5 research outputs found
New mass-loss rates of Magellanic Cloud B supergiants from global wind models
We provide global models of line-driven winds of B supergiants for
metallicities corresponding to the Large and Small Magellanic Clouds. The
velocity and density structure of the models is determined consistently from
hydrodynamical equations with radiative force derived in the comoving frame and
level populations computed from kinetic equilibrium equations. We provide a
formula expressing the predicted mass-loss rates in terms of stellar
luminosity, effective temperature, and metallicity. Predicted wind mass-loss
rates decrease with decreasing metallicity as and are
proportional to the stellar luminosity. The mass-loss rates increase below the
region of the bistability jump at about 20\,kK because of iron recombination.
In agreement with previous theoretical and observational studies, we find a
smooth change of wind properties in the region of the bistability jump. With
decreasing metallicity, the bistability jump becomes weaker and shifts to lower
effective temperatures. At lower metallicities above the bistability jump, our
predictions provide similar rates to those used in current evolutionary models,
but our rates are significantly lower than older predictions below the
bistability jump. Our predicted mass-loss rates agree with observational
estimates derived from H line assuming that observations of stellar
winds from Galaxy and the Magellanic Clouds are uniformly affected by clumping.
The models nicely reproduce the dependence of terminal velocities on
temperature derived from ultraviolet spectroscopy.Comment: 8 pages, accepted for publication in Astronomy & Astrophysic
Stellar wind models of central stars of planetary nebulae
Fast line-driven stellar winds play an important role in the evolution of
planetary nebulae. We provide global hot star wind models of central stars of
planetary nebulae. The models predict wind structure including the mass-loss
rates, terminal velocities, and emergent fluxes from basic stellar parameters.
We applied our wind code for parameters corresponding to evolutionary stages
between the asymptotic giant branch and white dwarf phases. We study the
influence of metallicity and wind inhomogeneities (clumping) on the wind
properties. Line-driven winds appear very early after the star leaves the
asymptotic giant branch (at the latest for T_\rm{eff}\approx10\,kK) and fade
away at the white dwarf cooling track (below T_\rm{eff}=105\,kK). Their
mass-loss rate mostly scales with the stellar luminosity and, consequently, the
mass-loss rate only varies slightly during the transition from the red to the
blue part of the Hertzsprung-Russell diagram. There are the following two
exceptions to the monotonic behavior: a bistability jump at around kK,
where the mass-loss rate decreases by a factor of a few (during evolution) due
to a change in iron ionization, and an additional maximum at about
T_\rm{eff}=40-50\,kK. On the other hand, the terminal velocity increases from
about a few hundreds of to a few thousands of
during the transition as a result of stellar radius
decrease. The wind terminal velocity also significantly increases at the
bistability jump. Derived wind parameters reasonably agree with observations.
The effect of clumping is stronger at the hot side of the bistability jump than
at the cool side. Derived fits to wind parameters can be used in evolutionary
models and in studies of planetary nebula formation. A predicted bistability
jump in mass-loss rates can cause the appearance of an additional shell of
planetary nebula.Comment: 14 pages, accepted for publication in Astronomy & Astrophysic
Understanding the rotational variability of K2 targets. HgMn star KIC 250152017 and blue horizontal branch star KIC 249660366
Ultraprecise space photometry enables us to reveal light variability even in
stars that were previously deemed constant. A large group of such stars show
variations that may be rotationally modulated. This type of light variability
is of special interest because it provides precise estimates of rotational
rates. We aim to understand the origin of the light variability of K2 targets
that show signatures of rotational modulation. We used phase-resolved
medium-resolution XSHOOTER spectroscopy to understand the light variability of
the stars KIC~250152017 and KIC~249660366, which are possibly rotationally
modulated. We determined the atmospheric parameters at individual phases and
tested the presence of the rotational modulation in the spectra. KIC 250152017
is a HgMn star, whose light variability is caused by the inhomogeneous surface
distribution of manganese and iron. It is only the second HgMn star whose light
variability is well understood. KIC 249660366 is a He-weak, high-velocity
horizontal branch star with overabundances of silicon and argon. The light
variability of this star is likely caused by a reflection effect in this
post-common envelope binary.Comment: 8 pages, accepted for publication in Astronomy & Astrophysic
Hot subdwarf wind models with accurate abundances I. Hydrogen dominated stars HD 49798 and BD+182647
Hot subdwarfs are helium burning objects in late stages of their evolution.
These stars can develop winds driven by light absorption in the lines of
heavier elements. The wind strength depends on chemical composition which can
significantly vary from star to star. We aim to understand the influence of
metallicity on the strength of the winds of the hot hydrogen-rich subdwarfs HD
49798 and BD+182647. We used UV and optical spectra to derive stellar
parameters and abundances. For derived stellar parameters, we predicted wind
structure (including mass-loss rates and terminal velocities) with our METUJE
code. We derived effective temperature K and mass
for HD 49798 and K and
for BD+182647. The abundances can be interpreted as
a result of interplay between stellar evolution and diffusion. HD 49798 has a
strong wind that does not allow for chemical separation and consequently it
shows solar chemical composition modified by hydrogen burning. On the other
hand, we did not find any wind in BD+182647 and its abundances are
therefore most likely affected by radiative diffusion. Accurate abundances do
not lead to a significant modification of wind mass-loss rate for HD 49798,
because the increase of the contribution of Fe and Ni to the radiative force is
compensated by the decrease of the force due to other elements. The resulting
wind mass-loss rate predicts
an X-ray light curve during the eclipse which closely agrees with observations.
On the other hand, the absence of the wind in BD+182647 for accurate
abundances is a result of its peculiar chemical composition. Wind models with
accurate abundances provide more reliable wind parameters, but the influence of
abundances on the wind parameters is limited in many cases.Comment: 11 pages, accepted for publication in Astronomy & Astrophysic