Dynamics and Statistical Mechanics of Keplerian Stellar Systems

Kaur, Karamveer

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7311

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DC Field	Value	Language
dc.contributor.advisor	Sridhar, S.	-
dc.contributor.author	Kaur, Karamveer	-
dc.date.accessioned	2019-10-11T12:11:18Z	-
dc.date.available	2019-10-11T12:11:18Z	-
dc.date.issued	2019-08	-
dc.identifier.citation	Ph.D. Thesis, Jawaharlal Nehru University, New Delhi, 2019	en_US
dc.identifier.uri	http://hdl.handle.net/2289/7311	-
dc.description	Restricted Access	en_US
dc.description.abstract	The nuclear star clusters (NSCs) orbiting massive blackholes (MBHs) at the centres of many galaxies are the densest known stellar systems, where the number density of stars can exceed those in globular clusters by a factor of 1000. The morphologies and kinematics of NSCs are varied (Seth et al., 2006), and questions concerning their dynamical evolution form the subject of this thesis. These are motivated by observations of the inner regions of the nearest two NSCs: the lopsided nuclear disc of M31 (Lauer et al., 1993), and the Milky Way NSC with its spheroid of old stars (Genzel et al., 2010) and a remnant disc of young stars (Yelda et al., 2014). The thesis explores the gravitational dynamics and kinetics of NSCs within the radius of influence of the MBH. The research presented is the first application of the general theory of secular dynamics and kinetics by Sridhar & Touma (2016a,b, 2017).	en_US
dc.language.iso	en	en_US
dc.publisher	Raman Research Institute, Bangalore.	en_US
dc.rights	2019 This thesis is posted here with the permission of the author. Personal use of this material is permitted. Any other use requires prior permission of the author. By choosing to view this document, you agree to all provisions of the copyright laws protecting it.	en_US
dc.subject.classification	Astronomy and Astrophysics	en
dc.title	Dynamics and Statistical Mechanics of Keplerian Stellar Systems	en_US
dc.type	Thesis	en_US
Appears in Collections:	Theses (A&A)

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