Cataclysmic Variables Observed During K2 Campaigns 0 and 1

Dai, Zhenwen; Szkody, Paula; Garnavich, P.; Kennedy, Mark

doi:10.3847/0004-6256/152/1/5

Cited by 19 publications

(45 citation statements)

References 49 publications

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“…The double-humped orbital variation at 55 minutes that has been observed in the optical (Mennickent et al 1999;Patterson et al 2003;Dai et al 2016) is also evident in the UV light curves (the middle of orbit 2 and the beginning and ends of orbits 3 and 4) and in the DFT. The amplitude of this variation is slightly less in the UV (0.3-0.4 in magnitude units) compared to 0.5 mag (Dai et al 2016) in the optical, although Mennickent et al (1999) note a large optical variation of the humps during their 11 year study. The model fitting of the UV spectrum by Pala et al (2017) determined the white dwarf has a temperature of 15,014±638 K and contributes 83% of the UV light.…”

Section: Rz Leomentioning

confidence: 78%

“…The short duration of this feature (about 3 min) could account for why it was not evident in previous reported data. Phasing and folding our data with the ephemeris in Dai et al (2016), based on the maximum of the primary orbital hump, shows the repeatability of the eclipse shape (Figure 4). However, further photometry with short exposures and over several days will be needed to confirm if this is indeed a partial eclipse and if the spin period can be detected in the optical.…”

Section: Rz Leomentioning

confidence: 84%

“…Its optical spectrum at quiescence (Szkody et al 2003) shows broad absorption surrounding doublepeaked Balmer emission lines, indicative of a high inclination, low mass transfer system. A short cadence (1 min) observation sequence by Kepler K2-1 for 82 days from 2014 May 30 to August 20 (Dai et al 2016) greatly improved the orbital period determination and showed a 0.5 mag double-humped light variation phased on this period. During the K2 observation, it also showed an unusual brightening event of about 0.6 mag that lasted almost 2 hr.…”

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 99%

“…Kepler K2 continuous short cadence 1 min observations on RZ Leo took place in 2014 from May 30 to August 20. The photometric extractions, resulting light curve, and a discussion of the observed double-humped orbital period variations are described in Dai et al (2016). In this paper, we subjected the short cadence (1 min) data set to the same period analysis procedure as for our HST data.…”

Section: Observationsmentioning

confidence: 99%

See 3 more Smart Citations

Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

Szkody¹,

Mukadam²,

Toloza³

et al. 2017

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Permanent WRAP URL:http://wrap.warwick.ac.uk/86770 Copyright and reuse:The Warwick Research Archive Portal (WRAP) makes this work by researchers of the University of Warwick available open access under the following conditions. Copyright © and all moral rights to the version of the paper presented here belong to the individual author(s) and/or other copyright owners. To the extent reasonable and practicable the material made available in WRAP has been checked for eligibility before being made available.Copies of full items can be used for personal research or study, educational, or not-for-profit purposes without prior permission or charge. Provided that the authors, title and full bibliographic details are credited, a hyperlink and/or URL is given for the original metadata page and the content is not changed in any way. Publisher's statement:Reproduced by permission of the AAS. Abstract Time-tag ultraviolet data obtained on the Hubble Space Telescope in 2013 reveal interesting variability related to the white dwarf spin in the two cataclysmic variables RZ Leo and CC Scl. RZ Leo shows a period at 220 s and its harmonic at 110 s, thus identifying it as a likely Intermediate Polar (IP). The spin signal is not visible in a short single night of ground-based data in 2016, but the shorter exposures in that data set indicate a possible partial eclipse. The much larger UV amplitude of the spin signal in the known IP CC Scl allows the spin of 389 s, previously only seen at outburst, to be visible at quiescence. Spectra created from the peaks and troughs of the spin times indicate a hotter temperature of several thousand degrees during the peak phases, with multiple components contributing to the UV light.

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Section: Rz Leomentioning

confidence: 78%

Section: Rz Leomentioning

confidence: 84%

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

See 2 more Smart Citations

Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

Szkody¹,

Mukadam²,

Toloza³

et al. 2017

Self Cite

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show abstract

“…Unlike the original mission which continuously monitored a 115 square degree field north of the Galactic plane between Cygnus and Lyra for 4 years, K2 monitors fields along the ecliptic plane, each pointing lasting ∼70-80 days (see Howell et al 2014). K2 has been used to study a wide variety of astronomical sources including exoplanets, galaxies, solar system objects, and cataclysmic variables (e.g., Dai et al 2016;Kennedy et al, 2016).…”

Section: Introductionmentioning

confidence: 99%

V729 Sgr: a long period dwarf nova showing negative superhumps during quiescence

Ramsay

Wood

Cannizzo³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We report K2 observations of the eclipsing cataclysmic variable V729 Sgr which covered nearly 80 days in duration. We find five short outbursts and two long outbursts, one of which shows a clear plateau phase in the rise to maximum brightness. The mean time between successive short outbursts is ∼10 d while the time between the two long outbursts is ∼38 d. The frequency of these outbursts are unprecedented for a CV above the orbital period gap. We find evidence that the mid-point of the eclipse occurs systematically earlier in outburst than in quiescence. During five of the six quiescent epochs we find evidence for a second photometric period which is roughly 5 percent shorter than the 4.16 h orbital period which we attribute to negative superhumps. V729 Sgr is therefore one of the longest period CVs to show negative superhumps during quiescence.

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The vast potential of exoplanet satellites for high‐energy astrophysics

Smith

2019

Astron Nachr

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The photometric precision, monitoring baselines, and rapid, even sampling rates required by modern satellites designed for detecting the signal of transiting exoplanets are ideally suited to a large number of applications in high-energy astrophysics. I will exemplify this by discussing the results for active galactic nuclei from Kepler and summarizing other high-energy results from Kepler/K2. These precision instruments are currently underutilized for high-energy applications despite their great potential, due in part to complex systematics affecting the data. I will summarize these effects and mitigation approaches, and conclude by discussing how the recently launched Transiting Exoplanet Survey Satellite mission will differ from Kepler/K2 in ways significant to the high-energy community.

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Cataclysmic Variables Observed During K2 Campaigns 0 and 1

Cited by 19 publications

References 49 publications

Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

V729 Sgr: a long period dwarf nova showing negative superhumps during quiescence

The vast potential of exoplanet satellites for high‐energy astrophysics

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