657 research outputs found
A Clumping Independent Diagnostic of Stellar Mass-loss Rates: Rapid Clump Destruction in Adiabatic Colliding Winds
Clumping in hot star winds can significantly affect estimates of mass-loss
rates, the inferred evolution of the star and the environmental impact of the
wind. A hydrodynamical simulation of a colliding winds binary (CWB) with clumpy
winds reveals that the clumps are rapidly destroyed after passing through the
confining shocks of the wind-wind collision region (WCR) for reasonable
parameters of the clumps if the flow in the WCR is adiabatic. Despite large
density and temperature fluctuations in the post-shock gas, the overall effect
of the interaction is to smooth the existing structure in the winds. Averaged
over the entire interaction region, the resulting X-ray emission is very
similar to that from the collision of smooth winds. The insensitivity of the
X-ray emission to clumping suggests it is an excellent diagnostic of the
stellar mass-loss rates in wide CWBs, and may prove to be a useful addition to
existing techniques for deriving mass-loss rates, many of which are extremely
sensitive to clumping. Clumpy winds also have implications for a variety of
phenomena at the WCR: particle acceleration may occur throughout the WCR due to
supersonic MHD turbulence, re-acceleration at multiple shocks, and
re-connection; a statistical description of the properties of the WCR may be
required for studies of non-equilibrium ionization and the rate of electron
heating; and the physical mixing of the two winds will be enhanced, as seems
necessary to trigger dust formation.Comment: 4 pages, 3 figures, accepted for publication in ApJ
Non-thermal X-ray and Gamma-ray Emission from the Colliding Wind Binary WR140
WR140 is the archetype long-period colliding wind binary (CWB) system, and is
well known for dramatic variations in its synchrotron emission during its
7.9-yr, highly eccentric orbit. This emission is thought to arise from
relativistic electrons accelerated at the global shocks bounding the
wind-collision region (WCR). The presence of non-thermal electrons and ions
should also give rise to X-ray and gamma-ray emission from several separate
mechanisms, including inverse-Compton cooling, relativistic bremsstrahlung, and
pion decay. We describe new calculations of this emission and make some
preliminary predictions for the new generation of gamma-ray observatories. We
determine that WR140 will likely require several Megaseconds of observation
before detection with INTEGRAL, but should be a reasonably strong source for
GLAST.Comment: 4 pages, 1 figure, contribution to "Massive Stars and High-Energy
Emission in OB Associations"; JENAM 2005, held in Liege (Belgium
Winds in Collision: high-energy particles in massive binary systems
High-resolution radio observations have revealed that non-thermal radio
emission in WR stars arises where the stellar wind of the WR star collides with
that of a binary companion. These colliding-wind binary (CWB) systems offer an
important laboratory for investigating the underlying physics of particle
acceleration. Hydrodynamic models of the binary stellar winds and the
wind-collision region (WCR) that account for the evolution of the electron
energy spectrum, largely due to inverse Compton cooling, are now available.
Radiometry and imaging obtained with the VLA, MERLIN, EVN and VLBA provide
essential constraints to these models. Models of the radio emission from WR146
and WR147 are shown, though these very wide systems do not have defined orbits
and hence lack a number of important model parameters. Multi-epoch VLBI imaging
of the archetype WR+O star binary WR140 through a part of its 7.9-year orbit
has been used to define the orbit inclination, distance and the luminosity of
the companion star to enable the best constraints for any radio emitting CWB
system. Models of the spatial distribution of relativistic electrons and ions,
and the magnetic energy density are used to model the radio emission, and also
to predict the high energy emission at X-ray and gamma-ray energies. It is
clear that high-energy facilities e.g. GLAST and VERITAS, will be important for
constraining particle acceleration parameters such as the spectral index of the
energy spectrum and the acceleration efficiency of both ions and electrons, and
in turn, identify unique models for the radio spectra. This will be especially
important in future attempts to model the spectra of WR140 throughout its
complete orbit. A WCR origin for the synchrotron emission in O-stars, the
progenitors of WR stars, is illustrated by observations of Cyg OB2 No. 9.Comment: Invited review at the 8th EVN Symposium, Torun September 26-29, 2006.
11 pages, 12 figure
3D Models of Radiatively Driven Colliding Winds In Massive O+O Star Binaries: I. Hydrodynamics
The dynamics of the wind-wind collision in massive stellar binaries is
investigated using three-dimensional hydrodynamical models which incorporate
gravity, the driving of the winds, the orbital motion of the stars, and
radiative cooling of the shocked plasma. In this first paper we restrict our
study to main-sequence O+O binaries. The nature of the wind-wind collision
region is highly dependent on the degree of cooling of the shocked plasma, and
the ratio of the flow timescale of the shocked plasma to the orbital timescale.
The pre-shock wind speeds are lower in close systems as the winds collide prior
to their acceleration to terminal speeds. Radiative inhibition may also reduce
the pre-shock wind speeds. Together, these effects can lead to rapid cooling of
the post-shock gas. Radiative inhibition is less important in wider systems,
where the winds are accelerated to higher speeds before they collide, and the
resulting collision region can be largely adiabatic. In systems with eccentric
orbits, cold gas formed during periastron passage can persist even at apastron,
before being ablated and mixed into its surroundings and/or accelerated out of
the system.Comment: 21 pages, 15 figures, accepted for publication in MNRA
The dominant X-ray wind in massive star binaries
We investigate which shocked wind is responsible for the majority of the
X-ray emission in colliding wind binaries, an issue where there is some
confusion in the literature, and which we show is more complicated than has
been assumed. We find that where both winds rapidly cool (typically close
binaries), the ratio of the wind speeds is often more important than the
momentum ratio, because it controls the energy flux ratio, and the faster wind
is generally the dominant emitter. When both winds are largely adiabatic
(typically long-period binaries), the slower and denser wind will cool faster
and the stronger wind generally dominates the X-ray luminosity.Comment: 4 pages, 1 figure, accepted by A&A Letter
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