scholarly journals Precise Orbital Solutions for KEPLER Eclipsing Binaries of W UMa Type Showing Total Eclipses

2016 ◽  
Vol 33 ◽  
Author(s):  
H. V. Şenavcı ◽  
M. B. Doğruel ◽  
R. H. Nelson ◽  
M. Yılmaz ◽  
S. O. Selam
Keyword(s):  
High Precision ◽  
Binary Stars ◽  
Photometric Data ◽  
Eclipsing Binaries ◽  
Grid Search ◽  
Mass Ratio ◽  
Velocity Data ◽  
Flat Bottom ◽  
Mass Ratios ◽  
Radial Velocity Data

AbstractWe aim to discover the accuracy of photometric mass ratios (qph) determined for eclipsing binary stars, in the case of the system having at least one ‘flat bottom’ as a minimum profile, as well as the accuracy of data used in that sense. Within this context, we present the results of two-dimensional grid search (q – i) for some W UMa-type eclipsing binaries showing total eclipses, based on the high precision photometric data provided by the KEPLER Mission. The radial velocity data obtained for KIC10618253 in this study, enables us to compare both qph and the corresponding spectroscopic mass ratio (qsp) values. The results indicate that the high precision photometric data for overcontact eclipsing binaries showing total eclipses allow us to obtain the photometric mass ratios as accurate as the spectroscopic values.

scholarly journals Test of the Optimization Techniques for the Photometric Analysis of Contact Binaries

1992 ◽  
Vol 151 ◽  
pp. 387-390
Author(s):  
E. Lapasset ◽  
M. Gomez ◽  
R. Fariñas
Keyword(s):  
Optimization Techniques ◽  
Light Curves ◽  
Mass Ratio ◽  
Velocity Data ◽  
Photometric Analysis ◽  
Reliable Parameter ◽  
Contact Binaries ◽  
Cross Correlations ◽  
Grid Technique ◽  
Radial Velocity Data

We present light curve analyses of contact binaries and comparisons with previously published cross-correlations radial velocity data. The critical parameter q (mass-ratio) obtained from a grid technique is confronted with the spectroscopic value. For total eclipsing systems, both values are always in a good or reasonable agreement, including some stars with shallow light curves. For partial eclipsing systems, convergent photometric and spectroscopic results are obtained for an important set of stars. Two exceptions are V523 Cas and XY Boo for which some arguments are suggested. We concluded that reliable parameter determinations can be obtained from pure photometric solutions, by means of grid techniques.

scholarly journals Revisiting theKeplerfield withTESS: Improved ephemerides usingTESS2 min data

2021 ◽  
Vol 503 (3) ◽  
pp. 4092-4104
Author(s):  
Matthew P Battley ◽  
Michelle Kunimoto ◽  
David J Armstrong ◽  
Don Pollacco
Keyword(s):  
Radial Velocity ◽  
High Precision ◽  
Photometric Method ◽  
Velocity Data ◽  
Signal To Noise ◽  
Data Set ◽  
The Future ◽  
Radial Velocity Data ◽  
Very High

ABSTRACTUp to date planet ephemerides are becoming increasingly important as exoplanet science moves from detecting exoplanets to characterizing their architectures and atmospheres in depth. In this work, ephemerides are updated for 22 Kepler planets and 4 Kepler planet candidates, constituting all Kepler planets and candidates with sufficient signal to noise in the TESS 2 min data set. A purely photometric method is utilized here to allow ephemeris updates for planets even when they do not posses significant radial velocity data. The obtained ephemerides are of very high precision and at least seven years ‘fresher’ than archival ephemerides. In particular, significantly reduced period uncertainties for Kepler-411d, Kepler-538b, and the candidates K00075.01/K00076.01 are reported. O–C diagrams were generated for all objects, with the most interesting ones discussed here. Updated TTV fits of five known multiplanet systems with significant TTVs were also attempted (Kepler-18, Kepler-25, Kepler-51, Kepler-89, and Kepler-396), however these suffered from the comparative scarcity and dimness of these systems in TESS. Despite these difficulties, TESS has once again shown itself to be an incredibly powerful follow-up instrument as well as a planet-finder in its own right. Extension of the methods used in this paper to the 30 min-cadence TESS data and TESS extended mission has the potential to yield updated ephemerides of hundreds more systems in the future.

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 Velocity-Curve Analysis of the Spectroscopic Binary Stars V373 Cas, V2388 Oph, V401 Cyg, GM Dra, V523 Cas, AB And and HD 141929 by Artificial Neural Networks

2009 ◽  
Vol 26 (2) ◽  
pp. 121-127 ◽  
Author(s):  
K. Karami ◽  
K. Ghaderi ◽  
R. Mohebi ◽  
R. Sadeghi ◽  
M. M. Soltanzadeh
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Curve Analysis ◽  
Velocity Data ◽  
Orbital Parameters ◽  
Spectroscopic Binary ◽  
Artificial Neural ◽  
Artificial Neural Network Ann ◽  
Radial Velocity Data ◽  
Good Agreement

AbstractWe used an Artificial Neural Network (ANN) to derive the orbital parameters of spectroscopic binary stars. Using measured radial velocity data of seven double-lined spectroscopic binary systems V373 Cas, V2388 Oph, V401 Cyg, GM Dra, V523 Cas, AB And and HD 141929, we found corresponding orbital and spectroscopic elements. Our numerical results are in good agreement with those obtained by others using more traditional methods.

scholarly journals Two Giant Planets Orbiting the K Giant Star η Cet

2013 ◽  
Vol 8 (S299) ◽  
pp. 309-310
Author(s):  
T. Trifonov ◽  
S. Reffert ◽  
X. Tan ◽  
M. H. Lee ◽  
A. Quirrenbach
Keyword(s):  
Radial Velocity ◽  
High Precision ◽  
Parameter Space ◽  
Planetary System ◽  
Giant Planets ◽  
Stable Region ◽  
Velocity Data ◽  
Giant Star ◽  
Present Evidence ◽  
Radial Velocity Data

AbstractWe present evidence of a new planetary system around the K giant η Cet (HIP 5364, HD 6805, HR 334), based on 124 high-precision optical and infrared radial velocity data, taken at Lick Observatory (Hamilton) and at VLT (CRIRES). The best dynamical fit to the data is consistent with two massive planets (m1sini≈2.6MJup, m2sini≈3.3MJup) and with periods of P1≈407 days, P2≈740 days. To test the η Cet system's stability we perform ~ 10,000 dynamical investigations with maximum time spans of 108 years. We find that in case of moderate eccentricities, the planets can be effectively trapped in an anti-aligned stable 2:1 mean motion resonance (MMR), very close to the separatrix. A larger non-resonant stable region exists in low-eccentricity parameter space, although less probable than the 2:1 MMR region.

scholarly journals Statistics of Binary Stars: Semi-Major Axes

1976 ◽  
Vol 73 ◽  
pp. 369-379
Author(s):  
V. Trimble ◽  
C. Cheung
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Major Axis ◽  
Small Mass ◽  
Close Binaries ◽  
Mass Ratio ◽  
Orbital Elements ◽  
Semi Major Axis ◽  
Mass Ratios ◽  
Show Evidence

We have examined the distribution of the semi-major axes of the binary systems in the Sixth Catalogue of the Orbital Elements of Spectroscopic Binary Systems (and its extensions) and the correlation of semi-major axis with other properties of the systems. The total distribution has a single peak near asini=107km. Evolved systems have wider separations and smaller mass ratios than unevolved systems. Among each type separately, the distribution of mass ratios is bimodal and small mass ratio is correlated with large separation. These data appear to show evidence of two mechanisms of binary system formation and of the process of mass transfer in close binaries.

Mass Ratios in Wide Binary Stars

1997 ◽  
Vol 485 (2) ◽  
pp. 785-788 ◽  
Author(s):  
Mauri J. Valtonen
Keyword(s):  
Binary Stars ◽  
Wide Binary ◽  
Mass Ratios

Twin stars as tracers of binary evolution in the Kepler era

2021 ◽  
Author(s):  
Sara Bulut ◽  
Baris Hoyman ◽  
Ahmet Dervisoglu ◽  
Orkun Özdarcan ◽  
Ömür Cakilrli
Keyword(s):  
High Resolution ◽  
Internal Structure ◽  
Spectroscopic Analysis ◽  
Independent Method ◽  
Eclipsing Binaries ◽  
Physical Parameters ◽  
Evolutionary Status ◽  
Mass Ratio ◽  
Orbital Parameters ◽  
Binary Evolution

Abstract We present results of the combined photometric and spectroscopic analysis of four systems, which are eclipsing binaries with a twin–component (mass ratio q ≃ 1). These are exceptional tools to provide information for probing the internal structure of stars. None of the systems were previously recognized as twin binaries. We used a number of high–resolution optical spectra to calculate the radial velocities and later combined them with photometry to derive orbital parameters. Temperatures and metallicities of systems were estimated from high-resolution spectra. For each binary, we obtained a full set of orbital and physical parameters, reaching precision below 3 per cent in masses and radii for whole pairs. By comparing our results with PARSEC and MIST isochrones, we assess the distance, age and evolutionary status of the researched objects. The primary and/or secondary stars of EPIC 216075815 and EPIC 202843107 are one of the cases where asteroseismic parameters of δ Sct and γ Dor pulsators were confirmed by an independent method and rare examples of the twin–eclipsing binaries, therefore the following analyses and results concern the pulsating nature of the components.

scholarly journals Kinematics of Disk Stars in the Solar Neighbourhood

1998 ◽  
Vol 11 (1) ◽  
pp. 574-574
Author(s):  
A.E. Gómez ◽  
S. Grenier ◽  
S. Udry ◽  
M. Haywood ◽  
V. Sabas ◽  
...  
Keyword(s):  
Dispersion Relation ◽  
Radial Velocity ◽  
Velocity Dispersion ◽  
Tangential Velocity ◽  
Thin Disk ◽  
The Other ◽  
Proper Motions ◽  
Velocity Data ◽  
Kinematic Data ◽  
Radial Velocity Data

Using Hipparcos parallaxes and proper motions together with radial velocity data and individual ages estimated from isochones, the velocity ellipsoid has been determined as a function of age. On the basis of the available kinematic data two different samples were considered: a first one (7789 stars) for which only tangential velocities were calculated and a second one containing 3104 stars with available U, V and W velocity components and total velocities ≤ 65 km.s-1. The main conclusions are: -Mixing is not complete at about 0.8-1 Gyr. -The shape of the velocity ellipsoid changes with time getting rounder from σu/σv/σ-w = 1/0.63/0.42 ± 0.04 at about 1 Gyr to1/0.7/0.62 ±0.04 at 4-5 Gyr. -The age-velocity-dispersion relation (from the sample with kinematical selection) rises to a maximum, thereafter remaining roughly constant; there is no dynamically significant evolution of the disk after about 4-5 Gyr. -Among the stars with solar metallicities and log(age) > 9.8 two groups are identified: one has typical thin disk characteristics, the other is older than 10 Gyr and lags the LSR at about 40 km.s-1 . -The variation of the tangential velocity with age(without selection on the tangential velocity) shows a discontinuity at about 10 Gyr, which may be attributed to stars typically of the thick disk populations for ages > 10 Gyr.

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