Cyclic variations with twice the accretion disk precession period in the old nova V603 Aquilae

Bruch, A.; Cook, Lewis M.

doi:10.1016/j.newast.2018.02.002

Cited by 5 publications

(2 citation statements)

References 34 publications

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“…The only consistent modulation present in the light curve has a slightly variable period close to 3.5 h, about 6% longer than the orbital period. It has first been detected by Haefner (1981) and then be confirmed by many authors (see Bruch & Cook 2018). Additionally, Patterson et al (1998) observed a modulation with a period being about 3% less than the orbital period.…”

Section: Appendix B: System Parametersmentioning

confidence: 62%

A comparative study of the strength of flickering in cataclysmic variables

Bruch

2021

Preprint

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Flickering is a universal phenomenon in accreting astronomical systems which still defies detailed physical understanding. It is particularly evident in cataclysmic variables (CVs). Attempting to define boundary conditions for models, the strength of the flickering is measured in several thousand light curves of more than 100 CVs. The flickering amplitude is parameterized by the FWHM of a Gaussian fit to the magnitude distribution of data points in a light curve. This quantity requires several corrections before a comparison between different sources can be made. While no correlations of the flickering strength with simple parameters such as component masses, orbital inclination or period were detected, a dependence on the absolute magnitude of the primary component and on the CV subtype is found. In particular, flickering in VY Scl tpye novalike variables is systematically stronger than in UX UMa type novalikes. The broadband spectrum of the flickering light source can be fit by simple models but shows excess in the U band. When the data permitted to investigate the flickering strength as a function of orbital phase in eclipsing CVs, such a dependence was found, but it is different for different systems. Surprisingly, there are also indications for variations of the flickering strength with the superhump phase in novalike variables with permanent superhumps. In dwarf novae, the flickering amplitude is high during quiescence, drops quickly at an intermediate magnitude when the system enters into (or returns from) an outburst and, on average, remains constant above a given brightness threshold.

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Section: Appendix B: System Parametersmentioning

confidence: 62%

A comparative study of the strength of flickering in cataclysmic variables

Bruch

2021

Preprint

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“…It is therefore an unsolved question why positive superhumps are also occasionally observed in systems with a much higher mass ratio and a wider orbit. Prominent examples are, among others, UU Aqr (Patterson et al 2005), V603 Aql (Bruch & Cook 2018, and references therein), KR Aur (Kozhevnikov 2007), TV Col (Rette, et al 2003), V751 Cyg (Patterson et al 2001;Papadaki et al 2009), V795 Her (Patterson & Skillman 1994;Papadaki et al 2006), and V378 Peg (Kozhevnikov 2012). TT Ari another case.…”

Section: Introductionmentioning

confidence: 99%

TT Arietis: 40 yr of photometry

Bruch

2019

Monthly Notices of the Royal Astronomical Society

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In an effort to characterize variations on the time scale of hours and smaller during the high and low states of the novalike variable TT Ari, light curves taken over the course of more than 40 yr are analyzed. It is found that the well known negative superhump observed during the high state persists until the present day at an average period of 0.13295 d which is slightly variable from year to year and exhibits substantial amplitude changes. The beat period between superhump and orbital period is also seen. QPOs occur at a preferred quasi-period of 18 -25 min and undergo a systematic frequency evolution during a night. The available data permit for the first time a detailed investigation of the low state which is highly structured on time-scales of tens of days. On hourly time scales the light curve exhibits strong variations which are mostly irregular. However, during an interval of several days at the start of the low state, coherent 1.2 mag oscillations with a period of 8.90 h are seen. During the deep low state quiet phases and strong (1.5 -3 mag), highly structured flares alternate in irregular intervals of roughly 1 day. The quiet phases are modulated on the orbital period of TT Ari, suggesting reflection of the light of the primary component off the secondary. This is the first time that the orbital period is seen in photometric data.

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TESS light curves of cataclysmic variables – I – Unknown periods in long-known stars

Bruch

2022

Monthly Notices of the Royal Astronomical Society

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Cataclysmic variables (CVs) exhibit a plethora of variable phenomena many of which require long, uninterrupted light curves to reveal themselves in detail. The month long datasets provided by TESS are well suited for this purpose. TESS has the additional advantage to have observed a huge number of stars, among them many CVs. Here, a search for periodic variations in a sample of CVs of the novalike and old novae subtypes is presented. In 10 of the 15 targets either previously unseen positive or negative superhumps or unusual features in known superhumps are identified. The TESS light curves demonstrate that the occurrence of superhumps in these types of CVs is not an exception but quite common. For 8 systems new or improved values for the orbital period are measured. In TV Col the long-sought optical manifestation of the white dwarf spin period is first seen in form of its orbital sideband. The mystery of multiple photometric periods observed in CP Pup in the past is explained by irregularly occurring anomalous states which are reflected in the light curve.

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Cyclic variations with twice the accretion disk precession period in the old nova V603 Aquilae

Cited by 5 publications

References 34 publications

A comparative study of the strength of flickering in cataclysmic variables

A comparative study of the strength of flickering in cataclysmic variables

TT Arietis: 40 yr of photometry

TESS light curves of cataclysmic variables – I – Unknown periods in long-known stars

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