Physics of Eclipsing Binaries. Ii. Toward the Increased Model Fidelity

Prša, Andrej; Conroy, Kyle E.; Horvat, Martin; Pablo, H.; Kochoska, A.; Bloemen, S.; Giammarco, J.; Hambleton, Kelly; Degroote, P.

doi:10.3847/1538-4365/227/2/29

Cited by 282 publications

(211 citation statements)

References 53 publications

Supporting

Mentioning

211

Contrasting

Order By: Relevance

“…It is composed of three processes: Doppler shift, time dilation, and light abberation (e.g., van Kerkwijk et al 2010;Bloemen et al 2011;Prša et al 2016).…”

Section: The Beaming Effect (Doppler Boosting)mentioning

confidence: 99%

The Astrophysics of Visible-light Orbital Phase Curves in the Space Age

Shporer

2017

PASP

129

107

View full text Add to dashboard Cite

The field of visible-light continuous time series photometry is now at its golden age, manifested by the continuum of past (CoRoT, Kepler), present (K2), and future (TESS, PLATO) space-based surveys delivering high precision data with a long baseline for a large number of stars. The availability of the high quality data has enabled astrophysical studies not possible before, including for example detailed asteroseismic investigations and the study of the exoplanet census including small planets. This has also allowed to study the minute photometric variability following the orbital motion in stellar binaries and star-planet systems which is the subject of this review. We focus on systems with a main sequence primary and a low-mass secondary, from a small star to a massive planet. The orbital modulations are induced by a combination of gravitational and atmospheric processes, including the beaming effect, tidal ellipsoidal distortion, reflected light, and thermal emission. Therefore, the phase curve shape contains information about the companion's mass and atmospheric characteristics, making phase curves a useful astrophysical tool. For example, phase curves can be used to detect and measure the mass of short-period low-mass companions orbiting hot fast-rotating stars, out of reach of other detection methods. Another interesting application of phase curves is using the orbital phase modulations to look for non-transiting systems, which comprise the majority of stellar binary and star-planet systems. We discuss the science done with phase curves, the first results obtained so far, and the current difficulties and open questions related to this young and evolving subfield.

show abstract

“…It is composed of three processes: Doppler shift, time dilation, and light abberation (e.g., van Kerkwijk et al 2010;Bloemen et al 2011;Prša et al 2016).…”

Section: The Beaming Effect (Doppler Boosting)mentioning

confidence: 99%

The Astrophysics of Visible-light Orbital Phase Curves in the Space Age

Shporer

2017

PASP

129

107

View full text Add to dashboard Cite

show abstract

“…The photometric and spectral data were fitted using the PHOEBE code (Prsa et al , ; Prsa & Zwitter ), which is based on the Wilson–Devinney (WD) code (Wilson , ; Wilson & Devinney ). It allows simultaneous modeling of photometric data in a number of filters as well as radial velocity data and provides a graphical user interface.…”

Section: Simultaneous Modelingmentioning

confidence: 99%

Photometric and spectral observations of two W UMa stars with periods of one third of a day

2018

View full text Add to dashboard Cite

Photometric and spectral observations of the W UMa binaries NSVS 254037 and V505 Lac with periods of around 8 hr are presented. The simultaneous light curve and radial velocity curve solutions revealed that their components are of G spectral type. The two targets undergo partial eclipses. They both have overcontact configurations of W subtype with fill‐out factor f ∼ 0.1. The derived parameters of NSVS 254037 are: mass ratio q = 2.42; orbital inclination i = 67.1°; temperatures T1 = 5800 K and T2 = 5585 K; masses M1 = 0.47 M⊙ and M2 = 1.15 M⊙; radii R1 = 0.72 R⊙ and R2 = 1.07 R⊙; luminosities L1 = 0.53 L⊙ and L2 = 1.0 L⊙; equatorial velocities V1 = 89 km−1 and V2 = 146 km−1; and distance d = 175 pc, almost the same as those of GAIA(DR2). The derived parameters of V505 Lac are: mass ratio q = 2.53; orbital inclination i = 57.30; temperatures T1 = 5,600 K and T2 = 5,166 K; masses M1 = 0.38 M⊙ and M2 = 0.97 M⊙; radii R1 = 0.69 R⊙ and R2 = 1.04 R⊙; luminosities L1 = 0.41 L⊙ and L2 = 0.68 L⊙; equatorial velocities V1 = 106 km−1 and V2 = 129 km−1; and distance d = 117 pc, smaller than those of GAIA by 19%. Thus, NSVS 254037 and V505 Lac turned out similar not only in periods and magnitudes but also in mass ratios, radii, and fill‐out factors.

show abstract

“…That would result in better evaluation of relative precision of each data sets and it would augmented the internal precision of the physical parameters of the whole sample. Significant help in this respect can be expected from using new, high precision numerical codes like ellc (Maxted 2016) or Phoebe-2 (Prša et al 2016), allowing for a very homogenous analysis of the full sample.…”

Section: Uniform Analysismentioning

confidence: 99%

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Graczyk

Konorski

Pietrzyński

et al. 2017

ApJ

View full text Add to dashboard Cite

In this study we investigate the calibration of surface brightness-color (SBC) relations based solely on eclipsing binary stars. We selected a sample of 35 detached eclipsing binaries with trigonometric parallaxes from Gaia DR1 or Hipparcos, whose absolute dimensions are known with an accuracy better than 3% and that lie within 0.3 kpc from the Sun. For the purpose of this study, we used mostly homogeneous optical and near-infrared photometry based on the Tycho-2 and 2MASS catalogs. We derived geometric angular diameters for all stars in our sample with a precision better than 10%, and for 11 of them with a precision better than 2%. The precision of individual angular diameters of the eclipsing binary components is currently limited by the precision of the geometric distances (∼5% on average). However, by using a subsample of systems with the best agreement between their geometric and photometric distances, we derived the precise SBC relations based only on eclipsing binary stars. These relations have precisions that are comparable to the best available SBC relations based on interferometric angular diameters, and they are fully consistent with them. With very precise Gaia parallaxes becoming available in the near future, angular diameters with a precision better than 1% will be abundant. At that point, the main uncertainty in the total error budget of the SBC relations will come from transformations between different photometric systems, disentangling of component magnitudes, and for hot OB stars, the main uncertainty will come from the interstellar extinction determination. We argue that all these issues can be overcome with modern high-quality data and conclude that a precision better than 1% is entirely feasible.

show abstract

Physics of Eclipsing Binaries. Ii. Toward the Increased Model Fidelity

Cited by 282 publications

References 53 publications

The Astrophysics of Visible-light Orbital Phase Curves in the Space Age

The Astrophysics of Visible-light Orbital Phase Curves in the Space Age

Photometric and spectral observations of two W UMa stars with periods of one third of a day

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Contact Info

Product

Resources

About