231 research outputs found
3D hydrodynamical CO5BOLD model atmospheres of red giant stars: I. Atmospheric structure of a giant located near the RGB tip
We investigate the character and role of convection in the atmosphere of a
prototypical red giant located close to the red giant branch (RGB) tip with
atmospheric parameters, Teff=3660K, log(g)=1.0, [M/H]=0.0. Differential
analysis of the atmospheric structures is performed using the 3D hydrodynamical
and 1D classical atmosphere models calculated with the CO5BOLD and LHD codes,
respectively. All models share identical atmospheric parameters, elemental
composition, opacities and equation-of-state. We find that the atmosphere of
this particular red giant consists of two rather distinct regions: the lower
atmosphere dominated by convective motions and the upper atmosphere dominated
by wave activity. Convective motions form a prominent granulation pattern with
an intensity contrast (~18%) which is larger than in the solar models (~15%).
The upper atmosphere is frequently traversed by fast shock waves, with vertical
and horizontal velocities of up to Mach ~2.5 and ~6.0, respectively. The
typical diameter of the granules amounts to ~5Gm which translates into ~400
granules covering the whole stellar surface. The turbulent pressure in the
giant model contributes up to ~35% to the total (i.e., gas plus turbulent)
pressure which shows that it cannot be neglected in stellar atmosphere and
evolutionary modeling. However, there exists no combination of the
mixing-length parameter and turbulent pressure that would allow to
satisfactorily reproduce the 3D temperature-pressure profile with 1D atmosphere
models based on a standard formulation of mixing-length theory.Comment: 13 pages, 18 figures, accepted for publication in A&
The musical text of piano works by M. K. Ciurlionis - aspects of genesis [Zusammenfassung]: summary of the dissertation (Vilnius 2002)
Zusammenfassung einer Dissertation zum Werk von Mikalajus Konstantinas Ciurlioni
Galactic globular cluster 47 Tucanae: new ties between the chemical and dynamical evolution of globular clusters?
It is generally accepted today that Galactic globular clusters (GGCs) consist
of at least two generations of stars that are different in their chemical
composition and perhaps age. However, knowledge about the kinematical
properties of these stellar generations, which may provide important
information for constraining evolutionary scenarios of the GGCs, is still
limited. We therefore study the connections between chemical and kinematical
properties of different stellar generations in the Galactic globular cluster 47
Tuc. To achieve this goal, we used abundances of Li, O, and Na determined in
101 main sequence turn-off (TO) stars with the aid of 3D hydrodynamical model
atmospheres and NLTE abundance analysis methodology. We divided our sample TO
stars into three groups according to their position in the [Li/Na]-[Na/O] plane
to study their spatial distribution and kinematical properties. We find that
there are statistically significant radial dependencies of lithium and oxygen
abundances, A(Li) and A(O), as well as that of [Li/Na] abundance ratio. Our
results show that first-generation stars are less centrally concentrated and
dynamically hotter than stars belonging to subsequent generations. We also find
a significant correlation between the velocity dispersion and O and Na
abundance, and between the velocity dispersion and the [Na/O] abundance ratio.Comment: 4 pages, 6 figures, accepted for publication in A&
Three-dimensional hydrodynamical CO5BOLD model atmospheres of red giant stars VI. First chromosphere model of a late-type giant
Although observational data unequivocally point out to the presence of
chromospheres in red giant stars, no attempts have been made so far to model
them using 3D hydrodynamical model atmospheres. We therefore compute an
exploratory 3D hydrodynamical model atmosphere for a cool red giant in order to
study the dynamical and thermodynamic properties of its chromosphere, as well
as the influence of the chromosphere on its observable properties. 3D radiation
hydrodynamics simulations are carried out with the CO5BOLD model atmosphere
code for a star with the atmospheric parameters (Teff=4010 K, log g=1.5,
[M/H]=0.0), which are similar to those of the K-type giant star Aldebaran
(alpha Tau). ... we compute the emergent continuum intensity maps at different
wavelengths, spectral line profiles of Ca II K, the Ca II infrared triplet line
at 854.2nm, and H alpha, as well as the spectral energy distribution (SED) of
the emergent radiative flux. The initial model quickly develops a dynamical
chromosphere characterised by propagating and interacting shock waves. The peak
temperatures in the chromospheric shock fronts reach values on the order of up
to 5000 K although the shock fronts remain quite narrow. Like for the Sun, the
gas temperature distribution in the upper layers is composed of a cool
component due to adiabatic cooling in the expanding post-shock regions and a
hot component due to shock waves. For this red giant model, the hot component
is a rather flat high-temperature tail, which nevertheless affects the
resulting average temperatures significantly. The simulations show that the
atmospheres of red giant stars are dynamic and intermittent. Consequently, many
observable properties cannot be reproduced with one-dimensional static models
but demand for advanced 3D HD modelling. Furthermore, including a chromosphere
in the models might produce significant contributions to the emergent UV flux.Comment: 14 pages, 8 figures, A&A (2017, accepted
Convection and observable properties of late-type giants
We show that contrary to what is expected from 1D stationary model
atmospheres, 3D hydrodynamical modeling predicts a considerable influence of
convection on the spectral properties of late-type giants. This is due to the
fact that convection overshoots into the formally stable outer atmospheric
layers producing a notable granulation pattern in the 3D hydrodynamical models,
which has a direct influence on the observable spectra and colors. Within the
framework of standard 1D model atmospheres the average thermal stratification
of the 3D hydro model can not be reproduced with any reasonable choice of the
mixing length parameter and formulation of the turbulent pressure. The
differences in individual photometric colors -- in terms of 3D versus 1D --
reach up to ~0.2 mag, or \Delta Teff~70K. We discuss the impact of full 3D
hydrodynamical models on the interpretation of observable properties of
late-type giants, briefly mentioning problems and challenges which need to be
solved for bringing these models to a routine use within the astronomical
community in 5-10 years from now.Comment: 4 pages, 3 figures. Proceedings of the IAU Symposium 232 "The
Scientific Requirements for Extremely Large Telescopes", eds. P. Whitelock,
B. Leibundgut, and M. Dennefel
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