1984

DOI: 10.1086/162156

|View full text |Cite

|

Sign up to set email alerts

|

Ultraviolet photometry from the Orbiting Astronomical Observatory. XXXIX - The structure of the eclipsing Wolf-Rayet binary V444 Cygni as derived from light curves between 2460 A and 3. 5 microns

A. M. Cherepashchuk¹,

Kh. F. Khaliullin²,

Help me understand this report

Search citation statements

Order By: Relevance

Paper Sections

Select...

Xmm-newton and Swift Light Curves1

Cause Of the Light Variations Of Hd 1642701

Eclipsing Binary Stars From Space1

Wolf-rayet Stars1

Citation Types

Supporting

4

Mentioning

43

Contrasting

1

Unclassified

2

Year Published

1986

1986

2014

2014

Publication Types

Select...

Article6

Book4

Relationship

Self Cite0

Independent10

Authors

Journals

Cited by 120 publications

(50 citation statements)

References 0 publications

Supporting

4

Mentioning

43

Contrasting

1

Unclassified

2

Order By: Relevance

“…4.1 for the implications of this scenario). Additionally the broad and deep (but nonzero) primary eclipse suggests that the WN star appears larger than what is suggested by visual and ultraviolet light curve analysis (Cherepashchuk et al 1984;St-Louis et al 1993). The dense wind of the WN star gives rise to a wind eclipse that is broader than the eclipse created by the stellar surface alone.…”

Section: Xmm-newton and Swift Light Curvesmentioning

confidence: 84%

V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

¹

,

²

,

³

et al. 2014

View full text Add to dashboard Cite

We present results from a study of the eclipsing, colliding-wind binary V444 Cyg that uses a combination of X-ray and optical spectropolarimetric methods to describe the 3D nature of the shock and wind structure within the system. We have created the most complete X-ray light curve of V444 Cyg to date using 40 ks of new data from Swift, and 200 ks of new and archived XMM-Newton observations. In addition, we have characterized the intrinsic, polarimetric phase-dependent behavior of the strongest optical emission lines using data obtained with the University of Wisconsin's Half-Wave Spectropolarimeter. We have detected evidence of the Coriolis distortion of the wind-wind collision in the X-ray regime, which manifests itself through asymmetric behavior around the eclipses in the system's X-ray light curves. The large opening angle of the X-ray emitting region, as well as its location (i.e. the WN wind does not collide with the O star, but rather its wind) are evidence of radiative braking/inhibition occurring within the system. Additionally, the polarimetric results show evidence of the cavity the wind-wind collision region carves out of the Wolf-Rayet star's wind.

“…4.1 for the implications of this scenario). Additionally the broad and deep (but nonzero) primary eclipse suggests that the WN star appears larger than what is suggested by visual and ultraviolet light curve analysis (Cherepashchuk et al 1984;St-Louis et al 1993). The dense wind of the WN star gives rise to a wind eclipse that is broader than the eclipse created by the stellar surface alone.…”

Section: Xmm-newton and Swift Light Curvesmentioning

confidence: 84%

V444 Cygni X-ray and polarimetric variability: Radiative and Coriolis forces shape the wind collision region

¹

,

²

,

³

et al. 2014

View full text Add to dashboard Cite

We present results from a study of the eclipsing, colliding-wind binary V444 Cyg that uses a combination of X-ray and optical spectropolarimetric methods to describe the 3D nature of the shock and wind structure within the system. We have created the most complete X-ray light curve of V444 Cyg to date using 40 ks of new data from Swift, and 200 ks of new and archived XMM-Newton observations. In addition, we have characterized the intrinsic, polarimetric phase-dependent behavior of the strongest optical emission lines using data obtained with the University of Wisconsin's Half-Wave Spectropolarimeter. We have detected evidence of the Coriolis distortion of the wind-wind collision in the X-ray regime, which manifests itself through asymmetric behavior around the eclipses in the system's X-ray light curves. The large opening angle of the X-ray emitting region, as well as its location (i.e. the WN wind does not collide with the O star, but rather its wind) are evidence of radiative braking/inhibition occurring within the system. Additionally, the polarimetric results show evidence of the cavity the wind-wind collision region carves out of the Wolf-Rayet star's wind.

“…To match the observed ~ 1T2 eclipse would require y -0.55, i.e., R wr -1 R 0 . This is to be compared with the estimated core radii of WR stars, which lie in the range ~ 2-10 R 0 (Rublev 1975;Leung, Moffat, and Seggewiss 1983;Cherepashchuk, Eaton, and Khaliullin 1984;Pauldrach et al 1985).…”

Section: Cause Of the Light Variations Of Hd 164270mentioning

confidence: 99%

The variable WC9 star HD 164270 revisited - A close binary with a precessing disk?

1986

View full text Add to dashboard Cite

Five independent sets of photometric data now support the cyclic variability claimed for this cool, carbon-sequence Wolf-Rayet star. With a period of 1.75404 days, the continuum intensity varies in a double wave per cycle with an amplitude of ~ 0™03 in the visible, and a tendency to increase at shorter wavelengths. As noted previously, the emission-line radial velocities tend to show a single wave per cycle, whose low amplitude is compatible with the presence of a neutron-star (NS) companion. The recently announced deep, broad, eclipse-like variations with a possible period of tens of years may be caused by a precessing disk associated with the WR-NS system. If so, an unseen third body of moderate mass must be invoked as the motor for this precession. The alternative possibility of nonradial pulsations to explain the photometric and spectroscopic variations cannot be excluded.

“…Cherepashchuk et al, 1984;Kondo et al, 1994). The Hipparcos astrometry mission obtained photometry at several hundred epochs for many bright stars, discovering 343 new eclipsing binary systems (Perryman et al, 1997).…”

Section: Eclipsing Binary Stars From Spacementioning

confidence: 99%

Space-Based Photometry of Eclipsing Binaries

2011

View full text Add to dashboard Cite

Abstract. I briefly review the history and prospects for the study of eclipsing binary star systems from space-based observatories. The benefits of shifting to space satellites lie in the high precision and cadence achievable, as well as the ability to access wavelength regions which are unattainable from the ground. Whilst small amounts of data on eclipsing binaries were obtained by the Voyager, IUE, OAO-II, Hipparcos and MOST, the more recent CoRoT and Kepler missions were the first to provide extensive data on large numbers of systems. The future holds the prospect of the PLATO satellite, which will go bigger, better and brighter.

scite is a Brooklyn-based organization that helps researchers better discover and understand research articles through Smart Citations–citations that display the context of the citation and describe whether the article provides supporting or contrasting evidence. scite is used by students and researchers from around the world and is funded in part by the National Science Foundation and the National Institute on Drug Abuse of the National Institutes of Health.

Contact Info

hi@scite.ai

10624 S. Eastern Ave., Ste. A-614

Henderson, NV 89052, USA

Product

Browser Extension Assistant by scite Citation Statement Search Reference Check Visualizations Dashboards Explore Journals Explore Organizations Explore Funders Embedding Badge Embedding Citation Search Pricing

Resources

Blog Help & FAQ Accessibility Statement API Terms For Universities & Governments For Researchers For Publishers For Corporate, Pharma & Enterprise Author Marketing Become an Affiliate Get an organization trial or quote scite Data & Services

About

News & Press Careers Read our Paper Coverage

Blog Terms and Conditions API Terms Privacy Policy Contact Cookie Preferences Do Not Sell or Share My Personal Information

Copyright © 2024 scite LLC. All rights reserved.

Made with 💙 for researchers

Part of the Research Solutions Family.