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    Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind

    74389.pdf (1.720Mb)
    Access Status
    Open access
    Authors
    Gatuzz, E.
    Trigo, M.
    Miller-Jones, James
    Migliari, S.
    Date
    2019
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Gatuzz, E. and Trigo, M. and Miller-Jones, J. and Migliari, S. 2019. Chandra high-resolution spectra of 4U 1630-47: the disappearance of the wind. Monthly Notices of the Royal Astronomical Society. 482 (2): pp. 2597-2611.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/sty2850
    ISSN
    0035-8711
    School
    Curtin Institute of Radio Astronomy (Physics)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/74104
    Collection
    • Curtin Research Publications
    Abstract

    We present the analysis of six Chandra X-ray high-resolution observations of the black hole low-mass X-ray binary 4U 1630-47 taken during its 2012–2013 outburst. Fe XXVI K α, K β, Fe XXV K α, K β, and Ca XX K α blueshifted absorption lines were identified in the first four observations, which correspond to soft accretion states. The remaining observations, associated to intermediate and possibly hard accretion states, do not show significant absorption features down to equivalent width of 1 eV for both Fe XXVI and Fe XXV. We inferred wind launching radii between 1.2 − 2.0 (1012 cm/n) × 1011 cm and column densities N(H) > 1023 cm−2. In the first four observations, we found that thermal pressure is likely to be the dominant launching mechanism for the wind, although such conclusions depend on the assumed density. We used the spectral energy distributions obtained from our continuum modelling to compute thermal stability curves for all observations using the XSTAR photoionization code. We found that the absence of lines in the transitional state cannot be attributed to an evolution of the plasma caused by thermal instabilities derived from the change in the continuum spectrum. In contrast, the disappearance of the wind could indicate an acceleration of the flow or that the plasma has been exhausted during the soft state.

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