[PDF] Top 20 Nova-like cataclysmic variables in the infrared

... The total system model (thick solid line) is composed of a WD (dotted line), M2.6 secondary star (short dashed line; semi-empirical template from Knigge et al. 2011 with additional IR po[r] ... See full document

... four nova-like variables, compared to a total of 55 detections in all classes of ...the nova-like variables, the lack of secondary star detections is probably the result of the ... See full document

... four nova-like variables, compared to a total of 55 detections in all classes of ...the nova-like variables, the lack of secondary star detections is probably the result of the ... See full document

... on nova-like variables, whilst our IPHAS search covered all CVs in the IPHAS ...24 nova-like variables we ...a nova eruption approximately 120 yr ...by ... See full document

... Thus, th e m ajority of sta rs in th e sam ple a re not a se p ara te halo population of CV. However, th e two sta rs w ith th e larg est z estim ates, DO Leo w ith z >740 an d RU LMi w ith z >1019, a re sufficiently fa ... See full document

... e Department of Physics, University of Warwick, Coventry, UK f Center for Plasma Astrophysics, University of Leuven, Belgium Abstract NSV 1907, formerly listed as an irregular variable in variability catalogues, was ... See full document

... Two additional emission sources can explain this infrared excess: the accretion disc and/or a brown dwarf secondary star. The isothermal and isobaric hydrogen slab we included in the fit procedure is a good model ... See full document

... Dwarf Nova Classification Non-magnetic cataclysmic variables are divided into several sub-classes due to the differing properties they ...novae. Nova outbursts are caused by the ignition of ... See full document

... 5. survivors of a common-envelope phase during which they existed within the atmosphere of a giant star, and 6. exposed to nova outbursts every ∼ 10 4 yr. In order to study the impact of some of these ... See full document

... the infrared bright spot is not aligned with its optical counterpart, but is located further downstream from the stream impact region, consistent with our results for VY ... See full document

... The term DQ Her star is often used for IPs of rapid rotation, typically ∼ <250 s, but some use the term in place of IP, treating DQ Her as the type star. Where disks exist there are two principal behaviours, resulting ... See full document

... magnetic cataclysmic variables (CVs) based upon synthetic spectral analyses of far ultraviolet ...recurrent nova T Pyxidis as it transitioned into quiescence following its April 2011 nova ... See full document

... The MEG data (Fig.6) reveal a rich emission-line spectrum, comparable to that of EX Hya observed with the ASCA SIS. Lines are detected from H- and He-like ions of O, Ne, Mg, Si, S, and probably Ar. Moreover, the ... See full document

... Results. All our systems show CO abundances that are within the range observed for single stars. The weakest 12 CO bands with re- spect to the spectral type are found in the pre-CV BPM 71214, although on a much smaller ... See full document

... The origin of a nova eruption is at the boundary between the degenerate core of the white dwarf and the newly accreted, hydrogen-rich surface layer. The high gravity of the white dwarf, coupled with a substantial ... See full document

... The white dwarfs in our sample show a strong ten- dency towards high masses. We show that this is unlikely to be due to selection effects, and instead is probably a real property of the short period SDSS CVs. The ... See full document

... 4.2. ANALYSIS OF T PYX 4.2.4 A R ADIAL -V ELOCITY S TUDY OF T P YX The Systemic Velocity We noticed early on in our analysis for both the VLT and Magellan data sets that the systemic velocity, γ, appeared to be varying ... See full document

... light curves in the bottom panel of Figure 8 demonstrate this. In addition to this, we also observed an apparent complete switch-off of accretion on 2015-06-24. This eclipse, the bottom light curve shown in the bottom ... See full document

... 5.1.3 Dependence on CV Type In order to examine whether Hα selection favours particu- lar CV sub-types, each system in our samples is assigned one of four basic types based on their classification in CV- Cat shown in ... See full document

... 2 https://www.ztf.caltech.edu/page/dr1 the fields toward the Galactic Bulge and the Magellanic Clouds ( Mr´oz et al. 2015 ) and the All Sky Automated Survey (ASAS) which had large pixels and a faint limit of only 14 mag ... See full document