Read more
This book deals with stars during a short episode before they undergo a ma jor, and fatal, transition. Soon the star will stop releasing nudear energy, it will become a planetary nebula for abrief but poetic moment, and then it will turn into a white dwarf and slowly fade out of sight. Just before this dramatic change begins the star has reached the highest luminosity and the largest diameter in its existence, and while it is a star detectable in galaxies beyond the Local Group, its structure contains already the inconspicuous white dwarf it will become. It is called an "asymptotic giant branch star" or "AGB star". Over the last 30 odd years AGB stars have become a topic of their own although individual members of this dass had already been studied for cen turies without realizing what they were. In the early evolution, so called "E-AGB"-phase, the stars are a bit bluer than, but otherwise very similar to, what are now called red giant branch stars (RGB stars). It is only in the sec ond half of their anyhow brief existence that AGB stars differ fundamentally from RGB stars.
List of contents
1 AGB Stars: History, Structure, and Characteristics.- 2 Evolution, Nucleosynthesis, and Pulsation of AGB Stars.- 3 Synthetic AGB Evolution.- 4 Atmospheres of AGB Stars.- 5 Molecule and Dust Grain Formation.- 6 Dynamics and Instabilities in Dusty Winds.- 7 Circumstellar Envelopes.- 8 AGB Stars as Tracers of Stellar Populations.- 9 AGB Stars in Binaries and Their Progeny.- 10 Post-AGB Stars.
Summary
This book deals with stars during a short episode before they undergo a ma jor, and fatal, transition. Soon the star will stop releasing nudear energy, it will become a planetary nebula for abrief but poetic moment, and then it will turn into a white dwarf and slowly fade out of sight. Just before this dramatic change begins the star has reached the highest luminosity and the largest diameter in its existence, and while it is a star detectable in galaxies beyond the Local Group, its structure contains already the inconspicuous white dwarf it will become. It is called an "asymptotic giant branch star" or "AGB star". Over the last 30 odd years AGB stars have become a topic of their own although individual members of this dass had already been studied for cen turies without realizing what they were. In the early evolution, so called "E-AGB"-phase, the stars are a bit bluer than, but otherwise very similar to, what are now called red giant branch stars (RGB stars). It is only in the sec ond half of their anyhow brief existence that AGB stars differ fundamentally from RGB stars.
Additional text
From the reviews:
"AGB stars have red giants as progenitors, and are fated to become planetary nebulae and white dwarfs. This book comprises a set of papers dealing with all aspects of the physics of these stars. It is intended for a graduate study level … . the chapters which are designed to be self-standing do provide interesting discussions about theory and corroborative observations, and I think there is lot that can be gleaned … ." (Callum Potter, Journal of the British Astronomical Association, Vol. 114 (3), 2004)
Report
From the reviews:
"AGB stars have red giants as progenitors, and are fated to become planetary nebulae and white dwarfs. This book comprises a set of papers dealing with all aspects of the physics of these stars. It is intended for a graduate study level ... . the chapters which are designed to be self-standing do provide interesting discussions about theory and corroborative observations, and I think there is lot that can be gleaned ... ." (Callum Potter, Journal of the British Astronomical Association, Vol. 114 (3), 2004)
