|
Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://crydee.sai.msu.ru/ftproot/pub/local/science/publications/
Дата изменения: Fri Mar 14 19:20:38 1997 Дата индексирования: Mon Dec 24 04:40:56 2007 Кодировка: koi8-r Поисковые слова: п п п п п п п п п п п п п п п п п п п п п п п п п р п р п р п р п р п р п р п р п р п п р п п р п п р п п р п |
All Postscript files are compressed with GNU zip (gzip). If you're
running some flavor of UNIX, you already have it (type
gzip -d filename). gzip for OS/2 can be
retrieved here. All these files are also
accessible via ftp.
If you don't have Postscript printer, get and install Ghostscript for your OS. Ask local computer guru if needed.
[ Chiwriter 3.x, Grapher, in Russian (66KB) ]
Abstract
Given the chemical composition (hydrogen abundance mainly), the mass and
internal physics, the structure of the star is determined uniquely.
The commonly used method for the choice of the hydrogen abundance
profile in the model of the present Sun is evolutionary calculations.
But the existing uncertainties in physics and evolution give us an idea
to consider a more extended set of possible solar models. We consider
models with solar values of radius, luminosity and mass, but with an
arbitrary profiles of hydrogen abundance in the core. Of course,
to get up to solar values, profile X(m/M)
must satisfy some (nonstrict) restrictions, which are determined by fitting.
In this poster we propose a hypothesis that within fixed assumptions about internal physics (opacity, thermodynamics, nuclear reactions) a strict relation between the surface helium abundance and the entropy of the adiabatic part of the convective zone exists for all solar models. This hypothesis is verified with models under simplified physics (Christensen-Dalsgaard 1988) and with six evolutionary models computed by Christensen-Dalsgaard (1992). Such relation mainly depends on the functions of the opacities in radiative zone between the lower boundary of convection and the region of nuclear reactions. The possibilities of the agreement between such relation and helioseismic determination of surface helium abundance and entropy is discussed.
[ LaTeX, Figure 1 | Postscript (37KB) ]
[ Postscript, in Russian, no figures (140KB) ]
Abstract
We propose
to use the surface helium abundance Y and the specific plasma entropy Scnv
in the adiabatic part of the convective zone for the solar model
comparison. The influence of the opacity and the hydrogen abundance profile
modifications on the model position on the (Y,Scnv) plane is discussed.
It is revealed that
such variations (when localized in the energy-generating core)
shift the solar model along a straight line. Opacity increasing
in the radiative zone results in this line shift to higher Y.
[ ASCII (866) | ASCII (KOI8) | Figure 1 | Postscript, in Russian (620KB) ]
Abstract
Standard solar models with five different opacity tables are
computed. Replacing the Los Alamos opacities with the Livermore ones results
in the increase of the convection zone depth by 0.015Rsun and surface helium
abundance (by mass) by 1.5% up to approximately 28% (Grevesse mixture).
[ ASCII (866) | ASCII (KOI8) | Figure 1 | Postcript, in Russian (275KB) ]
Abstract
A variety of solar models (namely, models of stars having solar values of
mass, radius, luminosity) is a subject of our study. The hydrogen profile in
the star's interior is usually determined by course of the evolution, but we
also consider models with arbitrary hydrogen profiles or diffusion profiles
also. Applying additional restrictions on the model which follow from recent
helioseismic results we consider the question of existence of the models.
These restrictions are: 1) calibration of the surface helium abundance and
the specific entropy in the convection zone (Vorontsov et al. 1991; Baturin,
Vorontsov 1994; there are few results on the helium calibration but we used
cited ones because they contain simultaneous determination of the helium and
the entropy); 2) estimation of the convection zone depth
(Christensen-Dalsgaard et al., 1991); 3) sound speed profile inferred from
oscillation frequencies (Vorontsov, Shibahashi 1992). These results are
basically independent of a specific solar model. Hereafter we roughly divide
a regular solar model into three zones: 1) the outer convection zone (the
envelope); the chemical composition and specific entropy are constant there;
2) the radiative zone; the chemical composition is constant there when
diffusion isn't taken into account; the structure of this area depends
mainly on the opacity; 3) the energy-generating core where the thermonuclear
reactions are significant; there is definitely variable hydrogen/helium
profile. Commonly speaking we study the possibility of fitting some cores
and convection zones while the fit conditions are determined by the
radiative zone...
[ Postscript, long preliminary version (38KB) | Postscript, final version (210KB) ]
[ ChiWriter 3.x (ouch!), in Russian ]
Abstract
Given the chemical composition profile and mass the internal structure of
the star is determined by Vogt-Russell theorem. It gives that this model
will have definite radius and luminosity (and they will not be equal to
solar ones). So we need two parameters to adjust when computing static solar
model. While computing the standard model these two parameters are initial
chemical composition and convection theory parameter controlling te
temperature gradient in the outermost layers. This choice is rather
arbitrary and done due to lack of knowledge about these values. In the other
words, these values were transformed from the parameters to the results
(e.g., the solar evolution modelling gives the best estimate of the presolar
helium abundance). The other results are neutrino fluxes, convection zone
depth, oscillation spectrum etc. The input data (nuclear reactions, opacity,
equation of state and description of convection) may contain significant
errors, especially opacity. And there is a question: how can these error
alter our results?
In this work we try to investigate some aspects of this problem. First, we replace the convection theory parameter with the entropy of the adiabatic part of the convection zone. Second, we study the influence of the opacity tables on the solar models. Third, we analyze the connections between the model parameters and the hydrogen profile and the opacities in the nonstandard models.
Abstract
We present the results of high-precision computing of standard solar models
with different opacity tables. A comparative analysis of models is done
utilizing two key parameters--helium abundance and specific entropy in the
convection zone. The influence of stellar opacity on these two parameters is
studied. Comparison of standard models with different opacities shows that
the increase of the opacity in the radiative zone causes decrease of entropy
whereas the increase of the opacity in the energy-generating core leads to
higher helium abundance. Investigation of nonstandard static models points
out that the common relation between the specific entropy and opacity in the
radiative zone of the Sun (outside of nuclear reactions region).
[ Postscript, in Russian, no figures (850KB) | LaTeX plus figures (KB) | Postscript, in English, with figures (KB) ]
Published in: Bull. Astr. Soc. India, 1996, 24, 329.
[
TeX |
Figure 1 |
Figure 2 |
Postscript (42KB)
]
This poster was not presented actually. I wish I were there....
Abstract
The problem of computation of the model of the present Sun with given sound
speed profile in the solar radiative zone is considered. It is shown that
the chemical composition is still a free parameter but the entropy of the
adiabatic part of the convection zone is determined by this procedure.
Parameters of the models are compared with the helioseismic calibration of
solar envelope and the disagreement is revealed. A study of the seismic
properties of the models' cores indicates that the best model is the one
closest to the standard solar model.
[ Postscript, in Russian, no figures (1680KB) | LaTeX plus figures (87KB) | Postscript, in English, with figures (145KB) ]
Abstract
Three alternative approaches in evaluating of the
entropy of the adiabatic part of the solar convection zone are compared.