Physics in the extreme: X-ray and optical studies of magnetic white dwarfs and related objects

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dc.contributor.advisorCallanan, Paulen
dc.contributor.advisorGarnavich, Peteren
dc.contributor.authorKennedy, Mark R.
dc.contributor.funderNaughton Foundationen
dc.contributor.funderUniversity College Corken
dc.description.abstractIn this thesis, we present results from optical and X-ray studies of compact binary systems. These observations are used to constrain orbital parameters - mainly periods and inclinations for several cataclysmic variables - and examine the accretion structures within the systems. In Chapters 3 and 4, optical and X-ray studies of two interesting cataclysmic variables systems, Lanning 386 and MASTER OTJ192328.22+612413.5, are presented. The X-ray and optical data of these objects suggest that both systems have a high inclination and harbour weakly magnetic white dwarfs with spin periods 17-22 min. There is also a strong focus on studying the long term behaviour in intermediate polars in this thesis. Chapter 5 presents results from Kepler observations of FO Aquarii taken over 69 consecutive days. The shape of the light curve is consistent with the outer edge of the accretion disc being eclipsed and the detected period is longer than the last reported period of 1254.284(16) s, suggesting that FO Aqr was now spinning down, and had a positive P˙ at the time of the observations. Chapter 6 continues the work on FO Aquarii, and presents X-ray data taken during a low accretion state. The X-ray spectrum shows an 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 and a change in the hydrogen column density within the disc. 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. The spin period of the white dwarf in 2014 and 2015 is refined to 1254.3342(8) s. Chapter 7 focuses on CSS120422:J111127+571239, an “evolved main-sequence” channel cataclysmic variable. We present spectroscopy of CSS120422:J111127+571239 using the COS FUV instrument on the Hubble Space Telescope and using the MODS spectrograph on the Large Binocular Telescope. The UV spectrum shows Si IV, N V and He II, but no detectable C IV. The anomalous nitrogen/carbon ratio is seen in a small number of other CVs and confirms a unique binary evolution. We also present and compare the optical spectrum of V418 Ser and advocate that it is also an evolved main-sequence system. Finally, Chapter 8 presents results on UW Coronae Borealis, a low mass X-ray x Abstract binary that shows both Type 1 X-ray and optical bursts. The orbital period is refined to 110.97680(1) min. 17 optical bursts are presented, with 10 of these bursts being resolved temporally. The average e-folding time of 19 ± 3s for the bursts is consistent with the previously found value. Optical bursts are observed during a previously identified gap in orbital phase centred on φ = 0.967, meaning the reprocessing site is not eclipsed as previously thought. Finally, the apparent P-Cygni profiles present in some of the atomic lines in the optical spectra are due to transient absorption, which suggests the origin of the absorption is not a wind from the primary.en
dc.description.sponsorshipNaughton Foundation (Martin and Carmel Naughton Graduate Fellowship); University College Cork (Strategic Research Fund)en
dc.description.statusNot peer revieweden
dc.description.versionAccepted Version
dc.identifier.citationKennedy, M. 2017. Physics in the extreme: X-ray and optical studies of magnetic white dwarfs and related objects. PhD Thesis, University College Cork.en
dc.publisherUniversity College Corken
dc.rights© 2017, Mark Kennedy.en
dc.subjectInteracting binary starsen
dc.subjectCataclysmic variablesen
dc.titlePhysics in the extreme: X-ray and optical studies of magnetic white dwarfs and related objectsen
dc.typeDoctoral thesisen
dc.type.qualificationlevelDoctoral Degree (Structured)en
dc.type.qualificationnamePhD (Science)en
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