MG14 - Talk detail

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The observation of several neutron stars with relatively low values of the surface magnetic field found in supernova remnants has led in recent years to controversial interpretations. A possible explanation is the slow rotation of the proto-neutron star at birth which is unable to amplify its magnetic field to typical pulsar levels. An alternative possibility, the hidden magnetic field scenario, seems to be favoured over the previous one due to the observation of three low magnetic field magnetars. This scenario considers the accretion of the fallback of the supernova debris onto the neutron star as the responsible for the observed low magnetic field. We have studied under which conditions the magnetic field of a neutron star can be buried into the crust due to an accreting fluid. We have considered a 1D calculation in general relativity to estimate the balance between the incoming accretion flow an the magnetosphere. Our study includes several models with different entropy, composition (including nuclear statistical equilibrium) and neutron star masses.

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We present initial results of the application of Total Variation (TV) denoising algorithms to LIGO real data. These algorithms, which do not need any a priori information about the signals, have been developed and fully tested in the context of image processing. In a recent paper we have shown the feasibility of these methods in the context of gravitational wave signals, for the considerably simpler case of signals embedded in additive Gaussian noise. Here, we apply our TV algorithms to two different types of numerically-simulated gravitational wave signals embedded in real noise, namely bursts produced from the core collapse of rotating stars and waveforms from binary black hole mergers.

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