Quasi-Normal Modes of Stars and Black Holes by Kokkotas, K D; Schmidt, B G

By Kokkotas, K D; Schmidt, B G

Show description

Read Online or Download Quasi-Normal Modes of Stars and Black Holes PDF

Best nonfiction_7 books

Photogrammetric Image Analysis: ISPRS Conference, PIA 2011, Munich, Germany, October 5-7, 2011. Proceedings

This booklet constitutes the refereed court cases of the ISPRS convention on Photogrammetric photograph research, held in Munich, Germany, in October 2011. The 25 revised complete papers provided have been rigorously reviewed and chosen from fifty four submissions. The papers are prepared in topical sections on orientation, matching, item detection, 3D reconstruction and DEM, category, humans and monitoring, in addition to photograph processing.

Transition, Turbulence and Combustion Modelling: Lecture Notes from the 2nd ERCOFTAC Summerschool held in Stockholm, 10–16 June, 1998

The purpose of the current booklet is to offer, in one quantity, an advent to the fields of transition, turbulence and combustion modelling of compressible flows and to supply the actual historical past for modern-day modelling methods in those fields. the fundamental equations for compressible flows are provided (Ch.

Additional resources for Quasi-Normal Modes of Stars and Black Holes

Sample text

The extension of this scheme to other cases, like neutron star collisions or supernovae collapse, is not trivial. But if one can define even numerical data on the initial hypersurface then the perturbation method will be probably enough or at least a very good test for the reliability of fully numerical evolutions. For a recent attempt towards applying the above techniques in colliding neutron stars see [6, 20]. Before going into details we would like to point out an important issue, namely the effect of the potential barrier on the QNMs of black holes.

Their Fig. 2) shows some enhancement around 7 kHz. Recently, Andersson and Kokkotas [18] have studied the excitation of axial modes by sending gravitational wave pulses to hit the star (see figure 5). The results of this study are encouraging because they provide the first indication that the w-modes can be excited in a dynamical scenario. Similar results have recently been obtained by Borelli [48] for particles falling onto a neutron star. The excitation of the axial QNMs by test particles scattered by a neutron star have been recently studied in detail [203, 84, 27] and some interesting conclusions can be drawn.

Following in the same spirit are more recent calculations [6] of the close limit for two identical neutron stars. The results show the excitation of stellar QNMs and it remains for numerical relativity to verify the results. Finally, perturbation theory can be also used as a tool to construct a gauge invariant measure of the gravitational radiation in a numerically generated perturbed black hole spacetime [7, 184]. 2 Second Order Perturbations A basic feature of linearized perturbation theory is that there is no “built-in” indication of how good the approximation is.

Download PDF sample

Rated 4.65 of 5 – based on 6 votes