Stellar dynamics around a massive black hole I: Secular collisionless theory

Sridhar, S.; Touma, Jihad R.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6462

Full metadata record

DC Field	Value	Language
dc.contributor.author	Sridhar, S.	-
dc.contributor.author	Touma, Jihad R.	-
dc.date.accessioned	2016-10-20T07:52:13Z	-
dc.date.available	2016-10-20T07:52:13Z	-
dc.date.issued	2016-06	-
dc.identifier.citation	Monthly Notices of the Royal Astronomical Society, 2016, Vol. 458, p4129-4142	en_US
dc.identifier.issn	0035-8711	-
dc.identifier.issn	1365-2966 - (online)	-
dc.identifier.uri	http://hdl.handle.net/2289/6462	-
dc.description	Open Access	en_US
dc.description.abstract	We present a theory in three parts, of the secular dynamics of a (Keplerian) stellar system of mass M orbiting a black hole of mass M∙≫M. Here we describe the collisionless dynamics; Papers II and III are on the (collisional) theory of Resonant Relaxation. The mass ratio, ε=M/M∙≪1, is a natural small parameter implying a separation of time scales between the short Kepler orbital periods and the longer orbital precessional periods. The collisionless Boltzmann equation (CBE) for the stellar distribution function (DF) is averaged over the fast Kepler orbital phase using the method of multiple scales. The orbit-averaged system is described by a secular DF, F, in a reduced phase space. F obeys a secular CBE that includes stellar self-gravity, general relativistic corrections up to 1.5 post-Newtonian order, and external sources varying over secular times. Secular dynamics, even with general time dependence, conserves the semi-major axis of every star. This additional integral of motion promotes extra regularity of the stellar orbits, and enables the construction of equilibria, F0, through a secular Jeans theorem. A linearized secular CBE determines the response and stability of F0. Spherical, non-rotating equilibria may support long-lived, warp-like distortions. We also prove that an axisymmetric, zero-thickness, flat disc is secularly stable to all in-plane perturbations, when its DF, F0, is a monotonic function of the angular momentum at fixed energy.	en_US
dc.language.iso	en	en_US
dc.publisher	Oxford University Press for the Royal Astronomical Society	en_US
dc.relation.uri	http://adsabs.harvard.edu/abs/2016MNRAS.458.4129S	en_US
dc.relation.uri	http://arxiv.org/abs/1509.02397	en_US
dc.relation.uri	http://dx.doi.org/10.1093/mnras/stw542	en_US
dc.rights	2016 The authors & the Royal Astronomical Society	en_US
dc.title	Stellar dynamics around a massive black hole I: Secular collisionless theory	en_US
dc.type	Article	en_US
Appears in Collections:	Research Papers (A&A)

Files in This Item:

File	Description	Size	Format
2016_MNRAS_458_4129.pdf Restricted Access	Open Access	305.88 kB	Adobe PDF	View/Open Request a copy

Show simple item record