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The theory of stellar atmospheres is one of the most important
branches of modern astrophysics. It is first of all a major tool
for understanding all aspects of stars. As the physical properties
of their outer layers can now be found with high precision, firm
conclusions can be drawn about the internal structure and evolution
of stars. Moreover, improvements in our knowledge of the chemical
composition of stars is shedding new light on the chemical
evolution of galaxies and of the Universe as a whole. Because the
outer layers of stars are among the best-understood astrophysical
objects, the theory of stellar atmospheres plays an important role
in the study of many other types of objects. These include
planetary nebulae, H II regions, interstellar matter, and objects
of interest in high-energy astrophysics, such as accretion disks
(close binaries, dwarf novae, cataclysmic variables, quasars,
active galactic nuclei), pulsar magnetospheres, and Seyfert
galaxies. Finally, as stars provide a laboratory in which plasmas
can be studied under more extreme conditions than on earth, the
study of stellar atmospheres has strong connections with modern
physics. Astronomical observations provided a vital stimulus in the
early stages of quantum theory and atomic physics; even today
topics such as low-temperature dielectronic recombination develop
hand in hand with the interpretation of stellar and nebular
spectra. Early work on MHD was similiarly motivated. Many such
connections remain to be explored.
The publication in English of this monograph seems to me to
indicate the ever increasing interest of astrophysicists in the
physical and dynamical problems of planetary nebulae-one of the
most interesting and fruitful branches of theoretical astrophysics.
Their interest in part arises from the fact that the methods of
identify ing the physical processes occurring in planetary nebulae,
as well as the many theo retical results, are now acquiring a
degree of uni versality as their sphere of application increases.
Finally, the special cosmic significance of planetary nebulae is
becoming apparent. The English edition of Planetary Nebulae differs
considerably from the Russian version published in 1962, primarily
because of the new results included in it, but also because of
numerous editorial revisions. The problems of magnetic fields and
hydrodynamics in planetary nebulae are beginning to occupy an
important place in the study of the dynamics of these objects.
Recent studies by D. H. Menzel confirm the idea advanced in the
present mono graph as to the existence of magnetic fields in
planetary nebulae. New light is being cast on the dynamics of
planetary nebulae by the hydrodynamic investigations of F. D. Kahn,
W. G. Mathews and others. Unfortunately I was not able to include
these and other interesting results in the present edition."
The theory of stellar atmospheres is one of the most important
branches of modern astrophysics. It is first of all a major tool
for understanding all aspects of stars. As the physical properties
of their outer layers can now be found with high precision, firm
conclusions can be drawn about the internal structure and evolution
of stars. Moreover, improvements in our knowledge of the chemical
composition of stars is shedding new light on the chemical
evolution of galaxies and of the Universe as a whole. Because the
outer layers of stars are among the best-understood astrophysical
objects, the theory of stellar atmospheres plays an important role
in the study of many other types of objects. These include
planetary nebulae, H II regions, interstellar matter, and objects
of interest in high-energy astrophysics, such as accretion disks
(close binaries, dwarf novae, cataclysmic variables, quasars,
active galactic nuclei), pulsar magnetospheres, and Seyfert
galaxies. Finally, as stars provide a laboratory in which plasmas
can be studied under more extreme conditions than on earth, the
study of stellar atmospheres has strong connections with modern
physics. Astronomical observations provided a vital stimulus in the
early stages of quantum theory and atomic physics; even today
topics such as low-temperature dielectronic recombination develop
hand in hand with the interpretation of stellar and nebular
spectra. Early work on MHD was similiarly motivated. Many such
connections remain to be explored.
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