Eclipsing Binary Stars: Modeling and Analysis

Kallrath, Joseph; Milone, Eugene F.

doi:10.1007/978-1-4419-0699-1

Cited by 154 publications

(154 citation statements)

References 2 publications

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“…One thousand individuals were used in the population and 300 generations were produced. The best fit found by this procedure was further refined using a simulated annealing chain (Kallrath & Milone 2009). The error was estimated using 10 4 random models with values within 1 2 c s + of our best solution.…”

Section: Modeling Of the Photometric And Radial Velocity Datamentioning

confidence: 99%

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

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Only a few well characterized very low-mass M dwarfs are known today. Our understanding of M dwarfs is vital as these are the most common stars in our solar neighborhood. We aim to characterize the properties of a rare F+dM stellar system for a better understanding of the low-mass end of the Hertzsprung-Russel diagram. We used photometric light curves and radial velocity follow-up measurements to study the binary. Spectroscopic analysis was used in combination with isochrone fitting to characterize the primary star. The primary star is an early F-type main-sequence star with a mass of (1.493 ± 0.073) M e and a radius of (1.474 ± 0.040) R e . The companion is an M dwarf with a mass of (0.188 ± 0.014) M e and a radius of (0.234 ± 0.009) R e . The orbital period is (1.35121±0.00001) days. The secondary star is among the lowest-mass M dwarfs known to date. The binary has not reached a 1:1 spin-orbit synchronization. This indicates a young main-sequence binary with an age below ∼250 Myr. The mass-radius relation of both components are in agreement with this finding.

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Section: Modeling Of the Photometric And Radial Velocity Datamentioning

confidence: 99%

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

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“…This procedure used the method described in Brandt (1998) and the flowchart of Kallrath & Milone (1999).…”

Section: Numerical Code and Basic Assumptionsmentioning

confidence: 99%

International observational campaigns of the last two eclipses in EE Cephei: 2003 and 2008/9

Gałan

Mikołajewski

Tomov

et al. 2012

A&A

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Context. EE Cep is an unusual long-period (5.6 yr) eclipsing binary discovered during the mid-twentieth century. It undergoes almost-grey eclipses that vary in terms of both depth and duration at different epochs. The system consists of a Be type star and a dark dusty disk around an invisible companion. EE Cep together with the widely studied ε Aur are the only two known cases of long-period eclipsing binaries with a dark, dusty disk component responsible for periodic obscurations. Aims. Two observational campaigns were carried out during the eclipses of EE Cep in 2003 and 2008/9 to verify whether the eclipsing body in the system is indeed a dark disk and to understand the observed changes in the depths and durations of the eclipses. Methods. Multicolour photometric data and spectroscopic observations performed at both low and high resolutions were collected with several dozen instruments located in Europe and North America. We numerically modelled the variations in brightness and colour during the eclipses. We tested models with different disk structure, taking into consideration the inhomogeneous surface brightness of the Be star. We considered the possibility of disk precession. Results. The complete set of observational data collected during the last three eclipses are made available to the astronomical community. The 2003 and 2008/9 eclipses of EE Cep were very shallow. The latter is the shallowest among all observed. The very high quality photometric data illustrate in detail the colour evolution during the eclipses for the first time. Two blue maxima in the colour indices were detected during these two eclipses, one before and one after the photometric minimum. The first (stronger) blue maximum is simultaneous with a "bump" that is very clear in all the UBV(RI) C light curves. A temporary increase in the I-band brightness at the orbital phase ∼0.2 was observed after each of the last three eclipses. Variations in the spectral line profiles seem to be recurrent during each cycle. The Na i lines always show at least three absorption components during the eclipse minimum and strong absorption is superimposed on the Hα emission. Conclusions. These observations confirm that the eclipsing object in EE Cep system is indeed a dark, dusty disk around a low luminosity object. The primary appears to be a rapidly rotating Be star that is strongly darkened at the equator and brightened at the poles. Some of the conclusions of this work require verification in future studies: (i) a complex, possibly multi-ring structure of the disk in EE Cep; (ii) our explanation of the "bump" observed during the last two eclipses in terms of the different times of obscuration of the hot polar regions of the Be star by the disk; and (iii) our suggested period of the disk precession (∼11-12 P orb ) and predicted depth of about 2. m for the forthcoming eclipse in 2014.

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“…The derived e and ω are then related as follows (Kallrath & Milone 2009): e cos ω ≈ π (t s − t p − 1 2 )/(1 + csc 2 i) and e sin ω ≈ (Θ p − Θ s )/(Θ p + Θ s ). A lower limit for e may thus be estimated by assuming | cos ω| = 1.…”

Section: Non-zero Orbital Eccentricitymentioning

confidence: 99%

Luminosity Discrepancy in the Equal-Mass, Pre-Main-Sequence Eclipsing Binary Par 1802: Non-Coevality or Tidal Heating?

Chew

Stassun

Prša

et al. 2011

ApJ

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Parenago 1802, a member of the ∼1 Myr Orion Nebula Cluster, is a double-lined, detached eclipsing binary in a 4.674 day orbit, with equal-mass components (M 2 /M 1 = 0.985 ± 0.029). Here we present extensive VI C JHK S light curves (LCs) spanning ∼15 yr, as well as a Keck/High Resolution Echelle Spectrometer (HIRES) optical spectrum. The LCs evince a third light source that is variable with a period of 0.73 days, and is also manifested in the high-resolution spectrum, strongly indicating the presence of a third star in the system, probably a rapidly rotating Classical T Tauri star. We incorporate this third light into our radial velocity and LC modeling of the eclipsing pair, measuring accurate masses (M 1 = 0.391 ± 0.032 and M 2 = 0.385 ± 0.032 M ), radii (R 1 = 1.73 ± 0.02 and R 2 = 1.62 ± 0.02 R ), and temperature ratio (T eff,1 /T eff,2 = 1.0924 ± 0.0017). Thus, the radii of the eclipsing stars differ by 6.9% ± 0.8%, the temperatures differ by 9.2% ± 0.2%, and consequently the luminosities differ by 62% ± 3%, despite having masses equal to within 3%. This could be indicative of an age difference of ∼3 × 10 5 yr between the two eclipsing stars, perhaps a vestige of the binary formation history. We find that the eclipsing pair is in an orbit that has not yet fully circularized, e = 0.0166 ± 0.003. In addition, we measure the rotation rate of the eclipsing stars to be 4.629 ± 0.006 days; they rotate slightly faster than their 4.674 day orbit. The non-zero eccentricity and super-synchronous rotation suggest that the eclipsing pair should be tidally interacting, so we calculate the tidal history of the system according to different tidal evolution theories. We find that tidal heating effects can explain the observed luminosity difference of the eclipsing pair, providing an alternative to the previously suggested age difference.

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Eclipsing Binary Stars: Modeling and Analysis

Cited by 154 publications

References 2 publications

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

International observational campaigns of the last two eclipses in EE Cephei: 2003 and 2008/9

Luminosity Discrepancy in the Equal-Mass, Pre-Main-Sequence Eclipsing Binary Par 1802: Non-Coevality or Tidal Heating?

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