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"International Meeting During The Total Solar Eclipse 2006" A great possibility to attend a meeting while preparing for observations and experiments and to do it right on the spot, on the line of totality. |
Conference Programme Sunday, March 26 - REGISTRATION and WELCOME RECEPTION Monday, March 27: SOLAR SYSTEM PHYSICS - BREAKFAST and REGISTRATION - OPENING / ANNOUNCEMENTS - SESSION 1 (Chair person: Edward GUINAN) 11:10
- 12:00 A. GIMENEZ - (INVITED) Planetary Transits - LUNCH BREAK - SESSION 2 (Chair person: Edwin BUDDING) 15:10
- 15:30 P. HEINZEL - Solar Prominences From
Space and Through Eclipses 16:10
- 16:30 (Chair
person: Eleni ROVITHIS-LIVANIOU) 18:10
- 18:30 O. A.-VUKMANOVIC - Solution of NLTE Radiative Transfer Problems
Using Forth-and-Back Implicit Lambda Iteration - DINNER - WINE PARTY AROUND BONFIRE AT THE BEACH Tuesday, March 28: STELLAR PHYSICS - BREAKFAST - SESSION 3 (Chair person: Alvaro GIMENEZ) 11:20
- 11:40 O. DEMİRCAN - Solar and Stellar Rotation - LUNCH BREAK - SESSION 4 (Chair person: Osman DEMİRCAN) 15:10
- 15:30 R. GAUDERON - Eclipsing Binaries in the SMC: Combining VLT Multi-Object Spectroscopy with OGLE Photometry (Chair
person: Zeki EKER) 18:10
- 18:30 - DINNER - SIGHT SEEING TOUR TO Wednesday, March 29: SOLAR ECLIPSE OBSERVATIONS - BREAKFAST - SESSION 5 (Chair person: Vladan
ČELEBONOVIĆ) 10:10
- 10:30 E. ROVITHIS-LIVANIOU - Eclipses and Ancient Greek Philosophers - LUNCH BREAK - ECLIPSE OBSERVATIONS - ROSTE-SREAC
(Sub-Regional European Astronomical Committee) SESSION Forth Meeting of the Sub-Regional European
Astronomical Committee (Chairman: Zeki ASLAN) (All participants are
free to attend as listeners) 16:00 - 16:30 Michel DENNEFELD - Coordination of
medium-sized telescopes, development activities for Extremely Large Telescopes
Abstracts of the Invited Talks (in alphabetical order according
to the speaker’s surname) Solar and Stellar
Eclipse Mapping Edwin BUDDING The special circumstance of solar eclipse affords an opportunity to
review its background, particularly in the cultural context of western Turning to the more general subject of
stellar eclipses, topics of particular note concern: choice of fitting
functions, disk eclipses, spot eclipses and the “gravity-darkening” effect. These topics arise within new era eclipsing binary studies and are
relevant to active researches on remote binaries and extrasolar planets. Modelling of the
Internal Structure of the Asteroids Vladan A.
ČELEBONOVIĆ Existing knowledge about the internal structure of
the asteroids is not very developed mainly due to lack of reliable couples of
experimental data (the masses and radii). This lecture will try to fulfill a
double aim: to review what is known about the interiors of the asteroids,and to explore the possibility of advancing the field by
introducing and using in it some well known notions from solid state physics. Helioseismology and
Plasma Physics Werner DÄPPEN Department of Physics and Astronomy, Helioseismology has become a very successful diagnostic tool of the solar
interior. Among the earliest targets of helioseismology was the equation of
state of the solar plasma. Although the plasma in the solar interior is only
weakly coupled and weakly degenerate, the great observational accuracy of the
helioseismological measurements has put strong constraints on the nonideal part
of the equation of state. For solar and stellar modeling, a high-quality
equation of state is crucial. But the inverse is also true: the astrophysical
data (helioseismic today, asteroseismic tomorrow) allow us to improve the
physical theories, thus making the Sun alaboratory for plasma physics.
Dynamical Evolution of Active
Detached Binaries and Formation of Zeki EKER First order decreasing rates of orbital angular momentum (OAM), systemic
mass (M=M1+M2) and orbital period of detached
chromospherically active binaries have been determined as J(dot)=3.48
10-10 yr-1 per systemic OAM, M(dot)= 1.30 10-10yr-1
per systemic mass and P(dot)= 3.96 10-10
yr-1 per orbital period from the subgroup kinematical ages of 62
field systems. The ratio of d log J/ d log M = 2.68 implies a mechanism which
amplifies the angular momentum loss A = 2.68 times with respect to an isotropic
angular momentum loss of a hypothetical isotropic wind. Various decreasing
rates of OAM (d log J / dt) and mass
loss (d log M/ dt) due to magnetically
driven stellar winds determine various speeds of dynamical evolutions that a
detached system could becomes a contact binary if dynamical evolution makes
system to pass the contact border on the log J – log M diagram. According to
average dynamical evolution with A = 2.68, the fraction of 10, 22 and 39
percent of current detached sample is expected to be contact system within 2, 4
and 6 Gyr respectively. Planetary Transits Alvaro GIMÉNEZ Research and Scientific Support Department, ESA, The Eclipses of the Sun by the Moon provide an
excellent example of the power of eclipsing events in the Universe. The transit
of the planets Mercury and Venus as well as the occultation of the Galilean
satellites by Jupiter have provided important science to astronomers in the
past. Furthermore the mutual eclipses shown by some binary stars have allowed
for independent and direct measurements of stellar radii and masses otherwise
only modeled. More recently, the discovery of extrasolar planetary transits has
open the possibility to understand the size and mean
densities of these objects, until now more or less similar to Jupiter, orbiting
around other stars. The extension of techniques developed for the analysis of
eclipsing binaries to extrasolar planetary transits is presented that leads to
accurate masses and radii of both the planet and the host star. Eclipse Power: The Brave
New World of Eclipsing Binaries – From Cosmology to
Exoplanets Edward GUINAN Villanova University, USA Recent new
developments in the study of eclipsing binary systems will be presented.
Eclipsing binaries systems are critically important for the determination of
the fundamental properties of stars - providing masses, radii and
luminosities. They also provide critical
tests of stellar physics, stellar evolution and stellar structure
theories. But more recently, eclipsing
binaries are now providing vital information on a wide variety of phenomena
ranging from cosmology to exoplanets. A dicussion of new
things that can be learned from the study of the thousands of eclipsing binary
systems that have been discovered in nearby Local Group galaxies, mainly as
offshoots of microlensing programs. Selected extragalactic binaries are serving
as accurate distance indicators.
Accurate distances are now known for the Magellanic Clouds from the
study of eclipsing binaries. Also
eclipsing binaries are being used to measure the distances to M31 and M33.
These studies are leading to a more accurate determination of the extragalactic
distance scale as well as a better determination of the zero point of the
Hubble Constant Ho. Also discussed
will be a new class of eclipsing star-planet systems. At present only about
eight eclipsing planet/star systems have been found but hundreds are expected
to be discovered within the next several years.
A discussion of important new information that can be gained about
exoplanets and their environments will be given. Solar Variations and
Climate on Planets Arnold
HANSLMEIER Karl-Franzens-Universität Graz, Institut für
Geophysik Astrophysik und Meteorologie, Austria It is well known that the Sun is variable on different time scales: days,
solar activity cycle(s), long term variation during
its evolution. In this review we focus on the problem of how these variations
could possibly influence planetary atmosphere and even their climate. The
luminosity of the Early Sun was about 70% that of the present value but on the
other hand the early Sun was a very active star. This can be studied by
comparing the Sun with solar like young stars. Today variations of solar
luminosity during an activity cycle are only a few 0.1 %
however it can be shown that even such low amplitude variations are comparable
to other effects like greenhouse gases. Selected examples of solar luminosity
variations (total solar irradiance as well as variations in the UV) are
compared and extrapolated to the situation of the early Sun and discuss
possible effects on planetary atmospheres.
Abstracts of the Contributed Talks (in alphabetical order according
to the speaker’s surname) Simon ALBRECHT, Leiden Observatory, albrecht@strw.leidenuniv.nl TITLE:
The Rossiter McLaughlin Effect in the Eclipsing Binary System V1143Cyg - First
Results AUTHOR(S):
S. Albrecht, S. Reffert, A. Quirrenbach, D. Mitchell ABSTRACT: Eclipsing
binaries are a great stellar laboratory for gathering information on stellar
surface structure. The crossing of the companion in front of the rotating star
causes a change in the line profile of the eclipsed star. The strength and
shape of this rotation effect, also called Rossiter McLaughlin effect, is a
function of the inclination and the projection of the stellar axes on the sky. We
observed the primary and secondary eclipse in the binary system V1143 Cyg with
the Olga
ATANACKOVIC-VUKMANOVIC, Faculty of Mathematics,
University of Belgrade, olga@matf.bg.ac.yu TITLE:
Solution of NLTE Radiative Transfer Problems Using Forth-and-Back Implicit
Lambda Iteration AUTHOR(S):
O. Atanackovic-Vukmanovic ABSTRACT: A fast
convergent iterative method for the exact solution of NLTE radiative transfer
problems is described. Forth-and-back implicit Lambda iteration dramatically
accelerates the convergence of the classical Lambda iteration (while retaining
its straightforwardness) by use of forth-and-back approach together with an
implicit representation of the source function in the computation of the
radiation field intensities. No matrix operation is required and the memory
storage grows only linearly with the dimension of the problem. The convergence
properties of the method are excellent and the exact solution is usually
obtained after only a few iterations even under conditions that are very far
from LTE. The method is very simple and easy to apply. In this paper the method
is applied to the solution of several RT problems. Numerical results are given
in each case and compared with those obtained by other authors using different
methods. Hicran
BAKIŞ, Çanakkale University, Department of
Physics, bhicran@physics.comu.edu.tr TITLE:
On The Light Curve Variation of The Be Star EM Cep AUTHOR(S): H. Bakış, O. Demircan, V. Bakış, E. Budding ABSTRACT: We are presenting
all historical light curves and also presenting new five seasons of UBV
photometric observations and one season spectroscopic observation of the Be
star EM Cephei. This star is shown 0.8061787 d period, is present in the
photometry, although there are large light amplitude variations from seasons to
seasons. On the 17-18 July 2003 a flare of this star has been deteched. U
brightness has maximum increases. New high-resolution spectroscopic
observations show the star to be a single. The variation of
the light curve show that Star seems to be a member of Lambda Eri type
variables. Additional changes on the light curve doesn't
show any periodicity. Binarity problem of the star has been discussed. The
strong wind effects must be the reason for the asymmetry in the light curve. Volkan
BAKIŞ, Çanakkale University, Department of
Physics, bakisv@physics.comu.edu.tr TITLE:
Photometric and Spectroscopic Study of the Eccentric Binary GSC 4288 0186 AUTHOR(S): V. Bakış, E. Budding, O. Demircan, H. Bakış ABSTRACT: First
BVRI light curves of the recently discovered eccentric binary GSC 4288 0186
together with radial velocity measurements are presented. Light curves together
with radial velocity data of the system were analyzed by the latest vesions of
ILOT and Wilson-Devinney(WD) light curve analysis
programs. Spectroscopic observations show the system to be a double-lined
binary. For the primary and secondary star respectively, we find the following
dimensions: M= 2.39(0.01) and 1.91(0.02) solar masses; R= 1.86(0.02) and
1.63(0.03) solar radii. We are giving an estimation on
distance of the eclipsing system. Véronique BOMMIER, LERMA, Observatoire de Paris, V.Bommier@obspm.fr TITLE:
Is the Solar Intranetwork Field a Resolved Turbulent Field? AUTHOR(S):
V. Bommier, E. Landi Degl’Innocenti, M. Landolfi, G. Molodij ABSTRACT: The
spectropolarimetric map observed below an active region filament on Werner CURDT, Max-Planck-Institute
for Solar System Research, curdt@mps.mpg.de TITLE:
The Transition Region Above Sunspots AUTHOR(S):
W. Curdt, E. Landi ABSTRACT: We
present results from spectroscopic observations of sunspots obtained in the
vacuum ultraviolet wavelength range by Hüseyin
ÇAVUŞ, Çanakkale University, Department of
Physics, h_cavus@comu.edu.tr TITLE:
Some MHD Solutions For The Bottom Of The Solar
Convective Layer AUTHOR(S): H. Çavuş, A. I. Karafistan ABSTRACT: The magnetic field
responsible for the solar activity is stored in the base of the convective
zone. Applying this knowledge to the bottom of the convection zone in the Sun
our objective was to investigate some magnetohydrodynamical (MHD) solutions.
The first order perturbation approximation was used in order to calculate the
small perturbations on the physical parameters of a Standard Solar Model (SSM)
excluding both rotation and magnetic field (Christensen-Dalsgaard et al., 1996)
in the unperturbed equilibrium case. The validity of each approximation is
tested and examined from the SSM. The MHD results thus obtained are presented
graphically and compared with those of the SSM. Osman
DEMİRCAN, Çanakkale University, Department of
Physics, demircan@comu.edu.tr TITLE:
Solar and Stellar Rotation AUTHOR(S):
O. Demircan ABSTRACT: The secular
evolution of the stellar rotation through angular momentum loss, driven by the
stellar wind, and the concequences of the angular momentum exchange between
rotation and orbit in binary star systems will be reviewed with the special
emphasis on the Solar case. A large co-rotating
distance (Alfven radius) of the magnetically driven wind around single stars
will be introduced in explaining the large angular momentum loss from the close
binary star systems. Michel DENNEFELD, Institut d'Astrophysique (IAP-Paris), dennefel@iap.fr TITLE:
Coordination of Medium-Sized Telescopes, Development Activities for Extremely
Large Telescopes AUTHOR(S): M. Dennefeld ABSTRACT: I will present a
short overview of the observing facilities (in the visible and infrared) accessible
to european astronomers, and some mechanisms to
promote collaborations across the borders. Cristiana
DUMITRACHE, Astronomical Institute of Romanian
Academy, crisd@aira.astro.ro TITLE:
Coronal Streamer Formation Post CME - Numerical Simulation AUTHOR(S): C. Dumitrache ABSTRACT: We
present a numerical experiment where a coronal streamer forms after coronal
mass ejections "en-raffale" produced Jochen EISLÖFFEL, Thüringer Landessternwarte, jochen@tls-tautenburg.de TITLE:
Results from the Exoplanet Search Programmes with BEST and TEST AUTHOR(S):
J. Eislöffel, A. Hatzes, H. Rauer, H. Voss, A. Erikson, P. Eigmüller. ABSTRACT: Thüringer
Landessternwarte Tautenburg and Deutsches Zentrum für Luft und In order to
determine their orbits, masses, and thus their nature, exoplanet transit
candidates are being followed up with radial velocity measurements with the
Echelle spectrograph of the Tautenburg 2-m reflector, which is equipped with an
iodine cell. I will report on results of these search programmes on exoplanet
candidates and eclipsing binaries. Romain GAUDERON, Laboratoire d'Astrophysique (EPFL), Switzerland, romain.gauderon@epfl.ch TITLE:
Eclipsing Binaries in the SMC: Combining VLT Multi-Object Spectroscopy with
OGLE Photometry AUTHOR(S): R. Gauderon1, F.
Royer2, P. North1 (1)
Laboratoire d'Astrophysique, Ecole Polytechnique Federale de Lausanne, CH-1290
Sauverny, SWITZERLAND (2) GEPI, CNRS UMR 8111,
Observatoire de Paris, F-92195 MEUDON Cedex, FRANCE ABSTRACT: We
present a detailed analysis of 33 eclipsing binary (EB) systems in the Small
Magellanic Cloud (SMC), which allowed us to give an essentially complete
description of the stellar properties of each system (including masses, radii,
luminosities, surface gravities and effective temperatures). These systems are
then used as primary distance indicators to provide a new estimate of the
distance to the SMC. The analysis is based on both spectroscopic and
photometric data, i.e. on radial velocity curves obtained through multi-object
spectroscopic observations made with the ESO FLAMES facility at the VLT
(Paranal Observatory, |
