scholarly journals New Photometric Observations of RS Oph

2011 ◽  
Vol 7 (S281) ◽  
pp. 201-202
Author(s):  
Irina Voloshina ◽  
Vladimir Metlov
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Astronomical Institute ◽  
Long Period ◽  
Photometric Observations ◽  
Sternberg Astronomical Institute ◽  
Recurrent Nova ◽  
Type Giant ◽  
Chandrasekhar Limit

AbstractThe recurrent nova RS Oph is a long period (~455 days) binary system consisting of a hot white dwarf with mass close to the Chandrasekhar limit and an M-type giant secondary. Here we present the results of photometric observations of this nova which were made during recent years with the telescopes of the Sternberg Astronomical Institute in Crimea.

scholarly journals Period Changes and Mass Loss Rates in 34 RS CVn-Type Binaries

1980 ◽  
Vol 88 ◽  
pp. 383-387 ◽  
Author(s):  
Douglas S. Hall ◽  
Jerzy M. Kreiner ◽  
Steven N. Shore
Keyword(s):  
Light Curve ◽  
Mass Loss ◽  
Least Squares ◽  
Weighted Least Squares ◽  
Astronomical Observatory ◽  
Astronomical Institute ◽  
Long Period ◽  
Sternberg Astronomical Institute ◽  
Short Period

We have collected all available times of minimum, over 1650, for 23 regular, 7 short-period, and 4 long-period eclipsing RS CVn binaries using the card catalogues at the Sternberg Astronomical Institute and the Krakow Astronomical Observatory, as well as unpublished data. We examined them critically, discarded those grossly in error, and assigned weights. For AD Cap, RV Lib, and ε UMi there are virtually no data. For the remaining 31 we determined quadratic ephemerides by weighted least squares. Values of d1nP/dt are given in the Table with their errors. Roughly 2/3 are variable at greater than the 2 σ level. Significant decreases outnumber significant increases by almost 2:1. We show that light curve asymmetry produced by the distortion wave probably accounts for the relatively small, rapid fluctuations in the O-C curve but not the long-term period changes.

scholarly journals IP Eridani: A surprising long-period binary system hosting a He white dwarf

2014 ◽  
Vol 567 ◽  
pp. A30 ◽  
Author(s):  
T. Merle ◽  
A. Jorissen ◽  
T. Masseron ◽  
S. Van Eck ◽  
L. Siess ◽  
...  
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Long Period

scholarly journals On the 2011 Outburst of the Recurrent Nova T Pyxidis

2015 ◽  
Vol 2 (1) ◽  
pp. 264-268
Author(s):  
L. Izzo ◽  
M. Della Valle ◽  
A. Ederoclite ◽  
M. Henze
Keyword(s):  
Binary System ◽  
White Dwarf ◽  
Line Profiles ◽  
X Ray ◽  
Recurrent Nova ◽  
System Configurations

We discuss the nebular phase emission during the 2011 outburst of the recurrent nova T Pyxidis and present preliminaryresults on the analysis of the line profiles. We also present some discussions about the binary system configurations and the X-ray emission, showing that the white dwarf mass should be larger than 0.8 M<sub>Θ</sub>.

scholarly journals The Apsidal Motion of the Eclipsing Binary Systems GSC 4487 0347 and GSC 4513 2537

2011 ◽  
Vol 7 (S282) ◽  
pp. 93-94
Author(s):  
V. S. Kozyreva ◽  
A. V. Kusakin ◽  
T. Krajci ◽  
J. Menke ◽  
T. M. Tsvetkova
Keyword(s):  
Binary Systems ◽  
Variable Stars ◽  
Eclipsing Binaries ◽  
Tien Shan ◽  
Astronomical Institute ◽  
Ccd Array ◽  
Photometric Observations ◽  
Sternberg Astronomical Institute ◽  
The Crimea ◽  
Orbital Periods

AbstractThe eclipsing variable stars GSC 44870347 and GSC 4513 2537 are recently discovered binary systems (Otero et al., 2006) with orbital periods 1d.99 and 6d.33 days. We carried out the photometric observations of these eclipsing binaries from 2009-2010 using a CCD-array at the Tien-Shan Observatory in Kazakstan, at the Crimea Station of the Sternberg Astronomical Institute, at the Astrokolkhoz Observatory in New Mexico (AAVSO), while the spectrophotometric observations were obtained at the Starlight Farm Observatory in Barnesville, USA.

scholarly journals Optical Light Curve of Nova KT Eridani

2012 ◽  
Vol 8 (S290) ◽  
pp. 191-192
Author(s):  
W. P. Chen ◽  
L. W. Hung ◽  
Fred Walter
Keyword(s):  
Light Curve ◽  
White Dwarf ◽  
Hot Spot ◽  
X Ray ◽  
Optical Emissions ◽  
Optical Light Curve ◽  
Recurrent Nova ◽  
Orbital Modulation ◽  
Type Giant

AbstractWe present the optical light curve of the very fast nova, KT Eridani, from its outburst in November 2009 to quiescence in 2012. Comparison of our data with the 24-hour monitoring by Swift on 2010 March 31 indicates a possible anticorrelation between the X-ray and optical emissions. A period of 57 d is found in the long-term optical light curve, which we interpret as the orbital modulation of the hot spot on the white dwarf disk accreting material from an early K-type giant. Our study lends support to the notation that KT Eri may be a recurrent nova.

scholarly journals Hydrogen Depletion and the Evolution of Cataclysmic Variables to Low Mass X-Ray Binaries

1987 ◽  
Vol 93 ◽  
pp. 681-685
Author(s):  
R.E. Williams ◽  
M.M. Phillips ◽  
S.R. Heathcote
Keyword(s):  
Emission Line ◽  
White Dwarf ◽  
White Dwarfs ◽  
Cataclysmic Variables ◽  
Core Collapse ◽  
X Ray ◽  
Low Mass ◽  
Recurrent Nova ◽  
Chandrasekhar Limit ◽  
X Ray Binaries

AbstractCertain cataclysmic variables may evolve into low mass X-ray binaries if the white dwarfs can steadily accrete sufficient mass to exceed the Chandrasekhar limit. We present spectra of a recurrent nova and a low mass X-ray binary which are very similar to each other, and are also unusual for the strengths of the observed He II emission. We suggest that this similarity is not coincidental, but is evidence for an evolutionary link between the two classes of objects. A hydrogen depletion in the accreting gas is implied from the emission line fluxes, and may be an important parameter in determining whether accreted gas remains bound to the white dwarf, enabling eventual core collapse to occur.

scholarly journals The Strange Story of BI Lyncis: an Extremely Helium-Rich Subdwarf with a Cool Companion

2002 ◽  
Vol 187 ◽  
pp. 59-64
Author(s):  
C. Simon Jeffery ◽  
R. Aznar Cuadrado
Keyword(s):  
Binary System ◽  
Accretion Disk ◽  
White Dwarf ◽  
Strange Story ◽  
Low Mass ◽  
Type Giant ◽  
Helium Star ◽  
Highly Evolved

AbstractThe star BI Lyn = PG 0900+400 was previously classified as an evolved binary system containing either a hot subdwarf or white dwarf and a thick accretion disk. We have analyzed new intermediate dispersion spectra and demonstrated that both views are wrong. BI Lyn is a highly-evolved system containing a luminous low-mass helium star and a rapidly rotating G-type giant. It may be closely related to the evolved sdO+G binary HD 128220.

scholarly journals Modeling of the IR Light Curves of the Symbiotic Recurrent Nova T CrB

2011 ◽  
Vol 7 (S281) ◽  
pp. 203-204
Author(s):  
A. A. Tatarnikova ◽  
A. M. Tatarnikov ◽  
V. I. Shenavrin
Keyword(s):  
White Dwarf ◽  
Roche Lobe ◽  
Light Curves ◽  
Mass Ratio ◽  
Cool Component ◽  
Recurrent Nova ◽  
Photometric Monitoring ◽  
Chandrasekhar Limit ◽  
Ir Light

AbstractWe analyze the results of our IR photometric monitoring of T CrB during 1987-2003 and describe the ellipsoidal variability of the Roche lobe filling cool component. We obtain limits to the binary inclination of i ∈ [50,60] deg and binary mass ratio q ∈ [0.4,2] (90 per cent confidence). The mass of the hot component is therefore 1.3-3 M⊙. If the hot component of T CrB is a white dwarf, its mass will be near the Chandrasekhar limit.

BM Cas – a long-period eclipsing young supergiant binary system in common envelope stage

2007 ◽  
Vol 26 (4-5) ◽  
pp. 339-350 ◽  
Author(s):  
I. Pustylnik ◽  
P. Kalv ◽  
V. Harvig ◽  
T. Aas
Keyword(s):  
Binary System ◽  
Common Envelope ◽  
Long Period ◽  
Cas A

scholarly journals The symbiotic binary system RX Puppis: a possible recurrent nova with a Mira companion

1999 ◽  
Vol 305 (1) ◽  
pp. 190-210 ◽  
Author(s):  
J. Mikolajewska ◽  
E. Brandi ◽  
W. Hack ◽  
P. A. Whitelock ◽  
R. Barba ◽  
...  
Keyword(s):  
Binary System ◽  
Recurrent Nova
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