Novae in the SuperWASP data base

McQuillin, Rachael C.; Evans, A.; Wilson, David M.; Maxted, P. F. L.; Pollacco, D.; West, R. G.; Hounsell, R.; Bode, M. F.

doi:10.1111/j.1365-2966.2011.19695.x

Cited by 13 publications

(8 citation statements)

References 38 publications

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“…Maxted et al 2008;Thomas et al 2010;Norton et al 2011;Smalley et al 2011Smalley et al , 2014Smalley et al , 2017McQuillin et al 2012;Holdsworth et al 2014;Holdsworth 2015). In this paper, we provide an in depth analysis of three sdBV stars which have been identified to vary by Holdsworth et al (2014) and Holdsworth (2015).…”

Section: The Superwasp Projectmentioning

confidence: 99%

Three new pulsating sdB stars discovered with SuperWASP

Holdsworth

Østensen

Smalley

et al. 2017

Mon. Not. R. Astron. Soc.

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We present an analysis of three new pulsating subdwarf B stars discovered in the SuperWASP archive. Two of the stars, J1938+5609 and J0902-0720, are p-mode pulsators; J1938+5609 shows a pulsation at 231.62 d −1 (P = 373 s; 2681 µHz) with an amplitude of 4 mmag, whereas J0902-0720 pulsates at frequencies 636.74 d −1 (P = 136 s; 7370 µHz) and 615.34 d −1 (P = 140 s; 7122 µHz), with amplitudes 7.27 and 1.53 mmag, respectively. The third star, J2344-3427, is a hybrid pulsator with a p-mode frequency at 223.16 d −1 (P = 387 s; 2583µHz) and a corresponding amplitude of 1.5 mmag, and g modes in the frequency range 8.68 − 28.56 d −1 (P = 3025 − 9954 s; 100 − 331µHz) and amplitudes between 0.76 and 1.17 mmag. Spectroscopic results place J1938+5609 and J2344-3427 among the long-period or hybrid pulsators, suggesting there may be further modes in these stars below our detection limits, with J0902-0720 placed firmly amongst the p-mode pulsators.

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Section: The Superwasp Projectmentioning

confidence: 99%

Three new pulsating sdB stars discovered with SuperWASP

Holdsworth

Østensen

Smalley

et al. 2017

Mon. Not. R. Astron. Soc.

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“…Ragan et al (2009) derived a distance of ∼ 6.5 kpc to KT Eri and pointed out that the 15th magnitude star located close to the KT Eri position in pre-discovery images is too bright to be its progenitor. McQuillin et al (2012) and Hounsell et al (2010) have obtained an impressive high cadence optical light curve of KT Eri before, during and after the outburst using data from SuperWASP (Pollacco et al 2006) and the USAF/NASA Solar Mass Ejection Imager (SMEI) (Jackson et al 2005) on board the Coriolis Satellite (Eyles 2003), respectively. The SMEI observations are spread over the period 2009 November 1.13 to 30.62 UT.…”

Section: Introductionmentioning

confidence: 99%

Nova KT Eri 2009: infrared studies of a very fast and small amplitude He/N nova

Raj

Banerjee

Ashok

2013

Monthly Notices of the Royal Astronomical Society

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We present near-infrared spectroscopic and photometric observations of the nova KT Eridani taken during the first 100 days following its discovery in 2009 November. The JHK spectra of the object have been taken from the Mount Abu Infrared Observatory using the Near-Infrared Imager/Spectrometer. The spectra, typical of the He/N class novae, show strong He i emission lines together with H i and O i emission features. The H i, Pa β and Br γ spectral lines and the He i line at 2.0581 µm show broad wings with a relatively narrow central component. The broad wings extend to ∼ 1900 km s −1 while the central component has FWHM of ∼ 2100 km s −1 . The V and near-infrared JHK light curves show an additional small amplitude outburst near 40 days after optical maximum. The distance to the nova d = 6.3 ± 0.1 kpc is derived using the MMRD relation and the estimated value of t 2 = 5.7 ± 0.3 days. The small value of t 2 places KT Eri in the class of very fast novae. Using the value of the distance to the nova d, we estimate the height of the nova to be z = 3.3 ± 0.1 kpc below the galactic plane. We have also calculated the upper limit for the ejecta mass for KT Eri to be in the range 2.4 -7.4 ×10 −5 M ⊙ . Kinematic evidence is presented from the shape of the line profiles for a possible bipolar flow. We analyze the temporal evolution of the continuum and also discuss the possibility of KT Eri being a recurrent nova.

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“…The spectroscopic orbital period was measured by Thorstensen & Taylor (2000). A slightly shorter photometric period was observed by McQuillin et al (2012) in SuperWASP data. It may be related to a negative superhump.…”

Section: Appendix B: System Parametersmentioning

confidence: 99%

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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Novae in the SuperWASP data base

Cited by 13 publications

References 38 publications

Three new pulsating sdB stars discovered with SuperWASP

Three new pulsating sdB stars discovered with SuperWASP

Nova KT Eri 2009: infrared studies of a very fast and small amplitude He/N nova

A comparative study of the strength of flickering in cataclysmic variables

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