The X-ray outburst of the Galactic Centre magnetar SGR J1745−2900 during the first 1.5 year

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Title: The X-ray outburst of the Galactic Centre magnetar SGR J1745−2900 during the first 1.5 year
Authors: Coti Zelati, Francesco | Rea, Nanda | Papitto, Alessandro | Viganò, Daniele | Pons, José A. | Turolla, Roberto | Esposito, Paolo | Haggard, Daryl | Baganoff, Frederick K. | Ponti, Gabriele | Israel, Gian Luca | Campana, Sergio | Torres, Diego F. | Tiengo, Andrea | Mereghetti, Sandro | Perna, Rosalba | Zane, Silvia | Mignani, Roberto P. | Possenti, Andrea | Stella, Luigi
Research Group/s: Astrofísica Relativista
Center, Department or Service: Universidad de Alicante. Departamento de Física Aplicada
Keywords: Stars: magnetars | Galaxy: centre | X-rays: individual: SGR J1745−2900
Knowledge Area: Astronomía y Astrofísica
Issue Date: 21-May-2015
Publisher: Royal Astronomical Society
Citation: Monthly Notices of the Royal Astronomical Society. 2015, 449(3): 2685-2699. doi:10.1093/mnras/stv480
Abstract: In 2013 April a new magnetar, SGR 1745−2900, was discovered as it entered an outburst, at only 2.4 arcsec angular distance from the supermassive black hole at the centre of the Milky Way, Sagittarius A*. SGR 1745−2900 has a surface dipolar magnetic field of ∼2 × 1014 G, and it is the neutron star closest to a black hole ever observed. The new source was detected both in the radio and X-ray bands, with a peak X-ray luminosity LX ∼ 5 × 1035 erg s−1. Here we report on the long-term Chandra (25 observations) and XMM–Newton (eight observations) X-ray monitoring campaign of SGR 1745−2900 from the onset of the outburst in 2013 April until 2014 September. This unprecedented data set allows us to refine the timing properties of the source, as well as to study the outburst spectral evolution as a function of time and rotational phase. Our timing analysis confirms the increase in the spin period derivative by a factor of ∼2 around 2013 June, and reveals that a further increase occurred between 2013 October 30 and 2014 February 21. We find that the period derivative changed from 6.6 × 10−12 to 3.3 × 10−11 s s−1 in 1.5 yr. On the other hand, this magnetar shows a slow flux decay compared to other magnetars and a rather inefficient surface cooling. In particular, starquake-induced crustal cooling models alone have difficulty in explaining the high luminosity of the source for the first ∼200 d of its outburst, and additional heating of the star surface from currents flowing in a twisted magnetic bundle is probably playing an important role in the outburst evolution.
URI: http://hdl.handle.net/10045/47030
ISSN: 0035-8711 (Print) | 1365-2966 (Online)
DOI: 10.1093/mnras/stv480
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/stv480
Appears in Collections:INV - Astrofísica Relativista - Artículos de Revistas

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