2017/02/14 by Paula Szkody, Anjum S. Mukadam, Odette Toloza +9 · 1 citation
Physics and Astronomy · #Amplitude #Astronomical spectroscopy #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Eclipse #Gamma-ray bursts and supernovae #Hubble space telescope #Light curve #Optics #Optoelectronics #Physics #Polar #Spectral line #Spin (aerodynamics) #Stars #Stellar, planetary, and galactic studies #Telescope #Ultraviolet #Ultraviolet astronomy #Ultraviolet light #White dwarf #White light #astro-ph.SR
paper · pdf · doi:10.3847/1538-3881/aa5c88
7 figures, 1 table Accepted for AJ
arxiv created 2017/02/14 · openalex publication_date 2017/02/21 · openalex created_date 2017/03/03 · arxiv updated 2017/12/08 · openalex updated_date 2026/08/06
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.