UID:
almafu_9959238886102883
Format:
1 online resource (xvi, 890 pages) :
,
digital, PDF file(s).
ISBN:
1-316-08959-2
,
1-139-77955-9
,
1-139-77651-7
,
1-139-06122-4
,
1-139-78351-3
,
1-139-78254-1
Content:
This text describes the microscopic physics operating in stars and demonstrates how stars respond from formation, through hydrogen-burning phases, up to the onset of helium burning. Intended for beginning graduate students and senior undergraduates with a solid background in physics, it illustrates the intricate interplay between the microscopic physical processes and the stars' macroscopic responses. The volume starts with the gravitationally contracting phase which carries the star from formation to the core hydrogen-burning main sequence, through the main sequence phase, through shell hydrogen-burning phases as a red giant, up to the onset of core helium burning. Particular emphasis is placed on describing the gravothermal responses of stars to nuclear transformations in the interior and energy loss from the surface, responses which express the very essence of stellar evolution. The volume is replete with many illustrations and detailed numerical solutions to prepare the reader to program and calculate evolutionary models.
Note:
Title from publisher's bibliographic system (viewed on 05 Oct 2015).
,
pt. I. Introduction and overview -- pt. II. Basic physical processes in stellar interiors -- pt. III. Pre-main sequence, main sequence, and shell hydrogen-burning evolution of single stars.
,
English
Additional Edition:
ISBN 1-107-01656-8
Language:
English
URL:
https://doi.org/10.1017/CBO9781139061223
Bookmarklink
