Bibliographic Details
| Title: |
X-ray observations of FO Aqr during the 2016 low state. |
| Authors: |
Kennedy, M. R.1,2 markkennedy@umail.ucc.ie, Garnavich, P. M.2, Littlefield, C.2, Callanan, P.1, Mukai, K.3,4, Aadland, E.5, Kotze, M. M.6,7, Kotze, E. J.6,8 |
| Source: |
Monthly Notices of the Royal Astronomical Society. Jul2017, Vol. 469 Issue 1, p956-967. 12p. |
| Subject Terms: |
*ACCRETION in galactic x-ray sources, *ECLIPSING binaries, *COSMIC magnetic fields, *NOVAE (Astronomy), *CATACLYSMIC variable stars |
| Abstract: |
We present the first ever X-ray data taken of an intermediate polar, FO Aquarii (FO Aqr), when in a low accretion state and during the subsequent recovery. Both the Swift and Chandra X-ray data taken during the low accretion state in 2016 July show a softer spectrum when compared to archival data taken when FO Aqr was in a high state. The X-ray spectrum in the low state showed a significant increase in the ratio of the soft X-ray flux to the hard X-ray flux due to a change in the partial covering fraction of the white dwarf from >85 per cent to 70+5 -8 per cent and a change in the hydrogen column density within the disc from 19+1.2 -0.9 × 1022 to 1.3+0.6 -0.3 × 1022 cm-2. XMM–Newton observations of FO Aqr during the subsequent recovery suggest that the system had not yet returned to its typical high state by 2016 November, with the hydrogen column density within the disc found to be 15+3.0 -2.0 cm-2. The partial covering fraction varied in the recovery state between 85 per cent and 95 per cent. The spin period of the white dwarf in 2014 and 2015 has also been refined to 1254.3342(8) s. Finally, we find an apparent phase difference between the high state X-ray pulse and recovery X-ray pulse of 0.17, which may be related to a restructuring of the X-ray-emitting regions within the system. [ABSTRACT FROM AUTHOR] |
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