winds are possibly inhomogeneous and clumped. We
investigate implications from this work on the spectral diagnostics of PN
central stars and introduce a method to determine wind clumping factors from
the relative strengths of Halpha and HeII 4686. Based on new results we discuss
the wind properties of CSPN.Comment: 8 pages, 12 figures; Proceedings, IAU Symposium No. 234, 2006,
"Planetary Nebulae in our Galaxy and Beyond", M.J. Barlow and R.H. Mendez,
ed
2D wind clumping in hot, massive stars from hydrodynamical line-driven instability simulations using a pseudo-planar approach
Context: Clumping in the radiation-driven winds of hot, massive stars arises
naturally due to the strong, intrinsic instability of line-driving (the `LDI').
But LDI wind models have so far mostly been limited to 1D, mainly because of
severe computational challenges regarding calculation of the multi-dimensional
radiation force. Aims: To simulate and examine the dynamics and
multi-dimensional nature of wind structure resulting from the LDI. Methods: We
introduce a `pseudo-planar', `box-in-a-wind' method that allows us to
efficiently compute the line-force in the radial and lateral directions, and
then use this approach to carry out 2D radiation-hydrodynamical simulations of
the time-dependent wind. Results: Our 2D simulations show that the LDI first
manifests itself by mimicking the typical shell-structure seen in 1D models,
but how these shells then quickly break up into complex 2D density and velocity
structures, characterized by small-scale density `clumps' embedded in larger
regions of fast and rarefied gas. Key results of the simulations are that
density-variations in the well-developed wind statistically are quite isotropic
and that characteristic length-scales are small; a typical clump size is ~0.01R
at 2R, thus resulting also in rather low typical clump-masses ~10^17 g.
Overall, our results agree well with the theoretical expectation that the
characteristic scale for LDI-generated wind-structure is of order the Sobolev
length. We further confirm some earlier results that lateral `filling-in' of
radially compressed gas leads to somewhat lower clumping factors in 2D
simulations than in comparable 1D models. We conclude by discussing an
extension of our method toward rotating LDI wind models that exhibit an
intriguing combination of large- and small-scale structure extending down to
the wind base.Comment: 9 pages, 7 figures + 1 Appendix with 1 figure. Recommended for
publication in A&
Mass loss from inhomogeneous hot star winds III. An effective-opacity formalism for line radiative transfer in accelerating, clumped two-component media, and first results on theory and diagnostics
[Abridged] We develop and benchmark a fast and easy-to-use effective-opacity
formalism for line and continuum radiative transfer in an accelerating
two-component clumpy medium. The formalism bridges the limits of optically thin
and thick clumps, and is here used to i) design a simple vorosity-modified
Sobolev with exact integration (vmSEI) method for analyzing UV wind resonance
lines in hot, massive stars, and ii) derive simple correction factors to the
line force driving the outflows of such stars. We show that (for a given
ionization factor) UV resonance doublets may be used to analytically predict
the upward corrections in empirically inferred mass-loss rates associated with
porosity in velocity space (a.k.a. velocity-porosity, or vorosity), but that
severe solution degeneracies exist. For an inter-clump density set to 1 % of
the mean density, we for O and B supergiants derive upward empirical mass-loss
corrections of typically factors of either ~5 or ~50, depending on which of the
two applicable solutions is chosen. Overall, our results indicate this solution
dichotomy severely limits the use of UV resonance lines as direct mass-loss
indicators of clumped hot stellar winds. We next apply the effective-opacity
formalism to the standard CAK theory of line-driven winds. By analytic and
numerical hydrodynamics calculations, we show that in cases where vorosity is
important at the critical point setting the mass-loss rate, the reduced
line-force leads to a lower theoretical mass loss, by a factor scaling with the
normalized velocity filling factor fvel. On the other hand, if vorosity is
important only above this critical point, the predicted mass loss is not
affected, but the wind terminal speed is reduced. This shows that porosity in
velocity space can have a significant impact not only on the diagnostics, but
also on the dynamics and theory of radiatively driven winds.Comment: 13 pages, 8 figures, accepted for publication in Astronomy and
Astrophysic
Carbon line formation and spectroscopy in O-type stars
The determination of chemical abundances constitutes a fundamental
requirement for obtaining a complete picture of a star. Particularly in massive
stars, CNO abundances are of prime interest, due to the nuclear CNO-cycle and
various mixing processes which bring these elements to the surface.
We aim at enabling a reliable carbon spectroscopy for our unified NLTE
atmosphere code FASTWIND.
We develop a new carbon model atom including CII/III/IV/V, and discuss
problems related to carbon spectroscopy in O-type stars. We describe different
tests to examine the reliability of our implementation, and investigate which
mechanisms influence the carbon ionization balance. By comparing with
high-resolution spectra from six O-type stars, we check in how far
observational constraints can be reproduced by our new carbon line synthesis.
Carbon lines are even more sensitive to a variation of temperature, gravity,
and mass-loss rate, than hydrogen/helium lines. We are able to reproduce most
of the observed lines from our stellar sample, and to estimate those specific
carbon abundances which bring the lines from different ions into agreement. For
hot dwarfs and supergiants earlier than O7, X-rays from wind-embedded shocks
can impact the synthesized line strengths, particularly for CIV, potentially
affecting the abundance determination.
We have demonstrated our capability to derive realistic carbon abundances by
means of FASTWIND, using our recently developed model atom. We found that
complex effects can have a strong influence on the carbon ionization balance in
hot stars. For a further understanding, the UV range needs to be explored as
well. By means of detailed nitrogen and oxygen model atoms available to use, we
will be able to perform a complete CNO abundance analysis for larger samples of
massive stars, and to provide constraints on corresponding evolutionary models
and aspects.Comment: 22 pages, 16 figures, 6 table
Mass loss from inhomogeneous hot star winds II. Constraints from a combined optical/UV study
Mass-loss rates currently in use for hot, massive stars have recently been
seriously questioned, mainly because of the effects of wind clumping. We
investigate the impact of clumping on diagnostic ultraviolet resonance and
optical recombination lines. Optically thick clumps, a non-void interclump
medium, and a non-monotonic velocity field are all accounted for in a single
model. We used 2D and 3D stochastic and radiation-hydrodynamic (RH) wind
models, constructed by assembling 1D snapshots in radially independent slices.
To compute synthetic spectra, we developed and used detailed radiative transfer
codes for both recombination lines (solving the "formal integral") and
resonance lines (using a Monte-Carlo approach). In addition, we propose an
analytic method to model these lines in clumpy winds, which does not rely on
optically thin clumping. Results: Synthetic spectra calculated directly from
current RH wind models of the line-driven instability are unable to in parallel
reproduce strategic optical and ultraviolet lines for the Galactic O-supergiant
LCep. Using our stochastic wind models, we obtain consistent fits essentially
by increasing the clumping in the inner wind. A mass-loss rate is derived that
is approximately two times lower than predicted by the line-driven wind theory,
but much higher than the corresponding rate derived from spectra when assuming
optically thin clumps. Our analytic formulation for line formation is used to
demonstrate the potential impact of optically thick clumping in weak-winded
stars and to confirm recent results that resonance doublets may be used as
tracers of wind structure and optically thick clumping. (Abridged)Comment: 14 pages+1 Appendix, 8 figures, 3 tables. Accepted for publication in
Astronomy and Astrophysics. One reference updated, minor typo in Appendix
correcte
The Performance Analysis of Two Relatively Small Capacity Urban Retrofit Stormwater Controls
This paper details field investigations that were conducted on the performance of small capacity urban retrofit stormwater control measures. The objective of the two year study (2013–2015) was to provide performance data on stormwater retrofits that could not be fully sized according to conventional standards due to space constraints. In many states performance credits are not granted to stormwater management controls that are not designed to manage regionally derived water quality volumes. In retrofit applications there may exist numerous limitations to conventionally sized systems such as limited rights of way, setback distances or existing utilities. The larger scale objective of green infrastructure implementation is to improve receiving water quality and therefore even undersized systems, to some extent, meet this objective.
This study introduces data on two systems: an innovative bioretention design with a water treatment residual amended filter media and an internal storage reservoir; and an undersized linear subsurface gravel wetland sized to optimize both phosphorus and nitrogen removal. The systems were retrofitted into existing developed areas and were sized at less than the water quality volume due to limited space at each location. The bioretention system (IBSC) was constructed in a commercial area in the town of Durham, NH in summer 2011 and the subsurface gravel wetland system (SGWSC) was constructed in a narrow drainage right of way in a residential neighbourhood of Durham, NH in the fall of 2013.
Sediment and metal removals for both undersized systems were high with median removal efficiencies in the SGW of 75% for both total suspended solids (TSS) and total zinc (TZn). The Durham IBSC recorded median removal efficiency (RE) of 86% for TSS and TZn. Total phosphorus (TP) REs were higher than conventional bioretention systems with the subsurface gravel wetland system achieving a median RE of 53% and the Durham IBSC achieving a median RE of 40% for TP. Both systems reduced total nitrogen (TN) by approximately 20% (23% for SGWSC and 21% for Durham IBSC) with median effluent concentrations of 1.4 mg/L. This project was funded by the U.S. Environmental Protection Agency Region 1, Regional Applied Research Effort (RARE) Program. Additional information can be found in the full project report Performance Analysis of Two Relatively Small Capacity Urban Retrofit Stormwater Controls (Houle et al. 2015)
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