The Large Magellanic Cloud Eclipsing Binary HV 2274: Fundamental Properties and Comparison with Evolutionary Models

2000 ◽  
Vol 528 (2) ◽  
pp. 692-701 ◽  
Author(s):  
Ignasi Ribas ◽  
Edward F. Guinan ◽  
Edward L. Fitzpatrick ◽  
Laurence E. DeWarf ◽  
Frank P. Maloney ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Evolutionary Models ◽  
Eclipsing Binary ◽  
Fundamental Properties

Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

2003 ◽  
Vol 587 (2) ◽  
pp. 685-700 ◽  
Author(s):  
E. L. Fitzpatrick ◽  
I. Ribas ◽  
E. F. Guinan ◽  
F. P. Maloney ◽  
A. Claret
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Fundamental Properties

scholarly journals The multiple system Sk-67°18 in the LMC

1995 ◽  
Vol 163 ◽  
pp. 251-253 ◽  
Author(s):  
V. S. Niemela ◽  
W. Seggewiss ◽  
A. F. J. Moffat
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Spectral Type ◽  
Orbital Period ◽  
Large Magellanic Cloud ◽  
Primary Component ◽  
Magellanic Cloud ◽  
Bright Star ◽  
High Mass ◽  
Eclipsing Binary

The bright star Sk—67°18 (Brey 5) in the Large Magellanic Cloud (LMC) contains an eclipsing binary system. Our radial velocity study reveals that the orbital period is almost exactly two days. The spectra also show that the star's primary component is not of spectral type WN, but that the star is rather an Of+O type binary where the primary is probably of type O3f*. Furthermore, Sk—67°18 appears to be a high-mass multiple system.

scholarly journals THE DISTANCE TO THE MASSIVE ECLIPSING BINARY LMC-SC1-105 IN THE LARGE MAGELLANIC CLOUD

2011 ◽  
Vol 729 (1) ◽  
pp. L9 ◽  
Author(s):  
Alceste Z. Bonanos ◽  
Norberto Castro ◽  
Lucas M. Macri ◽  
Rolf-Peter Kudritzki
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binary

scholarly journals Fundamental Properties and Distances of the Large Magellanic Cloud from Eclipsing Binaries. II. HV 982

2002 ◽  
Vol 564 (1) ◽  
pp. 260-273 ◽  
Author(s):  
E. L. Fitzpatrick ◽  
I. Ribas ◽  
E. F. Guinan ◽  
L. E. DeWarf ◽  
F. P. Maloney ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Fundamental Properties

scholarly journals An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent

Nature ◽  
2013 ◽  
Vol 495 (7439) ◽  
pp. 76-79 ◽  
Author(s):  
G. Pietrzyński ◽  
D. Graczyk ◽  
W. Gieren ◽  
I. B. Thompson ◽  
B. Pilecki ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binary

scholarly journals The Physical Parameters of Four WC-type Wolf–Rayet Stars in the Large Magellanic Cloud: Evidence of Evolution*

2022 ◽  
Vol 924 (2) ◽  
pp. 44
Author(s):  
Erin Aadland ◽  
Philip Massey ◽  
D. John Hillier ◽  
Nidia Morrell
Keyword(s):  
Spectral Synthesis ◽  
Mass Loss Rate ◽  
Large Magellanic Cloud ◽  
Stellar Atmosphere ◽  
Magellanic Cloud ◽  
Physical Parameters ◽  
Evolutionary Models ◽  
Single Star ◽  
Oxygen Abundance ◽  
Solar Metallicity

Abstract We present a spectral analysis of four Large Magellanic Cloud (LMC) WC-type Wolf–Rayet (WR) stars (BAT99-8, BAT99-9, BAT99-11, and BAT99-52) to shed light on two evolutionary questions surrounding massive stars. The first is: are WO-type WR stars more oxygen enriched than WC-type stars, indicating further chemical evolution, or are the strong high-excitation oxygen lines in WO-type stars an indication of higher temperatures. This study will act as a baseline for answering the question of where WO-type stars fall in WR evolution. Each star’s spectrum, extending from 1100 to 25000 Å, was modeled using cmfgen to determine the star’s physical properties such as luminosity, mass-loss rate, and chemical abundances. The oxygen abundance is a key evolutionary diagnostic, and with higher resolution data and an improved stellar atmosphere code, we found the oxygen abundance to be up to a factor of 5 lower than that of previous studies. The second evolutionary question revolves around the formation of WR stars: do they evolve by themselves or is a close companion star necessary for their formation? Using our derived physical parameters, we compared our results to the Geneva single-star evolutionary models and the Binary Population and Spectral Synthesis (BPASS) binary evolutionary models. We found that both the Geneva solar-metallicity models and BPASS LMC-metallicity models are in agreement with the four WC-type stars, while the Geneva LMC-metallicity models are not. Therefore, these four WC4 stars could have been formed either via binary or single-star evolution.

scholarly journals THE ECLIPSING BINARY CEPHEID OGLE-LMC-CEP-0227 IN THE LARGE MAGELLANIC CLOUD: PULSATION MODELING OF LIGHT AND RADIAL VELOCITY CURVES

2013 ◽  
Vol 768 (1) ◽  
pp. L6 ◽  
Author(s):  
M. Marconi ◽  
R. Molinaro ◽  
G. Bono ◽  
G. Pietrzyński ◽  
W. Gieren ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binary

scholarly journals A precise and accurate distance to the Large Magellanic Cloud from late-type eclipsing-binary systems

2012 ◽  
Vol 8 (S289) ◽  
pp. 169-172
Author(s):  
G. Pietrzyński ◽  
W. Gieren ◽  
D. Graczyk ◽  
I. Thompson ◽  
B. Pilecki ◽  
...  
Keyword(s):  
Binary Systems ◽  
Zero Point ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Distance Scale ◽  
Late Type ◽  
Eclipsing Binary ◽  
Extragalactic Distance Scale

AbstractWe present a precise and accurate measurement of the distance to the Large Magellanic Cloud based on late-type eclipsing-binary systems. Our results provide curently the most accurate zero point for the extragalactic distance scale.

scholarly journals CCD Photometry of the Eclipsing Binary HV 2274 in the Large Magellanic Cloud

1992 ◽  
Vol 151 ◽  
pp. 509-513
Author(s):  
R.D. Watson ◽  
S.R.D. West ◽  
William Tobin ◽  
A.C. Gilmore
Keyword(s):  
New Zealand ◽  
Orbital Period ◽  
Large Magellanic Cloud ◽  
Current Data ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Eccentric Orbit ◽  
Ccd Photometry ◽  
Eclipsing Binary ◽  
Data Points

B, V and Ic photometry of the eclipsing binary HV 2274, located in the LMC, was obtained with the CCD system at the Mount John University Observatory, Lake Tekapo, New Zealand during 1990. Over 100 data points were acquired in each filter to an estimated precision of 0.02 mag. The flat maxima evident in the light curves suggest that the system, which is currently classed as an interacting candidate, should probably be considered as a detached one. A revised orbital period based on the inclusion of current data is presented. Eclipse timings indicate an eccentric orbit. An apsidal period in the vicinity of 120 yr is likely.

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