# Silvano Bonazzola - LUTH

## Contact Details

NameSilvano Bonazzola |
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AffiliationLUTH |
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Location |
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## Pubs By Year |
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## Pub CategoriesGeneral Relativity and Quantum Cosmology (5) High Energy Astrophysical Phenomena (4) Solar and Stellar Astrophysics (3) Astrophysics (3) Earth and Planetary Astrophysics (2) High Energy Physics - Phenomenology (1) High Energy Physics - Theory (1) Quantum Physics (1) Physics - Computational Physics (1) |

## Publications Authored By Silvano Bonazzola

**Affiliations:**

^{1}LUTH,

^{2}LUTH,

^{3}CNRS, LUTH

Neutron-star magnetospheres are structured by very intense magnetic fields extending from 100 to 10 5 km traveled by very energetic electrons and positrons with Lorentz factors up to $\sim$ 10 7. In this context, particles are forced to travel almost along the magnetic field with very small gyro-motion, potentially reaching the quantified regime. We describe the state of Dirac particles in a locally uniform, constant and curved magnetic field in the approximation that the Larmor radius is very small compared to the radius of curvature of the magnetic field lines. Read More

We present a new code, Lorene's Ghost (for Lorene's gravitational handling of spectral transport) developed to treat the problem of neutrino transport in supernovae with the use of spectral methods. First, we derive the expression for the nonrelativistic Liouville operator in doubly spherical coordinates (r, theta, phi, epsilon, Theta, Phi)$, and further its general relativistic counterpart. We use the 3 + 1 formalism with the conformally flat approximation for the spatial metric, to express the Liouville operator in the Eulerian frame. Read More

**Affiliations:**

^{1}LUTH,

^{2}OAS,

^{3}LUTH

We investigate whether one or many companions are orbiting the extremely intermittent pulsar PSR B1931+24. We constrained our analysis on previous observations of eight fundamental properties of PSR B1931+24. The most puzzling properties are the intermittent nature of the pulsar's activity, with active and quiet phases that alternate quasi-periodically; the variation of the slowing-down rate of its period between active and quiet phases; and because there are no timing residuals, it is highly unlikely that the pulsar has a massive companion. Read More

**Affiliations:**

^{1}LUTH,

^{2}LUTH,

^{3}OAS

We investigate whether there may be one or many companions orbiting at close distance to the light cylinder around the extremely intermittent pulsars PSR B1931+24 and PSR J1841-0500. These pulsars, behaving in a standard way when they are active, also "switch off" for durations of several days, during which their magnetospheric activity is interrupted or reduced. We constrained our analysis on eight fundamental properties of PSR B1931+24 that summarise the observations. Read More

We present a numerical method for handling the resolution of a general transport equation for radiative particles, aimed at physical problems with a general spherical geometry. Having in mind the computational time difficulties encountered in problems such as neutrino transport in astrophysical supernovae, we present a scheme based on full spectral methods in 6d spherical coordinates. This approach, known to be suited when the characteristic length of the dynamics is much smaller than the domain size, has the potential advantage of a global speedup with respect to usual finite difference schemes. Read More

**Affiliations:**

^{1}LUTH,

^{2}IAA-CSIC,

^{3}LUTH

**Category:**General Relativity and Quantum Cosmology

We present a numerical technique for solving evolution equations, as the wave equation, in the description of rotating astrophysical compact objects in comoving coordinates, which avoids the problems associated with the light cylinder. The technique implements a fast spectral matching between two domains in relative rotation: an inner spherical domain, comoving with the sources and lying strictly inside the light cylinder, and an outer inertial spherical shell. Even though the emphasis is placed on spectral techniques, the matching is independent of the specific manner in which equations are solved inside each domain, and can be adapted to different schemes. Read More

Binary black hole systems in the pre-coalescence stage are numerically constructed by demanding that the associated spacetime admits a helical Killing vector. Comparison with third order post-Newtonian calculations indicates a rather good agreement until the innermost stable circular orbit. Read More

**Affiliations:**

^{1}LUTH, CNRS, Observatoire de Paris,

^{2}LUTH, CNRS, Observatoire de Paris

**Category:**General Relativity and Quantum Cosmology

We present a new formulation of the multipolar expansion of an exact boundary condition for the wave equation, which is truncated at the quadrupolar order. Using an auxiliary function, that is the solution of a wave equation on the sphere defining the outer boundary of the numerical grid, the absorbing boundary condition is simply written as a perturbation of the usual Sommerfeld radiation boundary condition. It is very easily implemented using spectral methods in spherical coordinates. Read More

**Affiliations:**

^{1}DARC, CNRS, Observatoire de Paris,

^{2}DARC, CNRS, Observatoire de Paris,

^{3}DARC, CNRS, Observatoire de Paris

We present the first results from a new method for computing spacetimes representing corotating binary black holes in circular orbits. The method is based on the assumption of exact equilibrium. It uses the standard 3+1 decomposition of Einstein equations and conformal flatness approximation for the 3-metric. Read More

We study equilibrium sequences of close binary systems composed of identical polytropic stars in Newtonian gravity. The solving method is a multi-domain spectral method which we have recently developed. An improvement is introduced here for accurate computations of binary systems with stiff equation of state ($\gamma > 2$). Read More

**Affiliations:**

^{1}DARC, Obs. Meudon, Fr.,

^{2}DARC, Obs. Meudon, Fr.

**Category:**High Energy Physics - Phenomenology

A simple model is exhibited in which the remnant density of charged vortons is used to provide candidates for explaining the observed ultra high energy cosmic rays (above $10^{20}$ eV). These vortons would be accelerated in active galaxies and propagated through intergalactic medium with negligible losses of energy. The expected number density of observable events is shown to be consistent with extrapolation of the observations. Read More