Multicolor Photometry of a Close Binary System with an X-ray Source

2019 ◽  
Vol 57 (2) ◽  
pp. 91-100
Author(s):  
A. N. Sazonov ◽  
I. N. Anakhina
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
X Ray ◽  
Multicolor Photometry

On the Possible Short-Period Irregular Light Fluctuations of V1357 CYG =CYG X-1

1982 ◽  
Vol 69 ◽  
pp. 467-472
Author(s):  
M.I. Kumsiashvili ◽  
Z. Kraicheva
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
X Ray ◽  
Light Fluctuations ◽  
Short Period ◽  
Photoelectric Observations ◽  
Fast Light

AbstractPhotoelectric observations in U, B, V, were carried out to study the possible rapid (during a night) fluctuations of the close binary system V1357 Cyg, including the X-ray source Cyg X-1. Assuming the existence of irregular fast light fluctuations in the X-ray source Cyg X-1,the conclusion can be drawn that during these observations in 1979 the amplitude of the variations did not exceed 0.04 mag.

scholarly journals Variability of Soft X-Ray Emission of Ex Hydrae Observed with Einstein Observatory

1982 ◽  
Vol 69 ◽  
pp. 457-466
Author(s):  
A. Kruszewski ◽  
R. Mewe ◽  
J. Heise ◽  
T. Chlebowski ◽  
W. van Dijk ◽  
...  
Keyword(s):  
High Resolution ◽  
Binary System ◽  
Variable Star ◽  
Close Binary System ◽  
Close Binary ◽  
Evolutionary Status ◽  
Cataclysmic Variable ◽  
X Ray ◽  
Optical Position ◽  
Einstein Observatory

The cataclysmic variable star EX Hydrae has been observed with the High Resolution Imager (HRI) and the Imaging Proportional Counter (IPC) onboard the Einstein Observatory. The X-ray position is coincident within 3 arcsec of the optical position as measured on Schmidt survey plates. During a 15 1/2 hour observation with IPC we have searched for a modulation of the X-ray flux. Strong evidence for a 67 min period (one of two known optical periods) has been found in the energy range 0.1-3.5 keV with the IPC. The time dependence of modulations is used to discuss a model and evolutionary status of this close binary system.

scholarly journals Origin of High Velocity Pulsar and Soft Gamma Ray Repeaters

1996 ◽  
Vol 160 ◽  
pp. 359-360
Author(s):  
Hitoshi Hanami
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
High Velocity ◽  
Relative Velocity ◽  
Gamma Ray ◽  
Center Of Mass ◽  
Supernova Explosion ◽  
Close Binary System ◽  
Close Binary ◽  
X Ray

AbstractWe consider a close binary system with separation ≃ 0.2 R⊙which consists of a (C+O) star of mass ≃ 4 M⊙and a neutron star as a progenitor of soft gamma-ray repeater (SGR) and a high velocity pulsar. After the event of the supernova explosion, both new and old neutron stars have high relative velocity of ≃ 1000km s−1to the center of mass of the ejecta. SGR activities can be induced by the episodic accretion of the supernova ejecta onto the old neutron star or the strange high rotating pulsar of the new neutron star. Future observations with fine positional resolution can clarify the position ambiguity between the gamma ray and X-ray sources.

scholarly journals The ROSAT view of the massive eclipsing O-type binary system 29 UW Canis Majoris

1995 ◽  
Vol 163 ◽  
pp. 382-387
Author(s):  
Thomas W. Berghöfer ◽  
Jürgen H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Stellar Winds ◽  
X Ray ◽  
Short Period

We have investigated a recently obtained ROSAT X-ray observation of the massive binary 29 UW Canis Majoris (HR 2781; HD 57060). This short-period binary (4.3934 d) consists of two eclipsing O-type stars and has been observed for about 9 days with the ROSAT PSPC. We discuss the origin of the X-ray emission in the close binary system 29 CMa in the context of the traditional colliding wind scenario as well as the scenario of X-ray emission from shock heated gas in the stellar winds.

scholarly journals X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

2018 ◽  
Vol 619 ◽  
pp. A138
Author(s):  
V. Perdelwitz ◽  
S. Czesla ◽  
J. Robrade ◽  
T. Pribulla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
Uv Light ◽  
Close Binary ◽  
Eclipsing Binary ◽  
X Ray ◽  
Uv Emission ◽  
Low Mass ◽  
Orbital Modulation

Context.Close binary systems provide an excellent tool for determining stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, postulated to be the underlying reason for radius inflation in many of the components. Aims.We extend the sample of low-mass binary systems with well-known X-ray properties. Methods.We analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve was modeled with the eclipsing binary modeling tool PHOEBE and data acquired with the EPIC cameras was analyzed to search for hints of orbital modulation. Results.We find clear evidence of orbital modulation in the UV light curve and show that PHOEBE is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on PHOENIX models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

scholarly journals Marginally low mass ratio close binary system V1191 Cyg

New Astronomy ◽  
2012 ◽  
Vol 17 (1) ◽  
pp. 46-49 ◽  
Author(s):  
B. Ulaş ◽  
B. Kalomeni ◽  
V. Keskin ◽  
O. Köse ◽  
K. Yakut
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Mass Ratio ◽  
Low Mass ◽  
Low Mass Ratio

scholarly journals Asteroseismology in action: a test of spin-orbit synchronism in the close binary system Feige 48

2008 ◽  
Vol 483 (3) ◽  
pp. 875-885 ◽  
Author(s):  
V. Van Grootel ◽  
S. Charpinet ◽  
G. Fontaine ◽  
P. Brassard
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Spin Orbit

scholarly journals V479 And: CV, LMXB, or Symbiotic?

2011 ◽  
Vol 7 (S281) ◽  
pp. 113-116
Author(s):  
Diego González Buitrago ◽  
Gagik Tovmassian ◽  
Juan Echevarría ◽  
Sergey Zharikov ◽  
Takamitsu Miyaji ◽  
...  
Keyword(s):  
Orbital Period ◽  
Main Sequence ◽  
Compact Object ◽  
Close Binary System ◽  
Close Binary ◽  
Stellar Winds ◽  
Primary Star ◽  
Giant Star ◽  
X Ray ◽  
Low Mass

AbstractV479 And is a 14.26 hour, close binary system, comprised of a G8-K0 star departing from the main sequence and a compact primary star accreting matter from the donor. The object is an X-ray source, modulated with the orbital period. This, and the presence of an intense He II line, leads us to speculate that the compact object is a magnetic white dwarf. However, we do not find strong constraints on the upper mass limit of the compact object, and we may have a neutron star in a low mass X-ray binary instead of a cataclysmic variable. The orbital period is certainly too short for the donor star to be an evolved giant star, so classifying this object as a symbiotic binary may be a big stretch; however there is an evidence that the mass transfer occurs via stellar winds, rather than through the L1 point of Roche filling secondary, a phenomenon more common for symbiotic stars.

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