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x about a sequence of reVlew lectures, each followed by contributed
talks and discussions. The opening session was devoted to reviewing
the most recent results concerning the determination of chemical
abundances in particularly inte resting objects providing direct
evidence for stellar nucleosynthesis (like planetary nebulae,
supernovae and supernova remnants). In Session 2 recent results on
some relevant nuclear reaction rates have been presented. Session 3
grouped the contributions concerning the quasi-static evolution of
normal stars, its relevance for the nucleosynthesis of the varlOUS
elements and isotopes, and the comparison of the evolutionary
models with the observations. Session 4 addressed the important
questions of identifying the precursors of both Type I and Type II
supernovae, and of determining the detailed composition of the
ejecta by explosive nucleosynthesis associated with these events.
Finally, Session 5 was devoted to a presentation of recent
calculations of the evolution of hypothetical pre-galactic very
massive objects (in cluding their potential role in pre-galactic
nucleosynthesis), and to reviewing the progress that has been made
in understanding the chemical evolution of galaxies. The discussion
during and after talks was spirited and contributed signi ficantly
to the succes of the workshop. We regrett for not having been able
of reporting it "in toto" in the proceedings. Nevertheless, we hope
that what has been recorded may still give to the reader at least
part of the excitement we have experienced during the ten days of
the workshop."
As it was said by one of the participants to this workshop" In our
attempts to understand the spectral evolution of galaxies, we are
fortunate indeed to have the ability to look back in time and
observe galaxies as they were billions of years ago. Perhaos in no
other discipline is it possible to gain such a direct view to
hJstory. The galaxies we seek to study are remote, their light
faint, and thus only recently has it become technicaJlv feasible to
sample the spectra of normal luminosity galaxies at lookback times
of five billion years or more" .... or, perhaps. even to see
galaxies in the process of their formation. or shortly afterwards.
This fourth workshop organized by the "Advanced School ot Astronomy
was indeed centered on the "Spectral Evolution of Galaxies." on
reviewing and discussing the relevant astrophysical processes and
on assessing our current ability to model and understand the
evolution of stellar populations. Following an opening session
dealing with some outstanding questions of galaxy evolution.
Session I addressed the specific problems of galaxy and star
formation processes. topics of uncertainty and controversy to which
IRAS observations may give novel perspectives. The properties of
stellar populations in the local group of galaxies formed the basis
of Session II. Session III dealt with the fundaments of the theory
of spectral and photometrical evolution of stellar populations. and
with recent developments in the theory of stellar structure. a
necessary step to model and understand galactic evolution.
The IAU Colloquium No. 59, "The effects of mass loss on Stellar
Evolution" was held on September 15-19, 1980 at the International
Centre for Theoretical Physics, Miramare, Trieste (Italy), under
the auspices of the IAU Executive Co~ mittee and the Italian
National Council of Research. The planning of this conference began
two years ago du ring the IAU Symposium No. 83 "Mass loss and
evolution of 0 type stars" (Qualicum Beach, Victoria, Canada) when
we felt that mass loss and its effects on the evolution of stars
was too broad a subject for being confined to 0 type stars only.
Therefore we thought that a conference dealing with the general
problem of mass loss across the whole HR diagram would have been of
interest to all people working in the field. The main idea was that
bringing together Astronomers and Astrophysicists of the widest
range of interests and e~ pertize - all in some way related to the
problem of mass loss from stars - would have spurred thorough
discussions on the many aspects and implications of this topic. We
hope this goal has been achieved. Furthermore, the most recent
observational and theoreti cal developments on the problem of mass
loss from early ty pe stars avoided this meeting to be a simple
updating of the Qualicum Beach Symposium as far as this issue is
concerned.
Recent years have witnessed the expansion and multiplication of the
observations of star formation and fragmentation accompanied by a
consequent growth in the study of the underlying physical
processes, the chemistry, the sites, the times, etc. Moreover,
recent studies have shown that the formation of stars is likely to
share many features with the formation of other self-gravitating
objects. The present volume, therefore, discusses the formation of
such objects in a systematic and comparative manner.
As it was said by one of the participants to this workshop" In our
attempts to understand the spectral evolution of galaxies, we are
fortunate indeed to have the ability to look back in time and
observe galaxies as they were billions of years ago. Perhaos in no
other discipline is it possible to gain such a direct view to
hJstory. The galaxies we seek to study are remote, their light
faint, and thus only recently has it become technicaJlv feasible to
sample the spectra of normal luminosity galaxies at lookback times
of five billion years or more" .... or, perhaps. even to see
galaxies in the process of their formation. or shortly afterwards.
This fourth workshop organized by the "Advanced School ot Astronomy
was indeed centered on the "Spectral Evolution of Galaxies." on
reviewing and discussing the relevant astrophysical processes and
on assessing our current ability to model and understand the
evolution of stellar populations. Following an opening session
dealing with some outstanding questions of galaxy evolution.
Session I addressed the specific problems of galaxy and star
formation processes. topics of uncertainty and controversy to which
IRAS observations may give novel perspectives. The properties of
stellar populations in the local group of galaxies formed the basis
of Session II. Session III dealt with the fundaments of the theory
of spectral and photometrical evolution of stellar populations. and
with recent developments in the theory of stellar structure. a
necessary step to model and understand galactic evolution.
The IAU Colloquium No. 59, "The effects of mass loss on Stellar
Evolution" was held on September 15-19, 1980 at the International
Centre for Theoretical Physics, Miramare, Trieste (Italy), under
the auspices of the IAU Executive Co~ mittee and the Italian
National Council of Research. The planning of this conference began
two years ago du ring the IAU Symposium No. 83 "Mass loss and
evolution of 0 type stars" (Qualicum Beach, Victoria, Canada) when
we felt that mass loss and its effects on the evolution of stars
was too broad a subject for being confined to 0 type stars only.
Therefore we thought that a conference dealing with the general
problem of mass loss across the whole HR diagram would have been of
interest to all people working in the field. The main idea was that
bringing together Astronomers and Astrophysicists of the widest
range of interests and e~ pertize - all in some way related to the
problem of mass loss from stars - would have spurred thorough
discussions on the many aspects and implications of this topic. We
hope this goal has been achieved. Furthermore, the most recent
observational and theoreti cal developments on the problem of mass
loss from early ty pe stars avoided this meeting to be a simple
updating of the Qualicum Beach Symposium as far as this issue is
concerned.
Recent years have witnessed the expansion and multiplication of the
observations of star formation and fragmentation accompanied by a
consequent growth in the study of the underlying physical
processes, the chemistry, the sites, the times, etc. Moreover,
recent studies have shown that the formation of stars is likely to
share many features with the formation of other self-gravitating
objects. The present volume, therefore, discusses the formation of
such objects in a systematic and comparative manner.
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