Superhumps and spin-period variations in the intermediate polar RX J2133.7+5107

Miguel, Enrique de; Patterson, Joseph; Jones, J. L.; Morelle, Etienne; Boyd, David; Stein, William; Koff, R. A.; Krajci, Thomas; Campbell, Tut; Roberts, George; Ulowetz, Joseph; Barrett, D.; Cejudo, D.; Menzies, Kenneth; Lemay, Damien; Rock, John; Sabo, Richard; Myers, Gordon

doi:10.1093/mnras/stx107

Cited by 5 publications

(2 citation statements)

References 21 publications

(27 reference statements)

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“…Secular spin-up, withṖ in the range ∼ 5 × 10 −13 -10 −10 s s −1 , has been detected in about ten WDs in binary systems of the intermediate polar type (see, e.g. the recent compilation in de Miguel et al 2017). These WDs have magnetic fields of about 1-20 MG and accrete from main sequence or evolved subgiant companions that are filling their Roche-lobe.…”

Section: Discussionmentioning

confidence: 99%

A young contracting white dwarf in the peculiar binary HD 49798/RX J0648.0–4418 ?

Попов

Mereghetti

Блинников

et al. 2017

Monthly Notices of the Royal Astronomical Society

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HD 49798/RX J0648.0-4418 is a peculiar X-ray binary with a hot subdwarf (sdO) mass donor. The nature of the accreting compact object is not known, but its spin period P = 13.2 s andṖ = −2.15 × 10 −15 s s −1 , prove that it can be only either a white dwarf or a neutron star. The spin-up has been very stable for more than 20 years. We demonstrate that the continuous stable spin-up of the compact companion of HD 49798 can be best explained by contraction of a young white dwarf with an age ∼ 2 Myrs. This allows us to interpret all the basic parameters of the system in the framework of an accreting white dwarf. We present examples of binary evolution which result in such systems. If correct, this is the first direct evidence for a white dwarf contraction on early evolutionary stages.

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Section: Discussionmentioning

confidence: 99%

A young contracting white dwarf in the peculiar binary HD 49798/RX J0648.0–4418 ?

Попов

Mereghetti

Блинников

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…de Miguel et al (2017) compiled published spin-up rates for intermediate polars. Among 16 objects listed there, V2306 Cyg has one of the longest orbital and spin periods.…”

Section: Discussionmentioning

confidence: 99%

Detection of white dwarf spin period variability in the intermediate polar V2306 Cygni

Breus,

Petrik,

Zola

2019

Preprint

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Magnetic cataclysmic variables are close binaries which consist of a compact objecta white dwarf -and a red dwarf filling its Roche Lobe. Such systems are physical laboratories which enable study of the influence of magnetic fields on matter flows. They often exhibit spin-up or spin-down of the white dwarf, while some systems exhibit more complex behaviour of the spin period change. We monitor changes of the spin periods of white dwarfs in a sample of close binary systems to study interaction of the magnetic field and accretion processes as well as evolution of intermediate polars. Within the framework of our intermediate polar monitoring program, we obtained photometric CCD observations at several observatories. Two-period trigonometric polynomial fitting was used for determination of extrema timings. The (O-C) analysis was performed to study the variability of the orbital and spin periods of the systems. Using data taken during 9 years of observations of the magnetic cataclysmic variable V2306 Cygni (formerly known as 1WGA J1958.2+3232), we detected the spin period variability which shows a spin-up of the white dwarf with a characteristic time of (53 ± 5) • 10 4 years. The value of the spin period was 733.33976 seconds with the formal accuracy of 0.00015 seconds. We derived an improved value of the orbital period of the system to be 4.371523 ± 0.000009 hours.

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TESS light curves of cataclysmic variables – II – Superhumps in old novae and novalike variables

Bruch

2022

Monthly Notices of the Royal Astronomical Society

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Superhumps are among the abundant variable phenomena observed in the light curves of cataclysmic variables (CVs). They come in two flavours as positive and negative superhumps, distinguished by periods slightly longer or shorter, respectively, than the orbital periods of these interacting binary systems. Positive superhumps are ubiquitous in superoutbursting short period dwarf novae of the SU UMa type but are less common in longer period systems with accretion disks in a permanent bright state such as novalike variables and most old novae. Negative superhumps do not seem not to have a preference for a particular type of CV. Here, I take advantage of the long high cadence light curves provided by TESS for huge number of stars, selecting all old novae and novalike variables with past reported superhumps for which TESS light curves are available and have not yet been analysed in previous publications in order to study their superhump behaviour. In combination with information taken from the literature the results enable to compile the most complete census of superhumps in these stars so far. As a corollary, for the eclipsing systems in the present sample of objects eclipse epochs derived from the TESS light curves and in some cases from archival light curves are listed and used to update orbital ephemeris and to discuss period changes.

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Superhumps and spin-period variations in the intermediate polar RX J2133.7+5107

Cited by 5 publications

References 21 publications

A young contracting white dwarf in the peculiar binary HD 49798/RX J0648.0–4418 ?

A young contracting white dwarf in the peculiar binary HD 49798/RX J0648.0–4418 ?

Detection of white dwarf spin period variability in the intermediate polar V2306 Cygni

TESS light curves of cataclysmic variables – II – Superhumps in old novae and novalike variables

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