Constraining the GRB-Magnetar Model by Means of the Galactic Pulsar Population

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Title: Constraining the GRB-Magnetar Model by Means of the Galactic Pulsar Population
Authors: Rea, Nanda | Gullón Juanes, Miguel | Pons, José A. | Perna, Rosalba | Dainotti, Maria G. | Miralles, Juan A. | Torres, Diego F.
Research Group/s: Astrofísica Relativista
Center, Department or Service: Universidad de Alicante. Departamento de Física Aplicada
Keywords: Gamma-ray burst: general | Pulsars: general | Stars: magnetars
Knowledge Area: Astronomía y Astrofísica
Issue Date: 10-Nov-2015
Publisher: IOP Publishing
Citation: The Astrophysical Journal. 2015, 813(92): 8pp. doi:10.1088/0004-637X/813/2/92
Abstract: A large fraction of Gamma-ray bursts (GRBs) displays an X-ray plateau phase within <105 s from the prompt emission, proposed to be powered by the spin-down energy of a rapidly spinning newly born magnetar. In this work we use the properties of the Galactic neutron star population to constrain the GRB-magnetar scenario. We re-analyze the X-ray plateaus of all Swift GRBs with known redshift, between 2005 January and 2014 August. From the derived initial magnetic field distribution for the possible magnetars left behind by the GRBs, we study the evolution and properties of a simulated GRB-magnetar population using numerical simulations of magnetic field evolution, coupled with Monte Carlo simulations of Pulsar Population Synthesis in our Galaxy. We find that if the GRB X-ray plateaus are powered by the rotational energy of a newly formed magnetar, the current observational properties of the Galactic magnetar population are not compatible with being formed within the GRB scenario (regardless of the GRB type or rate at z = 0). Direct consequences would be that we should allow the existence of magnetars and "super-magnetars" having different progenitors, and that Type Ib/c SNe related to Long GRBs form systematically neutron stars with higher initial magnetic fields. We put an upper limit of ≤16 "super-magnetars" formed by a GRB in our Galaxy in the past Myr (at 99% c.l.). This limit is somewhat smaller than what is roughly expected from Long GRB rates, although the very large uncertainties do not allow us to draw strong conclusion in this respect.
Sponsor: N.R. is supported by an NWO Vidi Grant, and kindly acknowledges Harvard ITC, NYU, Stony Brook University and the MIAPP institute in Garching, for the hospitality during the preparation of this work. N.R. and D.F.T. are also supported by grants AYA2012-39303 and SGR2014-1073. M.G. is supported by the fellowship BES-2011-049123. M.G., J.A.P. and J.A.M. acknowledge support by grants AYA2013-42184-P and Prometeu/2014/69. R.P. acknowledges support from NSF grant No. AST 1009396. M.G.D. is supported by FP7-PEOPLE-2013-IOF under the grant agreement number 626267, and thanks the ITHES group and the Astrophysical Big Bang Laboratory for fruitful discussions. This work is partially supported by the European COST Action MP1304 (NewCOMPSTAR).
ISSN: 0004-637X (Print) | 1538-4357 (Online)
DOI: 10.1088/0004-637X/813/2/92
Language: eng
Type: info:eu-repo/semantics/article
Rights: © 2015. The American Astronomical Society
Peer Review: si
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Appears in Collections:Research funded by the EU
INV - Astrofísica Relativista - Artículos de Revistas

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