scholarly journals The Third Body in the Eclipsing Binary AV CMi: Hot Jupiter or Brown Dwarf?

2011 ◽  
Vol 7 (S282) ◽  
pp. 57-58
Author(s):  
Alexios Liakos ◽  
Dimitris Mislis ◽  
Panagiotis Niarchos
Keyword(s):  
Light Curves ◽  
Third Body ◽  
Brown Dwarf ◽  
Eclipsing Binary ◽  
The Third ◽  
Hot Jupiter

AbstractNew transit light curves of the third body in the system AV CMi have been obtained. The eclipsing pair's light curves were re-analysed with the W-D code and new absolute elements were derived for the two components. Moreover the new light curves (together with those given by Liakos & Niarchos 2010) of the third body transiting one of the components were analysed with the Photometric Software for Transits (PhoS-T). The results from both analyses are combined with the aim to study the nature of the third component.

scholarly journals WD1032 + 011, an inflated brown dwarf in an old eclipsing binary with a white dwarf

2020 ◽  
Vol 497 (3) ◽  
pp. 3571-3580 ◽  
Author(s):  
S L Casewell ◽  
C Belardi ◽  
S G Parsons ◽  
S P Littlefair ◽  
I P Braker ◽  
...  
Keyword(s):  
Spectral Type ◽  
White Dwarf ◽  
Light Curves ◽  
Brown Dwarf ◽  
Eclipsing Binary ◽  
The Third ◽  
Thick Disc ◽  
Low Mass ◽  
High Cadence

ABSTRACT We present the discovery of only the third brown dwarf known to eclipse a non-accreting white dwarf. Gaia parallax information and multicolour photometry confirm that the white dwarf is cool (9950 ± 150 K) and has a low mass (0.45 ± 0.05 M⊙), and spectra and light curves suggest the brown dwarf has a mass of 0.067 ± 0.006 M⊙ (70MJup) and a spectral type of L5 ± 1. The kinematics of the system show that the binary is likely to be a member of the thick disc and therefore at least 5-Gyr old. The high-cadence light curves show that the brown dwarf is inflated, making it the first brown dwarf in an eclipsing white dwarf-brown dwarf binary to be so.

scholarly journals New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions

2020 ◽  
Vol 29 (1) ◽  
pp. 72-80 ◽  
Author(s):  
Fatemeh Davoudi ◽  
Atila Poro ◽  
Fahri Alicavus ◽  
Afshin Halavati ◽  
Saeed Doostmohammadi ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Function ◽  
Light Curves ◽  
Complete Analysis ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Third Body ◽  
Eclipsing Binary

AbstractNew observations of the eclipsing binary system V1848 Ori were carried out using the V filter resulting in a determination of new times of minima and new ephemeris were obtained. We presented the first complete analysis of the system’s orbital period behavior and analysis of O-C diagram done by the GA and MCMC approaches in OCFit code. The O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the LITE effect with a period of 10.57 years and an amplitude of 7.182 minutes. It appears that there is a third body with mass function of f (m3) = 0.0058 M⊙ in this binary system. The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%. The O’Connell effect was not seen in the light curve and there is no need to add spot.

scholarly journals NEAR-INFRARED LIGHT CURVES OF THE BROWN DWARF ECLIPSING BINARY 2MASS J05352184-0546085: CAN SPOTS EXPLAIN THE TEMPERATURE REVERSAL?

2009 ◽  
Vol 699 (2) ◽  
pp. 1196-1208 ◽  
Author(s):  
Yilen Gómez Maqueo Chew ◽  
Keivan G. Stassun ◽  
Andrej Prša ◽  
Robert D. Mathieu
Keyword(s):  
Near Infrared ◽  
Light Curves ◽  
Infrared Light ◽  
Brown Dwarf ◽  
Near Infrared Light ◽  
Eclipsing Binary

A high-mass-ratio red-dwarf contact binary with an extremely cool close-in red dwarf

2019 ◽  
Author(s):  
Xiao-Hui Fang ◽  
Shengbang Qian ◽  
Miloslav Zejda ◽  
Soonthornthum Boonrucksar ◽  
Xiao Zhou ◽  
...  
Keyword(s):  
Orbital Period ◽  
Light Curves ◽  
High Mass ◽  
Mass Ratio ◽  
Third Body ◽  
Dynamical Interaction ◽  
The Third ◽  
Short Period ◽  
Contact Binaries ◽  
Mass Component

Abstract 1SWASP J161335.80$-$284722.2 (hereafter J161335) is an eclipsing red-dwarf binary with an orbital period of $0.229778\:$d, which is around the short-period limit for contact binaries. Three sets of multi-color light curves of J161335 were obtained from different telescopes in 2015 and 2016 and are analyzed using the Wilson–Devinney method. We discovered that the system is a W-type contact system with a contact degree of 19% and a high mass ratio of 0.91. By using all available eclipse times, we found that the observed $-$ calculated $(O-C)$ diagram displays a cyclic oscillation with an amplitude of 0.00196($\pm 0.00006)\:$d and a period of 4.79($\pm 0.14)\:$yr while it undergoes a downward parabolic change. This downward variation corresponds to a continuous decrease in the orbital period at a rate of $dP/dt = -4.26(\pm$0.01) $\times$ 10$^{-7}\:$d$\:$yr$^{-1}$. The small-amplitude oscillation is explained as the light travel-time effect from the gravitational influence of a third body with a lowest mass of $M _{3}$ = 0.15($\pm 0.01)M_{\,\odot }$. In solving the light curves, we found that the third light is increasing, with the wavelength suggesting that the third body may be a cool red dwarf. This is in agreement with the results obtained by analyzing the $O-C$ diagram. The tertiary red dwarf is orbiting the central red-dwarf binary at an orbital separation of 2.8($\pm 0.2$) au. These results suggest that the J161335 system may be formed through early dynamical interaction where the original low-mass component was replaced by a higher-mass third body and the lower-mass component was kicked out to a wider orbit. In this way, a hierarchical triple system similar to J161335 with a high-mass-ratio binary and a small close-in third body is formed.

Photometric elements, apsidal motion, and the third body in the eclipsing binary V974 Cyg

2011 ◽  
Vol 55 (11) ◽  
pp. 989-999 ◽  
Author(s):  
M. V. Kuznetsov ◽  
Kh. F. Khaliullin ◽  
A. I. Khaliullina ◽  
V. G. Metlov ◽  
L. V. Mossakovskaya
Keyword(s):  
Apsidal Motion ◽  
Third Body ◽  
Eclipsing Binary ◽  
The Third ◽  
Photometric Elements

Visual orbit of the third body on the eclipsing binary SZ Cam

2007 ◽  
Vol 26 (1-3) ◽  
pp. 145-146 ◽  
Author(s):  
S. YU. Gorda ◽  
YU. YU. Balega ◽  
E. A. Pluzhnik ◽  
Z. U. Shkhagosheva
Keyword(s):  
Third Body ◽  
Eclipsing Binary ◽  
The Third

scholarly journals The Detectability of Binary Star Planetary and Brown Dwarf Companions From Eclipse Timing Variations

2021 ◽  
Author(s):  
A K Getley ◽  
B Carter ◽  
R King ◽  
S O’Toole
Keyword(s):  
Binary Star ◽  
Large Datasets ◽  
Orbital Eccentricity ◽  
Key Factors ◽  
Third Body ◽  
Brown Dwarf ◽  
Eclipsing Binary ◽  
Kepler Mission ◽  
Eclipsing Binary Star ◽  
Computational Resources

Abstract In this paper, we determine the detectability of eclipsing binary star companions from eclipse timing variations using the Kepler mission dataset. Extensive and precise stellar time-series photometry from space-based missions enable searches for binary star companions. However, due to the large datasets and computational resources involved, these searches would benefit from guidance from detection simulations. Our simulations start with and benefit from the use of empirical Kepler mission data, into which we inject third bodies to predict the resulting timing of binary star eclipses. We find that the orbital eccentricity of the third body and the orbital period of the host binary star are the key factors in detecting companions. Target brightness is also likely to be a factor in detecting companions. Detectable third body masses and periods can be efficiently bound using just two equations. Our results enable the setting of realistic expectations when planning searches for eclipsing binary star planetary and brown dwarf companions. Our results also suggest the brown dwarf desert is real rather than observational selection.

scholarly journals Light-time effect detected in fourteen eclipsing binaries

2020 ◽  
Vol 643 ◽  
pp. A130
Author(s):  
P. Zasche ◽  
R. Uhlař ◽  
P. Svoboda ◽  
P. Cagaš ◽  
M. Mašek
Keyword(s):  
Time Effect ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Physical Parameters ◽  
Third Body ◽  
Light Curve Analysis ◽  
Multiple Systems ◽  
The Third ◽  
Minimal Mass ◽  
Triple Star

The available minima timings of 14 selected eclipsing binaries (V1297 Cas, HD 24105, KU Aur, GU CMa, GH Mon, AZ Vel, DI Lyn, DK Her, GQ Dra, V624 Her, V1134 Her, KIC 6187893, V1928 Aql, V2486 Cyg) were collected and analyzed. Using the automatic telescopes, surveys, and satellite data, we derived more than 2500 times of eclipses, accompanied with our own ground-based observations. These data were used to detect the period variations in these multiple systems. The eclipse timing variations were described using the third-body hypothesis and the light-time effect. Their respective periods were derived as 2.5, 16.2, 27, 20, 64, 5.6, 22, 115, 27, 42, 6.9, 11.2, 4.1, and 8.4 years for these systems, respectively. The predicted minimal mass of the third body was calculated for each of the systems, and we discuss here their prospective detectability. The light curves of HD 24105, GH Mon, DK Her, V1134 Her, KIC 6187893, V1928 Aql, and V2486 Cyg were analyzed using the PHOEBE program, resulting in physical parameters of the components. Significant fractions of the third light were detected during the light-curve analysis, supporting our hypothesis of the triple-star nature of all these systems. The majority of these systems (nine out of 14) were already known as visual doubles. Our study shifts them to possible quadruples, what makes them even more interesting.

scholarly journals Planets in Binary Systems

2011 ◽  
Vol 7 (S282) ◽  
pp. 69-70
Author(s):  
Antonio Pilello
Keyword(s):  
Binary Systems ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Centre Of Mass ◽  
Third Body ◽  
Eclipsing Binary ◽  
The Public ◽  
Public Data ◽  
Low Mass ◽  
The Times

AbstractIn close eclipsing binary systems, measurements of the eclipse timing variations (ETV), obtained by means of accurate light curves, may be used to find circumbinary additional objects. The presence of these objects causes the motion of the eclipsing binary with respect to the centre of mass of the entire system and it results in advances or delays in the times of eclipses due to the light time effect. The most important issue of this project is to inspect the potential of detecting low mass substellar companions to close eclipsing binaries through the timing method. For this purpose, we use the public data from Kepler and CoRoT spacecrafts, collecting the light curves for a selected sample and analyzing the observed minus calculated (O-C) times of the eclipses in the search for ETVs and characterizing them. A large amplitude of the O-C ETVs can be explained in some cases by the presence of a third body in the system.

On the Third‐Body Hypothesis of the Eclipsing Binary AS Camelopardalis

1997 ◽  
Vol 475 (2) ◽  
pp. 798-802 ◽  
Author(s):  
S. A. Khodykin ◽  
V. G. Vedeneyev
Keyword(s):  
Third Body ◽  
Eclipsing Binary ◽  
The Third
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