Determination of differential limb darkening of eclipsing binaries from multicolor photometric observations. I

1961 ◽  
Vol 66 ◽  
pp. 405 ◽  
Author(s):  
K. Serkowski
Keyword(s):  
Eclipsing Binaries ◽  
Photometric Observations ◽  
Limb Darkening

scholarly journals Precise calibration of the dependence of surface brightness–colour relations on colour and class for late-type stars

2020 ◽  
Vol 640 ◽  
pp. A2 ◽  
Author(s):  
A. Salsi ◽  
N. Nardetto ◽  
D. Mourard ◽  
O. Creevey ◽  
D. Huber ◽  
...  
Keyword(s):  
Spectral Type ◽  
Surface Brightness ◽  
Eclipsing Binaries ◽  
Angular Diameter ◽  
Late Type ◽  
Luminosity Class ◽  
Photometric Observations ◽  
Photometric Measurements ◽  
Selection Of

Context. Surface brightness–colour relations (SBCRs) are used to derive the stellar angular diameters from photometric observations. They have various astrophysical applications, such as the distance determination of eclipsing binaries or the determination of exoplanet parameters. However, strong discrepancies between the SBCRs still exist in the literature, in particular for early and late-type stars. Aims. We aim to calibrate new SBCRs as a function of the spectral type and the luminosity class of the stars. Our goal is also to apply homogeneous criteria to the selection of the reference stars and in view of compiling an exhaustive and up-to-date list of interferometric late-type targets. Methods. We implemented criteria to select measurements in the JMMC Measured Diameters Catalog. We then applied additional criteria on the photometric measurements used to build the SBCRs, together with stellar characteristics diagnostics. Results. We built SBCRs for F5/K7–II/III, F5/K7–IV/V, M–II/III and M–V stars, with respective rms of σFV = 0.0022 mag, σFV = 0.0044 mag, σFV = 0.0046 mag, and σFV = 0.0038 mag. This results in a precision on the angular diameter of 1.0%, 2.0%, 2.1%, and 1.7%, respectively. These relations cover a large V − K colour range of magnitude, from 1 to 7.5. Our work demonstrates that SBCRs are significantly dependent on the spectral type and the luminosity class of the star. Through a new set of interferometric measurements, we demonstrate the critical importance of the selection criteria proposed for the calibration of SBCR. Finally, using the Gaia photometry for our samples, we obtained (G − K) SBCRs with a precision on the angular diameter between 1.1% and 2.4%. Conclusions. By adopting a refined and homogeneous methodology, we show that the spectral type and the class of the star should be considered when applying an SBCR. This is particularly important in the context of PLATO.

scholarly journals New observations and transit solutions of the exoplanets HAT-P-53b and XO-5b

2018 ◽  
pp. 15-20
Author(s):  
Diana Kjurkchieva ◽  
Nikola Petrov ◽  
Sunay Ibryamov ◽  
Grigor Nikolov ◽  
Velimir Popov
Keyword(s):  
Orbital Period ◽  
Empirical Investigation ◽  
High Sensitivity ◽  
Time Span ◽  
Photometric Observations ◽  
Higher Temperature ◽  
Limb Darkening ◽  
Host Stars

We present photometric observations of transiting exoplanets HATP-53b and XO-5b by the Rozhen 2 m telescope. The modeling of the HAT-P-53b transit required bigger planet radius than the previously published value due to the bigger depth of the newly-observed transit. The transit solution of XO-5b led to values of fitted parameters within errors of the previously published results. Based on a time span of around 9 years we improved the orbital period of XO-5b to the value of 4.187751515 d. The quality of our data does not allow determination of planet temperatures by the transit solutions. Our results confirmed the Jupiter type of the two targets. The more bloated nature of HAT-P-53b is a result of its considerable closer orbit and higher temperature of the host star. The best fits of the newly-observed transits of HAT-P-53b and XO-5b correspond to the quadratic limb-darkening law of their host stars whose coefficients were determined. The high sensitivity of the transit solutions to the stellar limb-darkening law and its coefficient( s) is proposed as a tool for precise empirical investigation of the limb-darkening effect of host stars and its interpretation.

scholarly journals Masses, Radii and Luminosities from Analysis of Eclipsing Binaries

1985 ◽  
Vol 111 ◽  
pp. 81-96
Author(s):  
Daniel M. Popper
Keyword(s):  
Eclipsing Binaries ◽  
Radiative Properties ◽  
Binary Analysis ◽  
Eclipsing Binary ◽  
Fundamental Properties ◽  
Photometric Observations

The reliability of values of the fundamental properties of stars derived from eclipsing binary analysis is discussed in terms of general concepts. Since the principles involved in the determination of masses and radii are simple, the heart of the matter is the care and judgment with which the relevant spectrographic and photometric observations are obtained and analyzed. Problems in the evaluation of the radiative properties require special attention.

scholarly journals Age Determination of Galactic B-type Stars in Double-lined Eclipsing Binaries

2019 ◽  
Vol 886 (1) ◽  
pp. 35 ◽  
Author(s):  
Jadwiga Daszyńska-Daszkiewicz ◽  
Amadeusz Miszuda
Keyword(s):  
Age Determination ◽  
Eclipsing Binaries

scholarly journals Close-In Substellar Companions and the Formation of sdB-Type Close Binary Stars

2015 ◽  
Vol 2 (1) ◽  
pp. 183-187 ◽  
Author(s):  
L. Y. Zhu ◽  
S. B. Qian ◽  
E.-G. Zhao ◽  
E. Fernández Lajús ◽  
Z.-T. Han
Keyword(s):  
Binary Stars ◽  
Eclipsing Binaries ◽  
Close Binary ◽  
Close Binaries ◽  
Close Binary Stars ◽  
Cataclysmic Binaries ◽  
Low Mass ◽  
Substellar Companions ◽  
Orbital Periods

The sdB-type close binaries are believed to have experienced a common-envelope phase and may evolve into cataclysmic binaries (CVs). About 10% of all known sdB binaries are eclipsing binaries consisting of very hot subdwarf primaries and low-mass companions with short orbital periods. The eclipse profiles of these systems are very narrow and deep, which benefits the determination of high precise eclipsing times and makes the detection of small and close-in tertiary bodies possible. Since 2006 we have monitored some sdB-type eclipsing binaries to search for the close-in substellar companions by analyzing the light travel time effect. Here some progresses of the program are reviewed and the formation of sdB-type binary is discussed.

scholarly journals Prospects for Detecting Unseen Companions of Periodic Variables

1995 ◽  
Vol 166 ◽  
pp. 205-208
Author(s):  
A. Pigulski
Keyword(s):  
Speckle Interferometry ◽  
Time Effect ◽  
Eclipsing Binaries ◽  
Pulsating Stars ◽  
Different Types ◽  
Mass Ratios ◽  
Orbital Periods

All periodic variables with stable periods such as pulsating stars, eclipsing binaries and pulsars offer the possibility of detecting unseen companion(s) by means of the light-time effect. We discuss the limitations of the method (the visibility of the effect) for different types of periodic variables. Special attention is paid to the ranges of mass ratios and orbital periods in which unseen companions can be found. We also indicate several systems with light-time effect in which hypothetical companions can be detected by speckle interferometry or precise astrometric observations. In these cases, the detection of the companions may lead to the determination of the components' masses.

scholarly journals A Precise Estimate of the Radius of HD 149026b

2008 ◽  
Vol 4 (S253) ◽  
pp. 466-469
Author(s):  
Philip Nutzman ◽  
David Charbonneau ◽  
Joshua N. Winn ◽  
Heather A. Knutson ◽  
Jonathan J. Fortney ◽  
...  
Keyword(s):  
Accurate Determination ◽  
Stellar Mass ◽  
Radius Ratio ◽  
Light Curves ◽  
Heavy Elements ◽  
Precise Estimate ◽  
Extrasolar Planet ◽  
Orbital Inclination ◽  
Limb Darkening

AbstractWe present Spitzer 8 μm transit observations of the extrasolar planet system HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb-darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet-star radius ratio of Rp/R∗=0.05158±0.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85°.4+0°.9−0°.8 and a planet radius of 0.755 ± 0.040 RJ. These measurements further support models in which the planet is greatly enriched in heavy elements.

scholarly journals OMC/INTEGRAL photometric observations of pulsating components in eclipsing binaries and characterization of DY Aqr

2014 ◽  
Vol 443 (4) ◽  
pp. 3022-3032 ◽  
Author(s):  
J. Alfonso-Garzón ◽  
B. Montesinos ◽  
A. Moya ◽  
J. M. Mas-Hesse ◽  
S. Martín-Ruiz
Keyword(s):  
Eclipsing Binaries ◽  
Photometric Observations
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