scholarly journals The supergiant O + O binary system HD 166734: a new study

2016 ◽  
Vol 12 (S329) ◽  
pp. 402-402 ◽  
Author(s):  
E. Gosset ◽  
L. Mahy ◽  
Y. Damerdji ◽  
C. Nitschelm ◽  
H. Sana ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Radial Velocity ◽  
Velocity Curve ◽  
Physical Parameters ◽  
Radial Velocity Curve ◽  
X Ray ◽  
Orbital Parameters

AbstractWe present here a modern study of the radial velocity curve and of the photometric light curve of the very interesting supergiant O7.5If + O9I(f) binary system HD 166734. The physical parameters of the stars and the orbital parameters are carefully determined. We also perform the analysis of the observed X-ray light curve of this colliding-wind binary.

scholarly journals Semidetached double-lined eclipsing binaries: Stellar parameters and rare classes

2019 ◽  
Vol 491 (4) ◽  
pp. 5489-5497 ◽  
Author(s):  
Oleg Yu Malkov
Keyword(s):  
Radial Velocity ◽  
Velocity Curve ◽  
Eclipsing Binaries ◽  
Physical Parameters ◽  
Radial Velocity Curve ◽  
Orbital Parameters ◽  
Comprehensive List ◽  
Use Of Data ◽  
Rare Classes

ABSTRACT Semidetached eclipsing systems provide a unique opportunity to derive the basic properties of interacting binaries. The goal of this work is to collect and to make use of data on semidetached systems with available light and radial velocity curve solutions. I have compiled the most comprehensive list to date, of 119 semidetached double-lined eclipsing binaries, containing the orbital parameters and physical parameters of the components. I consider the classification of semidetached binaries and discuss gaps between various classes in the Hertzspung–Russell diagram. I list systems with component parameters that are inverted and briefly discuss their evolutionary state.

scholarly journals Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye

2020 ◽  
Vol 633 ◽  
pp. A98 ◽  
Author(s):  
Ł. Wyrzykowski ◽  
P. Mróz ◽  
K. A. Rybicki ◽  
M. Gromadzki ◽  
Z. Kołaczkowski ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Function ◽  
Space Mission ◽  
Galactic Disc ◽  
Radial Velocity Curve ◽  
Orbital Parameters ◽  
Data Points ◽  
Binary Orbit

Gaia16aye was a binary microlensing event discovered in the direction towards the northern Galactic disc and was one of the first microlensing events detected and alerted to by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to I = 12 mag, and it was covered in great detail with almost 25 000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution. We employed a full Keplerian binary orbit microlensing model combined with the motion of Earth and Gaia around the Sun to reproduce the complex light curve. The photometric data allowed us to solve the microlensing event entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first-ever microlensing space-parallax between the Earth and Gaia located at L2. The properties of the binary system were derived from microlensing parameters, and we found that the system is composed of two main-sequence stars with masses 0.57 ± 0.05 M⊙ and 0.36 ± 0.03 M⊙ at 780 pc, with an orbital period of 2.88 years and an eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve for the binary system. Events such as Gaia16aye indicate the potential for the microlensing method of probing the mass function of dark objects, including black holes, in directions other than that of the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations that can be made with a network of heterogeneous telescopes.

scholarly journals 59 Cygni: A Tilted ϕ Persei like System

2000 ◽  
Vol 175 ◽  
pp. 581-584 ◽  
Author(s):  
Th. Rivinius ◽  
S. Štefl
Keyword(s):  
Radial Velocity ◽  
Compact Star ◽  
Velocity Curve ◽  
Similar Nature ◽  
Radial Velocity Curve ◽  
Orbital Parameters ◽  
The One

AbstractThe binarity of 59 Cygni was confirmed and orbital parameters from the radial velocity curve of the primary derived. The observed emission variability resembles the one of ɸ Per in quite some detail, suggesting a similar nature of the companion: a hot, compact star.

scholarly journals TheαCrB binary system: A new radial velocity curve, apsidal motion, and the alignment of rotation and orbit axes

2016 ◽  
Vol 586 ◽  
pp. A104 ◽  
Author(s):  
J. H. M. M. Schmitt ◽  
K.-P. Schröder ◽  
G. Rauw ◽  
A. Hempelmann ◽  
M. Mittag ◽  
...  
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Velocity Curve ◽  
Apsidal Motion ◽  
Radial Velocity Curve ◽  
System A

scholarly journals NEW ORBITAL PARAMETERS AND RADIAL VELOCITY CURVE ANALYSIS OF SPECTROSCOPIC BINARY STARS

2012 ◽  
Vol 45 (1) ◽  
pp. 1-6 ◽  
Author(s):  
Kamal Ghaderi ◽  
Ali Pirkhedri ◽  
Touba Rostami ◽  
Salem Khodamoradi ◽  
Hedayat Fatahi
Keyword(s):  
Radial Velocity ◽  
Binary Stars ◽  
Curve Analysis ◽  
Velocity Curve ◽  
Radial Velocity Curve ◽  
Orbital Parameters ◽  
Spectroscopic Binary

scholarly journals CoRoT target HD 51844: a δ Scuti star in a binary system with periastron brightening

2013 ◽  
Vol 9 (S301) ◽  
pp. 59-62 ◽  
Author(s):  
Markus Hareter ◽  
Margit Paparó
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Radial Velocity ◽  
Frequency Analysis ◽  
Significant Variation ◽  
Orbital Motion ◽  
The Other ◽  
Physical Parameters ◽  
Reflected Light ◽  
Scuti Star

AbstractThe star HD 51844 was observed in the CoRoT LRa02 as a target in the seismology field, which turned out to be an SB2 system. The 117-day light curve revealed δ Scuti pulsations in the range of 6 to 15 d−1 where four frequencies have amplitudes larger than 1.4 mmag, and a rich frequency spectrum with amplitudes lower than 0.6 mmag. Additionally, the light curve exhibits a 3-mmag brightening event recurring every 33.5 days with a duration of about 5 days. The radial velocities from spectroscopy confirmed that the star is an eccentric binary system with nearly identical masses and physical parameters. The brightening event in the light curve coincides with the maximum radial-velocity separation showing that the brightening is in fact caused by tidal distortion and/or reflected light. One component displays large line-profile variations, while the other does not show significant variation. The frequency analysis revealed a quintuplet structure of the four highest-amplitude frequencies, which is due to the orbital motion of the pulsating star.

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