CC Sculptoris: a superhumping intermediate polar

Woudt, P. A.; Warner, Brian D.; Gulbis, A. A. S.; Coppejans, Rocco; Hambsch, F. J.; Beardmore, A. P.; Evans, P. A.; Osborne, J. P.; Page, K. L.; Wynn, G. A.; Heyden, K. van der

doi:10.1111/j.1365-2966.2012.22010.x

Cited by 21 publications

(35 citation statements)

References 42 publications

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“…In contrast to RZ Leo, the UV light curve of CC Scl ( Figure 5 top) is completely dominated by the spin modulation of the white dwarf and its harmonic that Woudt et al (2012) only saw during the 2011 November outburst. The DFT (Figure 5, bottom) shows the harmonic of the spin at 194.6 s with a much higher amplitude (220 mma) than the spin period of 389 s (90 mma).…”

Section: Sclmentioning

confidence: 94%

“…Longa-Pena et al (2015) confirmed this low value of q from spectroscopy and suggested that CC Scl was a post-period bounce system. Observations with Swift along with ground-based photometry obtained during an outburst in 2011 (Woudt et al 2012) revealed a white dwarf spin period of 389.5 s which was only visible during the outburst. The presence of this spin period identified CC Scl as a member of the intermediate polar (IP) group, 9 systems containing magnetic white dwarfs whose spins are not synchronized with their orbits; see Warner (1995) for a review of IPs.…”

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 98%

“…Follow-up observations revealed spectra with strong Balmer and He II lines, short duration (9 day) outbursts with superhumps, and an orbital period of 1.40 hr (Chen et al 2001;Ishioka et al 2001;Woudt et al 2012). Kato et al (2015) later used shallow eclipses to determine an inclination of 81 deg, and refine the period to 84.337 minutes.…”

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 99%

“…The spin periods of white dwarfs are very stable over time and usually show up in X-ray observations. A few IPs (e.g., CC Scl, V455 And) show both the spin and the harmonic of the spin period, with the harmonic stronger than the rotation period at times (Woudt et al 2012;Mukadam et al 2016). Reis et al (2013) reported Swift-XRT data and modeling of RZ Leo, determining a 0.5-10 keV luminosity of 7.4±0.4×10 29  erg s −1 , (10 times the luminosity of V455 And).…”

Section: Rz Leomentioning

confidence: 99%

“…Our UV data show that the spin modulation is clearly present at quiescence. Since the Woudt et al (2012) observations were accomplished using the Swift UVOT with a filter centered at 2246Å, it is possible that the variability at longer UV wavelengths has lower amplitude due to the high temperature of the accreting areas. Pala et al (2017) determined a white dwarf temperature of 16,855±801 K for CC Scl from the average spectrum, but note that the white dwarf only contributes about 35% of the total UV flux (using a power law or constant flux additon for the remainder) and so the temperature is not very reliable.…”

Section: Sclmentioning

confidence: 99%

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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: Sclmentioning

confidence: 94%

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 98%

Section: Hubble Space Telescope Ultraviolet Light Curves Reveal Intermentioning

confidence: 99%

Section: Rz Leomentioning

confidence: 99%

Section: Sclmentioning

confidence: 99%

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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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Magnetic White Dwarfs

Ferrario¹,

Martino²,

Gänsicke³

2016

The Strongest Magnetic Fields in the Universe

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Magnetic White Dwarfs

2015

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In this paper we review the current status of research on the observational and theoretical characteristics of isolated and binary magnetic white dwarfs (MWDs). Magnetic fields of isolated MWDs are observed to lie in the range 10^3-10^9G. While the upper limit cutoff appears to be real, the lower limit is more difficult to investigate. The incidence of magnetism below a few 10^3G still needs to be established by sensitive spectropolarimetric surveys conducted on 8m class telescopes. Highly magnetic WDs tend to exhibit a complex and non-dipolar field structure with some objects showing the presence of higher order multipoles. There is no evidence that fields of highly magnetic WDs decay over time, which is consistent with the estimated Ohmic decay times scales of ~10^11 yrs. MWDs, as a class, also appear to be more massive than their weakly or non-magnetic counterparts. MWDs are also found in binary systems where they accrete matter from a low-mass donor star. These binaries, called magnetic Cataclysmic Variables (MCVs) and comprise about 20-25\% of all known CVs. Zeeman and cyclotron spectroscopy of MCVs have revealed the presence of fields in the range $\sim 7-230$\,MG. Complex field geometries have been inferred in the high field MCVs (the polars) whilst magnetic field strength and structure in the lower field group (intermediate polars, IPs) are much harder to establish. The origin of fields in MWDs is still being debated. While the fossil field hypothesis remains an attractive possibility, field generation within the common envelope of a binary system has been gaining momentum, since it would explain the absence of MWDs paired with non-degenerate companions and also the lack of relatively wide pre-MCVs.Comment: 73 pages, 22 figures, 2 large tables. Invited review chapter on Magnetic White Dwarfs to appear in Space Science Reviews, Springe

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CC Sculptoris: a superhumping intermediate polar

Cited by 21 publications

References 42 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

Magnetic White Dwarfs

Magnetic White Dwarfs

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