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  The very-faint X-ray binary IGR J17062-6143: a truncated disk, no pulsations and a possible outflow

Eijnden, J. v. d., Degenaar, N., Pinto, C., Patruno, A., Wette, K., Messenger, C., et al. (2018). The very-faint X-ray binary IGR J17062-6143: a truncated disk, no pulsations and a possible outflow. Monthly Notices of the Royal Astronomical Society, 475(2), 2027-2044. doi:10.1093/mnras/stx3224.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0001-1A93-C Version Permalink: http://hdl.handle.net/21.11116/0000-0002-E9F0-8
Genre: Journal Article

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 Creators:
Eijnden, J. van den, Author
Degenaar, N., Author
Pinto, C., Author
Patruno, A., Author
Wette, K.1, Author              
Messenger, C., Author
Santisteban, J. V. Hernandez, Author
Wijnands, R., Author
Miller, J. M., Author
Altamirano, D., Author
Paerels, F., Author
Chakrabarty, D., Author
Fabian, A. C., Author
Affiliations:
1Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: We present a comprehensive X-ray study of the neutron star low-mass X-ray binary IGR J17062-6143, which has been accreting at low luminosities since its discovery in $2006$. Analysing NuSTAR, XMM-Newton and Swift observations, we investigate the very faint nature of this source through three approaches: modelling the relativistic reflection spectrum to constrain the accretion geometry, performing high-resolution X-ray spectroscopy to search for an outflow, and searching for the recently reported millisecond X-ray pulsations. We find a strongly truncated accretion disk at $77^{+22}_{-18}$ gravitational radii ($\sim 164$ km) assuming a high inclination, although a low inclination and a disk extending to the neutron star cannot be excluded. The high-resolution spectroscopy reveals evidence for oxygen-rich circumbinary material, possibly resulting from a blueshifted, collisionally-ionised outflow. Finally, we do not detect any pulsations. We discuss these results in the broader context of possible explanations for the persistent faint nature of weakly accreting neutron stars. The results are consistent with both an ultra-compact binary orbit and a magnetically truncated accretion flow, although both cannot be unambigiously inferred. We also discuss the nature of the donor star and conclude that it is likely a CO or O-Ne-Mg white dwarf, consistent with recent multi-wavelength modelling.

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 Dates: 2017-12-112018
 Publication Status: Published in print
 Pages: 22 pages, 9 figures; accepted for publication in MNRAS
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 Rev. Method: -
 Identifiers: arXiv: 1712.03949
URI: http://arxiv.org/abs/1712.03949
DOI: 10.1093/mnras/stx3224
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Title: Monthly Notices of the Royal Astronomical Society
Source Genre: Journal
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Pages: - Volume / Issue: 475 (2) Sequence Number: - Start / End Page: 2027 - 2044 Identifier: -