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These are the proceedings of a meeting celebrating Michael
Thompson's seminal work on solar and stellar physics, as well as
his major contributions to the development of the National Center
for Atmospheric Research. The meeting also marked Michael J.
Thompson's untimely death in October 2018. Michael played a key
role in the development of helioseismology and its application to
the study of the structure and dynamics of the solar interior, and
he provided a strong foundation for the extension of seismic
studies for other stars. After focusing for several years on more
administrative activities, he was returning to leading the seismic
studies of solar interior rotation and he was deeply involved in
the understanding of the dynamics of the core of stars, when his
life was tragically lost. The conference focused on dynamical
aspects of the sun and stars, based on the large amount of data
available on solar and stellar oscillations, and the extensive and
detailed modelling now becoming feasible. Combining observations,
seismic analysis, and modelling the meeting and this book serve as
a fitting memorial to a close colleague and friend, much missed.
These are the proceedings of a meeting celebrating Michael
Thompson's seminal work on solar and stellar physics, as well as
his major contributions to the development of the National Center
for Atmospheric Research. The meeting also marked Michael J.
Thompson's untimely death in October 2018. Michael played a key
role in the development of helioseismology and its application to
the study of the structure and dynamics of the solar interior, and
he provided a strong foundation for the extension of seismic
studies for other stars. After focusing for several years on more
administrative activities, he was returning to leading the seismic
studies of solar interior rotation and he was deeply involved in
the understanding of the dynamics of the core of stars, when his
life was tragically lost. The conference focused on dynamical
aspects of the sun and stars, based on the large amount of data
available on solar and stellar oscillations, and the extensive and
detailed modelling now becoming feasible. Combining observations,
seismic analysis, and modelling the meeting and this book serve as
a fitting memorial to a close colleague and friend, much missed.
This volume contains the reviews and poster papers presented at the
workshop Solar Convection and Oscillations and their Relationship:
SCORe '96, held in Arhus, Denmark, May 27 - 31, 1996. The aim of
this workshop was to bring together experts in the fields of
convection and helioseismology, and to stimulate collaborations and
joint research. The participation to this workshop was purposely
kept limited in order to provide optimal conditions for informal
discussions. In autumn of 199,5 the long-awaited GONG network of
solar telescopes became fully operational and the first data
already show significant improvement over existing datasets on
solar oscillations. Furthermore, in December of 1995 the satellite
SOHO was launched which, together with GONG, provides a major step
forward in both the quantity and the quality of available solar
oscillation data. It is with this in mind that we decided to
organize the workshop to prepare for the optimal use of this wealth
of data, with which to deepen our understanding of solar structure
and specifically, of one of the longest-standing problems in solar
and stellar modelling: the treatment of convection.
The cover picture of this volume displays one of the most advanced
products of he lioseismic research: a view into the deep interior
of the sun, revealing its distinctly non-uniform rotation
throughout the entire depth of the convection zone. Just over 20
years ago, the first successful helioseismic experiment disclosed
an increase of ro tation velocity in the uppermost one dozen
megameters below the photosphere. The stunning progress in depth
and detail highlighted by the cover diagram (and by others shown in
this volume as well) was made possible by considerable advances in
instru mentation, by the development of powerful analytical tools
and, foremost, by the involvement of new brains of enthusiastic
proselytes and newcomers to the field, in creasing nearly
exponentially in number every year. New branches of research
widened the scope of "uranoseismology", as e. g. time-distance
seismology (the promising av enue towards small-scale and
short-time variability), atmospheric seismology (a new look at
strange phenomena we have all ways seen, but hardly understood),
and finally the growing observational assault on hundreds of
individual stars which are either manifestly or supposedly
oscillating -i. e. asteroseismology. The formation of numer ous
solar and stellar observing networks and, ultimately, space
missions like SOHO have greatly promoted the potential of this
science. This steady progress was accompanied by workshops,
colloquia, and symposia in quick succession.
The continuing success of helio- and asteroseismology in studying
the internal structure and dynamics of the Sun, and of other single
stars, has been highlighted in recent years by many topical
meetings. The present Proceedings document the first Seismology
symposium ever held in conjunction with an IAU General Assembly.
This substantially influenced the layout of the scientific
programme and demonstrates the vitality of this field of astronomy.
The invited reviews are intended to address an audience that
includes many non-specialists. Therefore, this volume is
particularly valuable as an introduction to the general concepts of
the field, and for conveying the excitement that comes with
discussions of the most recent observational and theoretical
results. There are two chapters on the many facets of
asteroseismology, which also compare solar and stellar
achievements. A major focus of the symposium was the new
developments resulting from the observations of unprecedented
quality obtained from global multi-site networks, and especially
from the Solar and Heliospheric Observatory SoHO, currently
continuing its observations from the Lagrangian point L1. From the
center of the Sun to its outer layers, the reader will learn how
modern diagnostic techniques reveal the inextricable links between
the complex structure of the interior and atmosphere of our nearest
star. The book is recommended for undergraduates, postgraduates,
and professionals with a strong interest in modern developments in
astrophysics.
This volume contains the reviews and poster papers presented at the
workshop Solar Convection and Oscillations and their Relationship:
SCORe '96, held in Arhus, Denmark, May 27 - 31, 1996. The aim of
this workshop was to bring together experts in the fields of
convection and helioseismology, and to stimulate collaborations and
joint research. The participation to this workshop was purposely
kept limited in order to provide optimal conditions for informal
discussions. In autumn of 199,5 the long-awaited GONG network of
solar telescopes became fully operational and the first data
already show significant improvement over existing datasets on
solar oscillations. Furthermore, in December of 1995 the satellite
SOHO was launched which, together with GONG, provides a major step
forward in both the quantity and the quality of available solar
oscillation data. It is with this in mind that we decided to
organize the workshop to prepare for the optimal use of this wealth
of data, with which to deepen our understanding of solar structure
and specifically, of one of the longest-standing problems in solar
and stellar modelling: the treatment of convection.
Helio- and asteroseismology study the interior of the Sun and other
stars, by means of observations of oscillations on their surfaces.
The last 10 years in the study of the solar interior, to a has
witnessed a very rapid evolution point where we can now contemplate
investigating the physical state of matter, or the details of
rotation and other large-scale motion, in the Sun. The stellar
studies are in some respects at the point of the solar studies 10
years ago, but appear poised to take off. Thus the time was deemed
ripe for lAO Symposium No 123, to assess the present status of this
work, and plan for its future development. Apart from the seismic
data, few observations are available to provide information about
stellar interiors. Detailed studies, by spectral analysis, can be
made of stellar surface properties, including atmospheric
temperature and chemical composition. However, the stellar
radiative spectrum is almost entirely fixed by the mass,
luminosity, radius and surface rotation of the star, and contains
essentially no other information about the interior. An important
test of stellar evolution theory is provided by observations of
stel lar clusters, whose members can reasonably be assumed to have
the same age and chemical composition. The location of such stars
in a HR diagram, where luminosity is plotted against the effective
temperature, can roughly be understood in terms of stellar
evolution calculations."
In all phases of the life of a star, hydrodynamical processes play
a major role. This volume gives a comprehensive overview of the
state of knowledge in stellar astrophysical fluid dynamics, and its
publication marked the 60th birthday of Douglas Gough, Professor of
Theoretical Physics at the University of Cambridge and leading
contributor to stellar astrophysical fluid dynamics. Topics include
properties of pulsating stars, helioseismology, convection and
mixing in stellar interiors, dynamics of stellar rotation, planet
formation and the generation of stellar and planetary magnetic
fields. Each chapter is written by leading experts in the field,
and the book provides an overview that is central to any attempt to
understand the properties of stars and their evolution. With
extensive references to the technical literature, this is a
valuable text for researchers and graduate students in stellar
astrophysics.
This comprehensive overview of stellar astrophysical fluid dynamics includes properties of pulsating stars; helioseismology; convection and mixing in stellar interiors; and dynamics of stellar rotation, planet formation and the generation of stellar and planetary magnetic fields. Each chapter is written by a leading expert in the field and extensive references to technical literature are made.
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