J/A+A/549/A77  SDSS J080434.20+510349.2 spectra and photometry (Zharikov+, 2013)

The accretion disk in the post period-minimum cataclysmic variable SDSS J080434.20+510349.2. Zharikov S., Tovmassian G., Aviles A., Michel R., Gonzalez-Buitrago D., Garcia-Diaz M.T. <Astron. Astrophys. 549, A77 (2013)> =2013A&A...549A..77Z 2013A&A...549A..77Z
ADC_Keywords: Binaries, cataclysmic ; Photometry ; Spectroscopy Keywords: novae, cataclysmic variables - stars: dwarf novae - stars: individual: SDSS J080434.20+510349.2 Abstract: This study of SDSS J080434.20+510349.2 (SDSS0804) is primarily concerned with the double-hump shape in the light curve and its connection with the accretion disk in this bounce-back system. Time-resolved photometric and spectroscopic observations were obtained to analyze the behavior of the system between superoutbursts. A qualitative geometric model of a binary system containing a disk with two outer annuli spiral density waves was applied to explain the light curve and the Doppler tomography. Observations were carried out during 2008-2009, after the object's magnitude decreased to V∼17.7±0.1 from the March 2006 eruption. The light curve clearly shows a sinusoid-like variability with a 0.07mag amplitude and a 42.48min periodicity, which is half of the orbital period of the system. In September 2010, the system underwent yet another superoutburst and returned to its quiescent level by the beginning of 2012. This light curve once again showed a double-hump-shape, but with a significantly smaller (∼0.01mag) amplitude. Other types of variability like a "mini-outburst" or SDSS1238-like features were not detected. Doppler tomograms, obtained from spectroscopic data during the same period of time, show a large accretion disk with uneven brightness, implying the presence of spiral waves. We constructed a geometric model of a bounce-back system containing two spiral density waves in the outer annuli of the disk to reproduce the observed light curves. The Doppler tomograms and the double-hump-shape light curves in quiescence can be explained by a model system containing a massive ≥0.7M white dwarf with a surface temperature of ∼12000K, a late-type brown dwarf, and an accretion disk with two outer annuli spirals. According to this model, the accretion disk should be large, extending to the 2:1 resonance radius, and cool ∼2500K. The inner parts of the disk should be optically thin in the continuum or totally void. Description: Photometry of SDSS J080434.20+510349.2 in V band obtained during 2008-2012. Flux-calibrated time-average spectra of SDSS J080434.20+510349.2 (Fig.5) Objects: ------------------------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------------------------- 08 04 34.20 +51 03 49.2 SDSS J080434.20+510349.2 = V* EZ Lyn ------------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file phot.dat 19 5711 Photometry of SDSS0804 sp-2004.dat 19 3860 The spectrum of SDSS0804 from SDSS obtained in 2004 sp-01-09.dat 19 1025 The spectrum of SDSS0804 obtained in Jan. 2009 sp-01-12.dat 19 2058 The spectrum of SDSS0804 obtained in Jan. 2012 sp-02-08.dat 19 1034 The spectrum of SDSS0804 obtained in March 2008 sp-03-08.dat 19 1026 The spectrum of SDSS0804 obtained in Feb. 2008 fits/* . 6 FITS version of the tables -------------------------------------------------------------------------------- Byte-by-byte Description of file: phot.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 2- 12 F11.6 d HJD [502/1959] Heliocentric Julian date (HJD-2454000) 14- 19 F6.3 mag Vmag V magnitude -------------------------------------------------------------------------------- Byte-by-byte Description of file: sp*.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 3- 6 I4 0.1nm lambda [3740/9230] Wavelength λ 8- 19 E12.6 cW/m2/nm Flux Flux (in erg/s/cm2/Å) -------------------------------------------------------------------------------- Acknowledgements: Sergey Zharikov, zhar(at)astrosen.unam.mx
(End) S. Zharikov [OAN SPM, IA UNAM, Mexico], P. Vannier [CDS] 17-Dec-2012
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