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TOPIC: CC Sculptoris

Blobrana

L

Posts: 131433

Date: Feb 15 11:17 2017

RX J2315.5-3049	Permalink

Title: Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis Author: Paula Szkody, Anjum S. Mukadam, Odette Toloza, Boris T. Gänsicke, Zhibin Dai, Anna F. Pala, Elizabeth O. Waagen, Patrick Godon, Edward M. Sion 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 220s and its harmonic at 110s, 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 dataset indicate a possible partial eclipse. The much larger UV amplitude of the spin signal in the known IP CC Scl allows the spin of 389s, 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. Read more (956kb, PDF) __________________

Blobrana

L

Posts: 131433

Date: Sep 30 02:41 2014

CC Sculptoris	Permalink

Title: CC Sculptoris: Eclipsing SU UMa-Type Intermediate Polar Author: Taichi Kato (Kyoto U), Franz-Josef Hambsch (GEOS, BAV, VVS), Arto Oksanen (Nyrola Obs.), Peter Starr (Warrumbungle Obs.), Arne Henden (AAVSO) We observed the 2014 superoutburst of the SU UMa-type intermediate polar CC Scl. We detected superhumps with a mean period of 0.05998(2) d during the superoutburst plateau and during three nights after the fading. During the post-superoutburst stage after three nights, a stable superhump period of 0.059523(6) d was detected. We found that this object is an eclipsing system with an orbital period of 0.058567233(8) d. By assuming that the disk radius in the post-superoutburst phase is similar to those in other SU UMa-type dwarf novae, we obtained a mass ratio of q=0.072(3) from the dynamical precession rate of the accretion disk. The eclipse profile during outbursts can be modelled by an inclination of 80.6±0.5 deg. The 2014 superoutburst was preceded by a precursor outburst and the overall appearance of the outburst was similar to superoutbursts in ordinary SU UMa-type dwarf novae. We showed that the standard thermal-tidal instability model can explain the outburst behavior in this system and suggest that inner truncation of the disk by magnetism of the white dwarf does not strongly affect the behavior in the outer part of the disk. Read more (194kb, PDF) __________________

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