The orbits of stars close to a massive black hole are nearly Keplerian ellipses. Such orbits exert long term torques on each other, which lead to an enhanced angular momentum relaxation known as resonant relaxation. Under certain conditions, this process can modify the angular momentum distribution and affect the interaction rates of the stars with the massive black hole more efficiently than n...

A compact binary on an eccentric orbit radiates gravitational waves (GWs) at all integer harmonics of its orbital frequency. Thus, the spectral energy distribution, the power and the timescale of GW radiation of a binary on an eccentric orbit are different from those of a binary on a circular orbit. Therefore, in order to predict spectra of gravitational wave background radiation (GWBR) from co...

We consider the effect of gravitational perturbations from a nearby satellite on the eccentricity e of a narrow particulate ring. The perturbations near a resonance in an eccentric ring may be divided into corotation and Lindblad terms. For small e, the corotation terms da,np e, whereas the Lindblad terms excite e. In the absence of saturation the corotation terms win by. a small margin, and e ...

INTRODUCTION Postoperative eccentric macular hole formation is an uncommon complication after pars plana vitrectomy (PPV) without internal limiting membrane (ILM) peeling for the treatment of epiretinal membrane (ERM). We present a case of eccentric macular hole formation after PPV for ERM without ILM peeling. CASE REPORT A 68-year-old male patient presented with ERM and visual acuity of 6/24...

The central bulge of M31 is observed to have two distinct brightness peaks with the separation of ∼ 2 pc. Tremaine (1995) recently proposed a new idea that the M31’s nucleus is actually a single thick eccentric disk surrounding the central super-massive black hole. In order to explore the origin of the proposed eccentric disk, we numerically investigate the dynamical evolution of a merger betwe...

We consider the possibility that an infalling bulge core or stellar cluster could form an eccentric disk, following tidal disruption by a massive black hole in the center of a galaxy. As a function of central black hole mass, we constrain the core radii and central densities of cluster progenitors capable of becoming nearly Keplerian disks which can support lopsided slow modes. We find that pro...

The triple nucleus of M31 consists of a population of old red stars in an eccentric disk (P1 and P2) and another population of younger A stars in a circular disk (P3) around M31’s central supermassive black hole (SMBH). We argue that P1 and P2 determine the maximal radial extent of the younger A star population and provide the gas that fueled the starburst that generated P3. The eccentric stell...