scholarly journals Radial velocity measurements and orbit determination of eight single-lined spectroscopic binary systems

2017 ◽  
Vol 338 (6) ◽  
pp. 671-679 ◽  
Author(s):  
R. Bischoff ◽  
M. Mugrauer ◽  
T. Zehe ◽  
D. Wöckel ◽  
A. Pannicke ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Orbit Determination ◽  
Binary Systems ◽  
Velocity Measurements ◽  
Spectroscopic Binary

scholarly journals Long Baseline Interferometry and Binary Stars

1983 ◽  
Vol 62 ◽  
pp. 191-201
Author(s):  
John Davis
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Current Status ◽  
Fundamental Properties ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Spectroscopic Binary ◽  
Future Plans ◽  
Intensity Interferometer

AbstractThe observations of α Vir with the Narrabri Stellar Intensity Interferometer demonstrated the potential of long baseline interferometry for the determination of fundamental properties of double-lined spectroscopic binary systems. Since the completion of the programme with the Narrabri instrument the Chatterton Astronomy Department has been conducting a study aimed at developing a stellar interferometer with limiting magnitude V ≳ +8 and maximum baseline ≳ 1 km (resolution at 500 nm ≲ 7 × 10−5 seconds of arc). The way in which a long baseline interferometer may be used in the study of binary stars is outlined, the requirements for this work are discussed, and the current status and future plans of the Chatterton Astronomy Department’s programme to develop a new long baseline interferometer are summarised.

High Velocity Spectroscopic Binary Orbits from Photoelectric Radial Velocities: BD+20 5152, a Possible Triple System

2010 ◽  
Vol 19 (3-4) ◽  
Author(s):  
J. Sperauskas ◽  
A. Bartkevičius ◽  
R. P. Boyle ◽  
V. Deveikis
Keyword(s):  
Radial Velocity ◽  
Proper Motion ◽  
High Velocity ◽  
Triple System ◽  
Mass Velocity ◽  
Center Of Mass ◽  
Primary Component ◽  
Eccentric Orbit ◽  
Velocity Measurements ◽  
Spectroscopic Binary

AbstractThe spectroscopic orbit of a high proper motion star, BD+20 5152, is calculated from 34 CORAVEL-type radial velocity measurements. The star has a slightly eccentric orbit with a period of 5.70613 d, half-amplitude of 47.7 km/s and eccentricity of 0.049. The center-of-mass velocity of the system is -24.3 km/s. BD+20 5152 seems to be a triple system consisting of a G8 dwarf as a primary component and of two K6-M0 dwarfs as secondary and tertiary components. This model is based on the analysis of its UBVRI and JHK magnitudes. According to the SuperWASP photometry, spots on the surface of the primary are suspected. The excessive brightness in the Galex FUV and NUV magnitudes and a non-zero eccentricity suggest the age of this system to be less than 1 Gyr.

scholarly journals Two new double-lined spectroscopic binary white dwarfs

2020 ◽  
Vol 493 (2) ◽  
pp. 2805-2816 ◽  
Author(s):  
Mukremin Kilic ◽  
A Bédard ◽  
P Bergeron ◽  
Alekzander Kosakowski
Keyword(s):  
Radial Velocity ◽  
White Dwarf ◽  
White Dwarfs ◽  
Binary Systems ◽  
Mass Ratio ◽  
Orbital Parameters ◽  
Long Period ◽  
Spectroscopic Binary ◽  
Velocity Variations ◽  
Period System

ABSTRACT We present radial velocity observations of four binary white dwarf candidates identified through their overluminosity. We identify two new double-lined spectroscopic binary systems, WD 0311–649 and WD 1606+422, and constrain their orbital parameters. WD 0311–649 is a 17.7 h period system with a mass ratio of 1.44 ± 0.06 and WD 1606+422 is a 20.1 h period system with a mass ratio of 1.33 ± 0.03. An additional object, WD 1447–190, is a 43 h period single-lined white dwarf binary, whereas WD 1418–088 does not show any significant velocity variations over time-scales ranging from minutes to decades. We present an overview of the 14 overluminous white dwarfs that were identified by Bédard et al., and find the fraction of double- and single-lined systems to be both 31 per cent. However, an additional 31 per cent of these overluminous white dwarfs do not show any significant radial velocity variations. We demonstrate that these must be in long-period binaries that may be resolved by Gaia astrometry. We also discuss the overabundance of single low-mass white dwarfs identified in the SPY survey, and suggest that some of those systems are also likely long-period binary systems of more massive white dwarfs.

scholarly journals WIYN Open Cluster Study. LXXXII. Radial-velocity Measurements and Spectroscopic Binary Orbits in the Open Cluster NGC 7789

2020 ◽  
Vol 160 (4) ◽  
pp. 169 ◽  
Author(s):  
Andrew C. Nine ◽  
Katelyn E. Milliman ◽  
Robert D. Mathieu ◽  
Aaron M. Geller ◽  
Emily M. Leiner ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Open Cluster ◽  
Velocity Measurements ◽  
Spectroscopic Binary

Application of a probabilistic neural network in radial velocity curve analysis of the spectroscopic binary stars PV Pup, BV Dra, AI Phe, V1130 Tau, NSV 223, and V502 Oph

2011 ◽  
Vol 89 (10) ◽  
pp. 1035-1040 ◽  
Author(s):  
K. Karami ◽  
K. Ghaderi ◽  
R. Mohebi ◽  
M.M. Soltanzadeh
Keyword(s):  
Radial Velocity ◽  
Binary Stars ◽  
Binary Systems ◽  
Probabilistic Neural Network ◽  
Curve Analysis ◽  
Velocity Data ◽  
Radial Velocity Curve ◽  
Spectroscopic Binary ◽  
Radial Velocity Data ◽  
Good Agreement

Using measured radial velocity data from six double-lined spectroscopic binary systems PV Pup, BV Dra, AI Phe, V1130 Tau, NSV 223 (or DZ Psc), and V502 Oph, we find corresponding orbital and spectroscopic elements via the method introduced by Karami et al. (New Astron. 14, 478 (2009)). Our numerical results are in good agreement with those obtained by others using more traditional methods. Using a statistical analysis, we also conclude that for BV Dra, V1130 Tau, NSV 223 (or DZ Psc), and V502 Oph, a circular orbit is quite consistent.

scholarly journals An overtone Cepheid variable in an LMC eclipsing binary

2004 ◽  
Vol 193 ◽  
pp. 372-376 ◽  
Author(s):  
D. Lepischak ◽  
D.L. Welch
Keyword(s):  
Evolutionary History ◽  
Binary Systems ◽  
Precise Determination ◽  
Light Curves ◽  
Intermediate Mass ◽  
Eclipsing Binary ◽  
Spectroscopic Binary ◽  
First Time ◽  
Absolute Luminosity

AbstractEclipsing binary systems potentially allow the direct and precise determination of the important properties of their component stars. An eclipsing binary containing a Cepheid variable which is also a double-lined spectroscopic binary would allow, for the first time, the direct measurement of the absolute luminosity and mass of the Cepheid. The MACHO Project LMC database contains five systems whose light curves show variations due to both eclipses and pulsation but only one has been clearly identified as an intermediate-mass, Population I object. This object, MACHO 81.8997.87 (= OGLELMC_SC16 119952) is a 2.035-d overtone Cepheid in an 800.4-d binary system with an M-type companion. Here we present the results of the analysis of the light curve of this system, the implications for its evolutionary history and discuss the prospects for future observations.

scholarly journals Searching for Earth-mass planets around α Centauri: precise radial velocities from contaminated spectra

2014 ◽  
Vol 14 (2) ◽  
pp. 173-176 ◽  
Author(s):  
Christoph Bergmann ◽  
Michael Endl ◽  
John B. Hearnshaw ◽  
Robert A. Wittenmyer ◽  
Duncan J. Wright
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Binary Systems ◽  
Angular Separation ◽  
Radial Velocities ◽  
The Other ◽  
Cross Contamination ◽  
Star System ◽  
Spectroscopic Binary ◽  
Ongoing Project

AbstractThis work is part of an ongoing project which aims to detect terrestrial planets in our neighbouring star system α Centauri using the Doppler method. Owing to the small angular separation between the two components of the α Cen AB binary system, the observations will to some extent be contaminated with light coming from the other star. We are accurately determining the amount of contamination for every observation by measuring the relative strengths of the H-α and NaD lines. Furthermore, we have developed a modified version of a well-established Doppler code that is modelling the observations using two stellar templates simultaneously. With this method we can significantly reduce the scatter of the radial velocity (RV) measurements due to spectral cross-contamination and hence increase our chances of detecting the tiny signature caused by potential Earth-mass planets. After correcting for the contamination we achieve RV precision of ~2.5 m s−1 for a given night of observations. We have also applied this new Doppler code to four southern double-lined spectroscopic binary systems (HR159, HR913, HR7578 and HD181958) and have successfully recovered radial velocities for both components simultaneously.

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