000			02084nam a22003258i 4500
001			CR9781139061230
003			UkCbUP
005			20200124160333.0
006			m|||||o||d||||||||
007			cr||||||||||||
008			110414s2013||||enk o ||1 0|eng|d
020			_a9781139061230 (ebook)
020			_z9781107016576 (hardback)
040			_aUkCbUP _beng _erda _cUkCbUP
050	0	0	_aQB806 _b.I24 2013
082	0	0	_a523.8/8 _223
100	1		_aIben, Icko, _d1931- _eauthor.
245	1	0	_aStellar evolution physics. _nVolume 2, _pAdvanced evolution of single stars / _cIcko Iben.
264		1	_aCambridge : _bCambridge University Press, _c2013.
300			_a1 online resource (x, pages 893-1495) : _bdigital, PDF file(s).
336			_atext _btxt _2rdacontent
337			_acomputer _bc _2rdamedia
338			_aonline resource _bcr _2rdacarrier
500			_aTitle from publisher's bibliographic system (viewed on 05 Oct 2015).
520			_aThis volume explains the microscopic physics operating in stars in advanced stages of their evolution and describes with many numerical examples and illustrations how they respond to this microphysics. Models of low and intermediate mass are evolved through the core helium-burning phase, the asymptotic giant branch phase (alternating shell hydrogen and helium burning) and through the final cooling white dwarf phase. A massive model is carried from the core helium-burning phase through core and shell carbon-burning phases. Gravothermal responses to nuclear reaction-induced transformations and energy loss from the surface are described in detail. Written for senior graduate students and researchers who have mastered the principles of stellar evolution, as developed in the first volume of Stellar Evolution Physics, sufficient attention is paid to how numerical solutions are obtained to enable the reader to engage in model construction on a professional level.
650		0	_aStars _xEvolution.
650		0	_aStellar dynamics.
776	0	8	_iPrint version: _z9781107016576
856	4	0	_uhttps://doi.org/10.1017/CBO9781139061230
999			_c522764 _d522762