6.1 Harmonic Oscillator Reif §6.1: A simple harmonic one-dimensional oscillator has energy levels given by E n = (n + 1 2)ω, where ω is the characteristic (angular) frequency of the oscillator and where the quantum number n can assume the possible integral values n = 0, 1, 2,. . .. Suppose that such an oscillator is in thermal contact with a heat reservoir at temperature T low enough so that kT...

We note that the recently discovered 450 Hz frequency in the X-ray flux of the black hole candidate GRO J1655-40 is in a 3:2 ratio to the previously known 300 Hz frequency of quasi-periodic oscillations (QPO) in the same source. If the origin of high frequency QPOs in black hole systems is a resonance between orbital and epicyclic motion of accreting matter, as suggested previously, the angular...

A new explicit time-reversible orbit integrator for the equations of motion in a static homogeneous magnetic field —called Cyclotronic integrator— is presented. Like Spreiter and Walter’s Taylor expansion algorithm, for sufficiently weak electric field gradients this second order method does not require a fine resolution of the Larmor motion; it has however the essential advantage of being symp...

We investigate the modal properties of the r-modes with l = m in rotating neutron stars with the superfluid core, where l and m are the indices of the spherical harmonic function representing the angular dependence of the r-modes. For the modal analysis, we employ simple neutron star models, which are composed of the normal fluid envelope and the core filled with neutron and proton superfluids ...

We calculate the vacuum polarization-induced ellipticity acquired by a linearly polarized laser beam of angular frequency ω̄ on traversing a region containing a transverse magnetic field rotating with a small angular velocity Ω around the beam axis. The transmitted beam contains the fundamental frequency ω̄ and weak sidebands of frequency ω̄±2Ω, but no other sidebands. To first order in small quan...

We investigate the modal properties of the r-modes of rotating neutron stars with the core filled with neutron and proton superfluids, taking account of entrainment effects between the superfluids. The stability of the r-modes against gravitational radiation reaction is also examined considering viscous dissipation due to shear and a damping mechanism called mutual friction between the superflu...

We study the fully non-adiabatic tidal response of a uniformly rotating unevolved 20M ⊙ star to the dominant l = m = 2 component of the companion's perturbing potential. This is done numerically with a 2D implicit finite difference scheme. We assume the star is rotating slowly with angular speed Ω s ≪ Ω c , so that the centrifugal force can be neglected, but the Coriolis force is taken fully in...

We investigate the properties of relativistic r-modes of slowly rotating neutron stars by using a relativistic version of the Cowling approximation. In our formalism, we take into account the influence of the Coriolis like force on the stellar oscillations, but ignore the effects of the centrifugal like force. For three neutron star models, we calculated the fundamental r-modes with l = m = 2 a...

conclusions where there is a relationship between two longitudinal and survival responses, joint modeling can estimate it. background admission to the icu (intensive care unit) is frequently complicated by early aki (acute kidney injury). the development of aki following cardiac surgery is particularly associated with increased mortality and morbidity. according to akin (acute kidney injury net...

Using a quantum Boltzmann equation framework, we analyze the nature of generic low-energy deformations critical Fermi surface, which exists at non-Fermi liquid fixed point system consisting fermions interacting with massless bosons. The behaviour arises due to itinerant quasiparticles surface strongly bosons, on other hand undergo Landau damping as result mutual interactions. Focussing collisio...