Jesús Misráyim Rueda-Becerril

Astrophysics, Computational Physics, Fluid Dynamics

MSc
7.91

Publications

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    Jesus M. Rueda-Becerril · Petar Mimica · Miguel A. Aloy
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    ABSTRACT: The internal shocks scenario in relativistic jets is used to explain the variability of the blazar emission. Recent studies have shown that the magnetic field significantly alters the shell collision dynamics, producing a variety of spectral energy distributions and light-curves patterns. However, the role played by magnetization in such emission processes is still not entirely understood. In this work we numerically solve the magnetohydodynamic evolution of the magnetized shells collision, and determine the influence of the magnetization on the observed radiation. Our procedure consists in systematically varying the shell Lorentz factor, relative velocity, and viewing angle. The calculations needed to produce the whole broadband spectral energy distributions and light-curves are computationally expensive, and are achieved using a high-performance parallel code.
    Full-text · Article · Feb 2015
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    J. M. Rueda-Becerril · P. Mimica · M. A. Aloy
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    ABSTRACT: We explore the signature imprinted by dynamically relevant magnetic fields on the spectral energy distribution (SED) of blazars. It is assumed that the emission from these sources originates from the collision of cold plasma shells, whose magnetohydrodynamic evolution we compute by numerically solving Riemann problems. We compute the SEDs including the most relevant radiative processes and scan a broad parameter space that encompasses a significant fraction of the commonly accepted values of not directly measurable physical properties. We reproduce the standard double-hump SED found in blazar observations for unmagnetized shells, but show that the prototype double-hump structure of blazars can also be reproduced if the dynamical source of the radiation field is very ultrarelativistic both, in a kinematically sense (namely, if it has Lorentz factors ≳50) and regarding its magnetization (e.g. with flow magnetizations σ ≃ 0.1). A fair fraction of the blazar sequence could be explained as a consequence of shell magnetization: negligible magnetization in flat-spectrum radio quasars, and moderate or large (and uniform) magnetization in BL Lacs. The predicted photon spectral indices (Γph) in the γ-ray band are above the observed values (Γph, obs ≲ 2.6 for sources with redshifts 0.4 ≤ z ≤ 0.6) if the magnetization of the sources is moderate (σ ≃ 10−2).
    Full-text · Article · Oct 2013 · Monthly Notices of the Royal Astronomical Society
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    Jesus M. Rueda-Becerril · Petar Mimica · Miguel A. Aloy · Carmen Aloy
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    ABSTRACT: The internal-shocks scenario in relativistic jets has been used to explain the variability of blazars' outflow emission. Recent simulations have shown that the magnetic field alters the dynamics of these shocks producing a whole zoo of spectral energy density patterns. However, the role played by magnetization in such high-energy emission is still not entirely understood. With the aid of \emph{Fermi}'s second LAT AGN catalog, a comparison with observations in the $\gamma$-ray band was performed, in order to identify the effects of the magnetic field.
    Full-text · Article · Sep 2013 · The European Physical Journal Conferences
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    Petar Mimica · Miguel Angel Aloy · Jesus M. Rueda-Becerril · Siham Tabik · Carmen Aloy
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    ABSTRACT: Broadband emission from relativistic outflows (jets) of active galactic nuclei (AGN) and gamma-ray bursts (GRBs) contains valuable information about the nature of the jet itself, and about the central engine which launches it. Using special relativistic hydrodynamics and magnetohydronamics simulations we study the dynamics of the jet and its interaction with the surrounding medium. The observational signature of the simulated jets is computed using a radiative transfer code developed specifically for the purpose of computing multi-wavelength, time-dependent, non-thermal emission from astrophysical plasmas. We present results of a series of long-term projects devoted to understanding the dynamics and emission of jets in parsec-scale AGN jets, blazars and the afterglow phase of the GRBs.
    Full-text · Article · Nov 2012 · Journal of Physics Conference Series
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    F. S. Guzman · J. M. Rueda-Becerril
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    ABSTRACT: We present spherically symmetric boson stars as black hole mimickers based on the power spectrum of a simple accretion disk model. The free parameters of the boson star are the mass of the boson and the fourth order self-interaction coefficient in the scalar field potential. We show that even if the mass of the boson is the only free parameter it is possible to find a configuration that mimics the power spectrum of the disk due to a black hole of the same mass. We also show that for each value of the self-interaction a single boson star configuration can mimic a black hole at very different astrophysical scales in terms of the mass of the object and the accretion rate. In order to show that it is possible to distinguish one of our mimickers from a black hole we also study the deflection of light. Comment: 8 revtex pages, 10 eps figures
    Full-text · Article · Sep 2010 · Physical review D: Particles and fields

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