Chandra monitoring of the Galactic Centre magnetar SGR J1745−2900 during the initial 3.5 years of outburst decay

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Título: Chandra monitoring of the Galactic Centre magnetar SGR J1745−2900 during the initial 3.5 years of outburst decay
Autor/es: Coti Zelati, Francesco | Rea, Nanda | Turolla, Roberto | Pons, José A. | Papitto, Alessandro | Esposito, Paolo | Israel, Gian Luca | Campana, Sergio | Zane, Silvia | Tiengo, Andrea | Mignani, Roberto P. | Mereghetti, Sandro | Baganoff, Frederick K. | Haggard, Daryl | Ponti, Gabriele | Torres, Diego F. | Borghese, Alice | Elfritz, Justin G.
Grupo/s de investigación o GITE: Astrofísica Relativista
Centro, Departamento o Servicio: Universidad de Alicante. Departamento de Física Aplicada
Palabras clave: Methods: data analysis | Methods: observational | Stars: magnetars | Galaxy: centre | X-rays: individual: SGR J1745−2900
Área/s de conocimiento: Astronomía y Astrofísica
Fecha de publicación: 6-jul-2017
Editor: Oxford University Press
Cita bibliográfica: Monthly Notices of the Royal Astronomical Society. 2017, 471(2): 1819-1829. doi:10.1093/mnras/stx1700
Resumen: We report on 3.5 yr of Chandra monitoring of the Galactic Centre magnetar SGR J1745−2900 since its outburst onset in 2013 April. The magnetar spin-down has shown at least two episodes of period derivative increases so far, and it has slowed down regularly in the past year or so. We observed a slightly increasing trend in the time evolution of the pulsed fraction, up to ∼55 per cent in the most recent observations. SGR J1745−2900 has not reached the quiescent level yet, and so far the overall outburst evolution can be interpreted in terms of a cooling hot region on the star surface. We discuss possible scenarios, showing in particular how the presence of a shrinking hotspot in this source is hardly reconcilable with internal crustal cooling and favours the untwisting bundle model for this outburst. Moreover, we also show how the emission from a single uniform hotspot is incompatible with the observed pulsed fraction evolution for any pair of viewing angles, suggesting an anisotropic emission pattern.
Patrocinador/es: FCZ, NR, PE, AB and JE acknowledge funding in the framework of a Vidi award A.2320.0076 of the Netherlands Organisation for Scientific Research (PI: N. Rea), and the European COST Action MP1304 (NewCOMPSTAR). FCZ, NR and DFT are supported by grant AYA2015-71042-P. NR and DFT are also supported by grant SGR2014-1073. RT, AT and SM acknowledge financial contribution from the agreement ASI/INAF I/037/12/0 and from PRIN INAF 2014. JAP acknowledges support by grants AYA2015-66899-C2-2-P and PROMETEOII-2014-069. AP is supported via an EU Marie Sködowska-Curie Individual fellowship under contract no. 660657-TMSP-H2020-MSCA-IF-2014. RPM acknowledges financial support from an ‘Occhialini Fellowship’. DH acknowledges support from a Natural Sciences and Engineering Research Council of Canada Discovery Grant and a Fonds de recherche du Québec Nature et Technologies Nouveaux Chercheurs Grant. GP acknowledges support via the Bundesministerium für Wirtschaft und Technologie/Deutsches Zentrum für Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OR 1604) and the Max Planck Society.
ISSN: 0035-8711 (Print) | 1365-2966 (Online)
DOI: 10.1093/mnras/stx1700
Idioma: eng
Tipo: info:eu-repo/semantics/article
Derechos: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Revisión científica: si
Versión del editor:
Aparece en las colecciones:INV - Astrofísica Relativista - Artículos de Revistas

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