Results 31 to 40 of about 493,128 (267)
The remarkable outburst of the highly evolved post- period- minimum dwarf nova SSS J122221.7-311525 [PDF]
, 2017 We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7−311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d
V. Neustroev +24 more
semanticscholar +1 more source
Temperatture esttiimattiion off EXDRA and SSUMI dwarff Nova systtems from spectroscopic data
Iraqi Journal of Physics, 2019 The seasonal behavior of the light curve for selected star SS UMI and EXDRA during outburst cycle is studied. This behavior describes maximum temperature of outburst in dwarf nova.
Arshed Ali Kadhem
doaj +1 more source
Dwarf nova outbursts in intermediate polars [PDF]
, 2017 The disc instability model (DIM) has been very successful in explaining the dwarf nova outbursts observed in cataclysmic variables. When, as in intermediate polars (IP), the accreting white dwarf is magnetized, the disc is truncated at the magnetospheric
J. Hameury, J. Lasota
semanticscholar +1 more source
Cyclic Period Oscillation of the Eclipsing Dwarf Nova DV UMa [PDF]
, 2017 DV UMa is an eclipsing dwarf nova with an orbital period of ∼2.06 hr, which lies just at the bottom edge of the period gap. To detect its orbital period changes, we present 12 new mid-eclipse times by using our CCD photometric data and archival data. The
Z.-T. Han, S. Qian, V. Irina, L.-Y. Zhu
semanticscholar +1 more source
Open Astronomy, 2012 We have analyzed the optical light curve of the symbiotic star V407 Cyg that underwent a classical nova outburst in 2010 March. Being guided by a supersoft X-ray phase observed during days 20-40 after the nova outburst, we are able to reproduce the light
Hachisu I., Kato M.
doaj +1 more source
Multicolor photometry of the classical nova V446 Her in "QUIESCENCE"
Odessa Astronomical Publications, 2017 We present the result of 2-year observations of Nova Her 1960 = V446 Her in 2002 - 2003. Data obtained in VRI spectral bands display the dwarf- nova-like outbursts with amplitude ~ 1m - 1.8m and typical time of 14 days.
E. P. Pavlenko +4 more
doaj +1 more source
Hystereses in dwarf nova outbursts and low-mass X-ray binaries [PDF]
, 2017 Context. The disc instability model (DIM) successfully explains why many accreting compact binary systems exhibit outbursts, during which their luminosity increases by orders of magnitude.
J. Hameury +3 more
semanticscholar +1 more source
Radiation from dwarf nova discs
Physics Reports, 1999 We use the Shaviv and Wehrse (1991) code to model the vertical structure and the emission properties of quiescent dwarf nova discs. We find that in the case of HT Cas the quiescent disc must be optically thin, in contradiction with the requirements of the standard disc instability model. We find a viscosity parameter alpha > 1. Although this is much
Idan, Irit +3 more
openaire +2 more sources
Roche tomography of cataclysmic variables – VIII. The irradiated and spotted dwarf nova, SS Cygni [PDF]
, 2017 We present the results of our spectroscopic study of the dwarf nova SS Cygni, using Roche tomography to map the stellar surface and derive the system parameters.
C. Hill +4 more
semanticscholar +1 more source
OGLE-BLG504.12.201843: a possible extreme dwarf nova
Monthly Notices of the Royal Astronomical Society, 2022 ABSTRACT We present the analysis of existing optical photometry and new optical spectroscopy of the candidate cataclysmic variable star OGLE-BLG504.12.201843. As was shown previously, this object has an orbital period of 0.523419 d and exhibits year-long outbursts with a mean period of 973 d.
Camille Landri +7 more
openaire +3 more sources