ORBITAL-PHASE-RESOLVED SPECTROSCOPY OF THE INTERMEDIATE POLAR FO AQR USING<i>XMM-NEWTON</i>OBSERVATORY DATA

Pekön, Yakup; Balman, Ş.

doi:10.1088/0004-6256/144/2/53

Cited by 3 publications

(2 citation statements)

References 32 publications

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“…The cause of the orbital modulation is thought to be due to photoelectric absorption by material in the impact region between the ballistic stream and the accretion disc. Pekön & Balman (2012) also noted this behaviour in FO Aqr, and showed how the X-ray spectrum varied over the orbital period.…”

Section: Introductionmentioning

confidence: 70%

X-ray observations of FO Aqr during the 2016 low state

Kennedy

Garnavich

Callanan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first ever X-ray data taken of an intermediate polar, FO Aqr, when in a low accretion state and during the subsequent recovery. The Swift and Chandra X-ray data taken during the low accretion state in July 2016 both 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% to 70 +5 −8 % and a change in the hydrogen column density within the disc from 19 +1.2 −0.9 × 10 22 cm −2 to 1.3 +0.6 −0.3 × 10 22 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 November 2016, 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% and 95%. 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.

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Section: Introductionmentioning

confidence: 70%

X-ray observations of FO Aqr during the 2016 low state

Kennedy

Garnavich

Callanan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Physics at the Magnetospheric Boundary spectrum of the source can be represented with a complex absorption, multiple plasma emission and Gaussian lines (See [7] and references therein) Fo Aqr was observed with XMM-Newton on 12 May 2001 for 35 ks and after standard pipeline was followed for data preparation, EPIC pn data was utilized since it has a better sensitivity. Standard tools and packages such as SAS, XRONOS and XSPEC were used in order to perform the spectral and timing analysis (See Pekon & Balman 2012 for full analysis).…”

Section: Fo Aqrmentioning

confidence: 99%

Phase Resolved X-Ray Spectral Analysis of Intermediate Polars EX Hya and FO Aqr

Pekön

Balman

2014

EPJ Web of Conferences

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Abstract. Intermediate Polars (IPs): EX Hya and FO Aqr whichs are a subclass of Cataclysmic Variables (CVs) where a white dwarf with magnetic field strength of about 1-10 MG accretes material from a main sequence companion through a truncated disc. In this talk we present orbital and spin phase-resolved X-ray spectroscopy of EX Hya and orbital phase-resolved X-ray spectroscopy of FO Aqr. We utilize XMM-Newton archive data of these objects for analysis. We investigate the change of the source spectrum over the spin and orbital periods. This analysis enhances our understanding about the accretion structure in these systems, temperature and composition of the X-ray emitting region together with the structure of the outer accretion disc and absorption in the system

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A long serendipitous XMM–Newton observation of the intermediate polar XY Ari1

Çamurdan

Balman

Burwitz

2018

Monthly Notices of the Royal Astronomical Society

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XY Ari is one of the few known eclipsing intermediate polars. We present results from a detailed analysis of an unpublished archival observation using XMM-Newton EPIC pn and MOS data in a quiescent state of XY Ari. The X-ray orbital modulation and spin pulse variations were investigated for energy dependent modulations in different energy bands. The broad orbital modulation observed with various observations was confirmed with XMM-Newton at hard X-ray (>1.6 keV). The EPIC light curves folded at the spin phases show a double peak profile as expected from two pole accretion. The pulse profile is found to be energy dependent. Hardness ratio variations and energy modulation depth during spin modulation can be explained by photoelectric absorption. The simultaneously fitted EPIC spectra with CEVMKL model yield maximum plasma temperature of 28 +3.1 −2.9 keV with an iron abundance Fe/Fe = 0.37 +0.06 −0.05 . We find two intrinsic partial covering absorption columns of 6.2 +1.0 −0.9 ×10 22 and 105.3 +35.4 −30.4 ×10 22 cm −2 with covering fractions of 0.53 +0.05 −0.04 , 0.41 +0.14 −0.13 respectively. In addition, a Gaussian emission line at 6.43 +0.01 −0.02 keV with an equivalent width of 51 +12 −10 eV is required to account for fluorescent emission from neutral iron. The X-ray luminosity of the source is 4.2 × 10 32 erg s −1 in the 0.2-10.0 keV energy band.

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ORBITAL-PHASE-RESOLVED SPECTROSCOPY OF THE INTERMEDIATE POLAR FO AQR USINGXMM-NEWTONOBSERVATORY DATA

Cited by 3 publications

References 32 publications

X-ray observations of FO Aqr during the 2016 low state

X-ray observations of FO Aqr during the 2016 low state

Phase Resolved X-Ray Spectral Analysis of Intermediate Polars EX Hya and FO Aqr

A long serendipitous XMM–Newton observation of the intermediate polar XY Ari1

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