Results 41 to 50 of about 493,128 (267)
Kepler Observations of V447 Lyr: An Eclipsing U Gem Cataclysmic Variable [PDF]
, 2012 We present the results of an analysis of data covering 1.5 years of the dwarf nova V447 Lyr. We detect eclipses of the accretion disk by the mass donating secondary star every 3.74 hrs which is the binary orbital period.
Alan Smale +39 more
core +3 more sources
International Astronomical Union Colloquium, 1979 AbstractExtensive photoelectric observations of EX Hya were obtained between 1962 and 1976 at different telescopes and observatories. Evaluation of the data reveals a decrease of the orbital period at the rate Ṗ = −5.2 × 10−12. This period change is likely caused by mass transfer with angular momentum exchange between orbital motion and disc rotation ...
N. Vogt, W. Krzeminski, C. Sterken
openaire +1 more source
An estimation of the white dwarf mass in the Dwarf Nova GK Persei with NuSTAR observations of two states [PDF]
, 2017 We report on X-ray observations of the Dwarf Nova GK Persei performed by {\it NuSTAR} in 2015. GK Persei, behaving also as an Intermediate Polar, exhibited a Dwarf Nova outburst in 2015 March--April.
Y. Wada +5 more
semanticscholar +1 more source
MASTER OT J030227.28+191754.5: A Dwarf Nova at a Massive Oxygen–Neon White Dwarf System?
The Astrophysical Journal, 2023 We present timing and spectral analysis results of the NICER and NuSTAR observations of the dwarf nova MASTER OT J030227.28+191754.5 during the 2021–2022 outburst.
Mariko Kimura +5 more
doaj +1 more source
Nuclear Mixing Meters for Classical Novae [PDF]
, 2013 Classical novae are caused by mass transfer episodes from a main sequence star onto a white dwarf via Roche lobe overflow. This material forms an accretion disk around the white dwarf.
Champagne, Art +4 more
core +3 more sources
Observations of Eclipsing Dwarf Novae [PDF]
International Astronomical Union Colloquium, 1987 AbstractHigh Speed Photometry of four eclipsing dwarf novae, Z Cha, OY Car, HT Cas and IP Peg, is used to determine the orbital parameters and the masses of the two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the ...
openaire +1 more source
ASASSN-16eg: New candidate for a long-period WZ Sge-type dwarf nova [PDF]
, 2017 We report on our photometric observations of the 2016 superoutburst of ASASSN-16eg. This object showed a WZ Sge-type superoutburst with prominent early superhumps with a period of 0.075478(8) d and a post-superoutburst rebrightening.
Yasuyuki Wakamatsu +21 more
semanticscholar +1 more source
Dwarf nova-type cataclysmic variable stars are significant radio emitters [PDF]
, 2016 We present 8–12 GHz radio light curves of five dwarf nova (DN) type cataclysmic variable stars (CVs) in outburst (RX And, U Gem, and Z Cam), or superoutburst (SU UMa and YZ Cnc), increasing the number of radio-detected DN by a factor of 2.
D. Coppejans +9 more
semanticscholar +1 more source
RZ Leonis Minoris bridging between ER Ursae Majoris-type dwarf nova and nova-like system [PDF]
, 2016 We observed RZ LMi, which is renowned for the extremely (~19d) short supercycle and is a member of a small, unusual class of cataclysmic variables called ER UMa-type dwarf novae, in 2013 and 2016.
Taichi Kato +66 more
semanticscholar +1 more source
The rms–flux relation in accreting white dwarfs: another nova-like variable and the first dwarf nova [PDF]
, 2015 We report on the detection of the linear rms-flux relation in two accreting white dwarf binary systems: V1504 Cyg and KIC 8751494. The rms-flux relation relates the absolute root-mean-square (rms) variability of the light curve to its mean flux.
M. Sande, S. Scaringi, C. Knigge
semanticscholar +1 more source