4,661 research outputs found
Stellar mass-loss near the Eddington limit. Tracing the sub-photospheric layers of classical Wolf-Rayet stars
Towards the end of their evolution hot massive stars develop strong stellar
winds and appear as emission line stars, such as WR stars or LBVs. The
quantitative description of the mass loss in these important pre-SN phases is
hampered by unknowns such as clumping and porosity due to an in-homogeneous
wind structure, and by an incomplete theoretical understanding of optically
thick stellar winds. In this work we investigate the conditions in deep
atmospheric layers of WR stars to find out whether these comply with the theory
of optically thick winds, and whether we find indications of clumping in these
layers. We use a new semi-empirical method to determine sonic-point optical
depths, densities, and temperatures for a large sample of WR stars of the
carbon (WC) and oxygen (WO) sequence. Based on an artificial model sequence we
investigate the reliability of our method and its sensitivity to uncertainties
in stellar parameters. We find that the WR stars in our sample obey an
approximate relation with P_rad/P_gas~80 at the sonic point. This 'wind
condition' is ubiquitous for radiatively driven, optically thick winds, and
sets constraints on possible wind/envelope solutions affecting radii, mass-loss
rates, and clumping properties. Our results suggest that the presence of an
optically thick wind may force many stars near the Eddington limit to develop
clumped, radially extended sub-surface zones. The clumping in these zones is
most likely sustained by the non-linear strange-mode instability, and may be
the origin of the observed wind clumping. The properties of typical late-type
WC stars comply with this model. Solutions without sub-surface clumping and
inflation are also possible but demand for compact stars with comparatively low
mass-loss rates. These objects may resemble the small group of WO stars with
their exceptionally hot stellar temperatures and highly ionized winds.Comment: accepted by A&
Narrow He II emission in star-forming galaxies at low metallicity. Stellar wind emission from a population of Very Massive Stars
In a recent study star-forming galaxies with HeII emission between redshifts
2 and 4.6 have been found to occur in two modes, distinguished by the width of
their HeII emission lines. Broad HeII emission has been attributed to stellar
emission from a population of evolved Wolf-Rayet (WR) stars while narrow HeII
emission has been attributed to nebular emission excited by a population of
very hot PopIII stars formed in pockets of pristine gas at moderate redshifts.
In this work we propose an alternative scenario for the origin of the narrow
HeII emission, namely very massive stars (VMS) at low metallicity (Z) which
form strong but slow WR-type stellar winds due to their proximity to the
Eddington limit. We estimate the expected HeII line fluxes and equivalent
widths based on wind models for VMS and population synthesis models, and
compare the results with recent observations of star-forming galaxies at
moderate redshifts. The observed HeII line strengths and equivalent widths are
in line with what is expected for a population of VMS in one or more young
super-clusters located within these galaxies. In our scenario the two observed
modes of HeII emission originate from massive stellar populations in distinct
evolutionary stages at low Z. If this interpretation is correct there is no
need to postulate the existence of PopIII stars at moderate redshifts to
explain the observed narrow HeII emission. An interesting possibility is the
existence of self-enriched VMS with similar WR-type spectra at extremely low Z.
Stellar HeII emission from such very early generations of VMS may be detectable
in future studies of star-forming galaxies at high redshifts with the James
Webb Space Telescope. The fact that the HeII emission of VMS is largely
neglected in current population synthesis models will generally affect the
interpretation of the integrated spectra of young stellar populations.Comment: 4 pages, 1 figure, A&A letters (accepted
Bladvlekken zomerbloemen : meer veroorzakers, dus extra alert reageren
Bladvlekkenziekten veroorzaken regelmatig problemen in de teelten van verschillende soorten zomerbloemen. Bladvlekken kunnen door verschillende ziekteverwekkende schimmels worden veroorzaakt
Bladvlekken in zomerbloemen 2 : vervolg op onderzoek 2007-2008
Bladvlekkenziekten veroorzaken regelmatig problemen in de teelten van verschillende soorten zomerbloemen. Bladvlekken kunnen door verschillende ziekteverwekkende schimmels worden veroorzaakt. Om een betrouwbaar en gericht advies te geven is het van belang om te weten welk organisme de bladvlekken veroorzaakt. In dit project zijn monsters met bladvlekken bij telers verzameld en is met behulp van de infectieproeven getracht de veroorzaker aan te wijzen
Jets as diagnostics of the circumstellar medium and the explosion energetics of supernovae: the case of Cas A
We present hydrodynamical models for the Cassiopeia A (Cas A) supernova
remnant and its observed jet / counter-jet system. We include the evolution of
the progenitor's circumstellar medium, which is shaped by a slow red supergiant
wind that is followed by a fast Wolf-Rayet (WR) wind.
The main parameters of the simulations are the duration of the WR phase and
the jet energy. We find that the jet is destroyed if the WR phase is
sufficiently long and a massive circumstellar shell has formed. We therefore
conclude that the WR phase must have been short (a few thousand yr), if present
at all. Since the actual jet length of Cas A is not known we derive a lower
limit for the jet energy, which is ~10^{48} erg. We discuss the implications
for the progenitor of Cas A and the nature of its explosion.Comment: 9 pages, 5 figures, ApJ accepted. Version with high resolution
figures available at http://www.phys.uu.nl/~schure/CasA_jet.pd
The main transition in the Pink membrane model: finite-size scaling and the influence of surface roughness
We consider the main transition in single-component membranes using computer
simulations of the Pink model [D. Pink {\it et al.}, Biochemistry {\bf 19}, 349
(1980)]. We first show that the accepted parameters of the Pink model yield a
main transition temperature that is systematically below experimental values.
This resolves an issue that was first pointed out by Corvera and co-workers
[Phys. Rev. E {\bf 47}, 696 (1993)]. In order to yield the correct transition
temperature, the strength of the van der Waals coupling in the Pink model must
be increased; by using finite-size scaling, a set of optimal values is
proposed. We also provide finite-size scaling evidence that the Pink model
belongs to the universality class of the two-dimensional Ising model. This
finding holds irrespective of the number of conformational states. Finally, we
address the main transition in the presence of quenched disorder, which may
arise in situations where the membrane is deposited on a rough support. In this
case, we observe a stable multi-domain structure of gel and fluid domains, and
the absence of a sharp transition in the thermodynamic limit.Comment: submitted to PR
An explanation for the curious mass loss history of massive stars: from OB stars, through Luminous Blue Variables to Wolf-Rayet stars
The stellar winds of massive stars show large changes in mass-loss rates and
terminal velocities during their evolution from O-star through the Luminous
Blue Variable phase to the Wolf-Rayet phase. The luminosity remains
approximately unchanged during these phases. These large changes in wind
properties are explained in the context of the radiation driven wind theory, of
which we consider four different models. They are due to the evolutionary
changes in radius, gravity and surface composition and to the change from
optically thin (in continuum) line driven winds to optically thick radiation
driven winds.Comment: Accepted for publication in Astronomy and Astrophysics (Letter to the
Editor
Cladosporium Ă©n Botrytis belangrijkste oorzaken bladvlekken in pioenroos
De schimmels Cladosporium paeoniae en Botrytis spp. veroorzaken verschillende soorten bladvlekken in pioenroos. PPO zocht uit welke schimmels of bacteriën in de bladvlekken aanwezig waren. Met deze kennis is het mogelijk om bladvlekkenziekten gerichter aan te pakken
On the nature of the bi-stability jump in the winds of early-type supergiants
We study the origin of the observed bi-stability jump in the terminal
velocity of the winds of supergiants near spectral type B1. To this purpose, we
have calculated a grid of wind models and mass-loss rates for these stars. The
models show that the mass-loss rate 'jumps' by a factor of five around spectral
type B1. Up to now, a theoretical explanation of the observed bi-stability jump
was not yet provided by radiation driven wind theory. The models demonstrate
that the subsonic part of the wind is dominated by the line acceleration due to
Fe. The elements C, N and O are important line drivers in the supersonic part
of the wind. We demonstrate that the mass-loss rate 'jumps' due to an increase
in the line acceleration of Fe III below the sonic point. Finally, we discuss
the possible role of the bi-stability jump on the mass loss during typical
variations of Luminous Blue Variable stars.Comment: Accepted by A&A, 19 pages Latex, 10 figure
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