000 04313nam a22005655i 4500
001 978-981-96-0551-4
003 DE-He213
005 20251030114939.0
007 cr nn 008mamaa
008 250206s2024 si | s |||| 0|eng d
020 _a9789819605514
_9978-981-96-0551-4
024 7 _a10.1007/978-981-96-0551-4
_2doi
050 4 _aQB460-466
072 7 _aPHVB
_2bicssc
072 7 _aSCI005000
_2bisacsh
072 7 _aPHVB
_2thema
100 1 _aNagele, Chris.
_eauthor.
_4aut
_4http://id.loc.gov/vocabulary/relators/aut
_990689
245 1 0 _aGeneral Relativistic Instability Supernovae
_h[electronic resource] /
_cby Chris Nagele.
250 _a1st ed. 2024.
264 1 _aSingapore :
_bSpringer Nature Singapore :
_bImprint: Springer,
_c2024.
300 _aXII, 73 p. 28 illus., 26 illus. in color.
_bonline resource.
336 _atext
_btxt
_2rdacontent
337 _acomputer
_bc
_2rdamedia
338 _aonline resource
_bcr
_2rdacarrier
347 _atext file
_bPDF
_2rda
490 1 _aSpringer Theses, Recognizing Outstanding Ph.D. Research,
_x2190-5061
505 0 _a -- 1 Introduction. -- 2 Methods. -- 3 Results. -- 4 Discussion. -- 5 Conclusion.
520 _aThis book provides a comprehensive description of advances in the study of general relativistic instability supernovae. These supernovae, if observed, would provide direct evidence of the existence of supermassive stars, thus confirming that massive seed black holes played a crucial role in the assembly of observed high redshift quasars. The book begins with a review of the history of and motivation for the study of supermassive stars. Supermassive stars are most likely to exist in the high redshift universe and are thus difficult to find. One possibility for observing these stars is the thermonuclear explosion occurring at the end of the lives of some supermassive stars. In order to model these explosions, the author first performs evolutionary simulations with a post Newtonian stellar evolution code HOSHI, evolves these simulations to the general relativistic radial instability, locating the instability using a normal mode analysis of the radial perturbations of the star in general relativity. Next, when the star becomes unstable, the author simulates the dynamics of the explosion or collapse to a black hole by transporting the model to a general relativistic Lagrangian hydrodynamics code with a nuclear network. The two main explosion mechanisms for these stars are the explosive alpha process and the CNO cycle and rapid proton capture process. If the model explodes, the nucleosynthetic ejecta and the light-curve are computed. For multiple types of supermassive stars, it is found that general relativistic instability supernovae are a general consequence of the existence of supermassive stars which are destabilized during their evolution by general relativity. These results run contrary to those of previous papers which found that these types of explosions were much rarer. The results are compared to existing James Webb Space Telescope data and prospects for observation using future instruments are discussed. The book is intended for physics and astronomy researchers interested in the origin and growth of massive black holes, the evolution and explosions of massive stars, and supernovae and chemical enrichment of the early universe.
650 0 _aAstrophysics.
_968037
650 0 _aAstronomy
_xObservations.
_967976
650 0 _aGravitation.
650 0 _aCosmology.
_976015
650 1 4 _aAstrophysics.
_968037
650 2 4 _aAstronomy, Observations and Techniques.
_967977
650 2 4 _aGravitational Physics.
_969498
650 2 4 _aCosmology.
_976015
710 2 _aSpringerLink (Online service)
773 0 _tSpringer Nature eBook
776 0 8 _iPrinted edition:
_z9789819605507
776 0 8 _iPrinted edition:
_z9789819605521
776 0 8 _iPrinted edition:
_z9789819605538
830 0 _aSpringer Theses, Recognizing Outstanding Ph.D. Research,
_x2190-5061
_966370
856 4 0 _uhttps://doi.org/10.1007/978-981-96-0551-4
912 _aZDB-2-PHA
912 _aZDB-2-SXP
999 _c66650
_d66650