Population synthesis of isolated neutron stars with magneto-rotational evolution – II. From radio-pulsars to magnetars

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Title: Population synthesis of isolated neutron stars with magneto-rotational evolution – II. From radio-pulsars to magnetars
Authors: Gullón Juanes, Miguel | Pons, José A. | Miralles, Juan A. | Viganò, Daniele | Rea, Nanda | Perna, Rosalba
Research Group/s: Astrofísica Relativista
Center, Department or Service: Universidad de Alicante. Departamento de Física Aplicada
Keywords: Stars: magnetic field | Stars: neutron | Pulsars: general
Knowledge Area: Astronomía y Astrofísica
Issue Date: 21-Nov-2015
Publisher: Oxford University Press
Citation: Monthly Notices of the Royal Astronomical Society. 2015, 454(1): 615-625. doi:10.1093/mnras/stv1644
Abstract: Population synthesis studies constitute a powerful method to reconstruct the birth distribution of periods and magnetic fields of the pulsar population. When this method is applied to populations in different wavelengths, it can break the degeneracy in the inferred properties of initial distributions that arises from single-band studies. In this context, we extend previous works to include X-ray thermal emitting pulsars within the same evolutionary model as radio-pulsars. We find that the cumulative distribution of the number of X-ray pulsars can be well reproduced by several models that, simultaneously, reproduce the characteristics of the radio-pulsar distribution. However, even considering the most favourable magneto-thermal evolution models with fast field decay, lognormal distributions of the initial magnetic field overpredict the number of visible sources with periods longer than 12 s. We then show that the problem can be solved with different distributions of magnetic field, such as a truncated lognormal distribution, or a binormal distribution with two distinct populations. We use the observational lack of isolated neutron stars (NSs) with spin periods P > 12 s to establish an upper limit to the fraction of magnetars born with B > 1015 G (less than 1 per cent). As future detections keep increasing the magnetar and high-B pulsar statistics, our approach can be used to establish a severe constraint on the maximum magnetic field at birth of NSs.
Sponsor: This work was supported in part by the grants AYA2013-42184-P and Prometeu/2014/69, and by the New Comp-star COST action MP1304. MG is supported by the fellowship BES-2011-049123. DV and NR acknowledges support from grants AYA2012-39303 and SGR2014-1073. NR is additionally supported by an NWO Vidi award.
URI: http://hdl.handle.net/10045/51289
ISSN: 0035-8711 (Print) | 1365-2966 (Online)
DOI: 10.1093/mnras/stv1644
Language: eng
Type: info:eu-repo/semantics/article
Rights: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Peer Review: si
Publisher version: http://dx.doi.org/10.1093/mnras/stv1644
Appears in Collections:INV - Astrofísica Relativista - Artículos de Revistas

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