Yoneda, Hiroki and Done, Chris and Paerels, Frits and Takahashi, Tadayuki and Watanabe, Shin (2018) 'Search for gravitational redshifted absorption lines in LMXB Serpens X-1.', Monthly notices of the Royal Astronomical Society., 475 (2). pp. 2194-2203.
The equation of state for ultradense matter can be tested from observations of the ratio of mass to radius of neutron stars. This could be measured precisely from the redshift of a narrow line produced on the surface. X-rays bursts have been intensively searched for such features, but so far without detection. Here instead we search for redshifted lines in the persistent emission, where the accretion flow dominates over the surface emission. We discuss the requirements for narrow lines to be produced, and show that narrow absorption lines from highly ionized iron can potentially be observable in accreting low-mass X-ray binaries (LMXBs; low B field) that have either low spin or low inclination so that Doppler broadening is small. This selects Serpens X-1 as the only potential candidate persistent LMXB due to its low inclination. Including surface models in the broad-band accretion flow model predicts that the absorption line from He-like iron at 6.7 keV should be redshifted to ∼5.1–5.7 keV (10–15 km for 1.4 M⊙) and have an equivalent width of 0.8–8 eV for surface temperatures of 7–10 × 106 K. We use the high-resolution Chandra grating data to give a firm upper limit of 2–3 eV for an absorption line at ∼5 keV. We discuss possible reasons for this lack of detection (the surface temperature and the geometry of the boundary layer etc.). Future instruments with better sensitivity are required in order to explore the existence of such features.
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|Publisher Web site:||https://doi.org/10.1093/mnras/stx3328|
|Publisher statement:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||21 December 2017|
|Date deposited:||29 March 2018|
|Date of first online publication:||27 December 2017|
|Date first made open access:||29 March 2018|
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