Comparative Analysis of Phenomenological Approximations for the Light Curves of Eclipsing Binary Stars with Additional Parameters

Андронов, И. Л.; Tkachenko, Mariia G.; Chinarova, L. L.

doi:10.1007/s10511-017-9462-0

Cited by 8 publications

(6 citation statements)

References 19 publications

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“…Сплайни iз змiнним ступенем були запропонованi [13], якi виправляли проблему "нефiзичних" хвиль на апроксимацiях полiномами. Огляди iснуючих методiв приведенi [15][16][17][18].…”

Section: вступunclassified

MAVKA: Program of statistically optimal determination of phenomenological parameters of extrema. Parabolic spline algorithm and analysis of variability of the semi-regular star Z UMa

Andrych¹,

Андронов²,

Chinarova³

2020

J. Phys. Stud.

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the difference between the 0.975 and 0.025 percentiles (divided by 2*1.96) as the accuracy estimate of a given parameter in the bootstrap method. The variability of the semi-regular pulsating star Z UMa is analyzed. The presence of multicomponent variability of an object, including, four periodic oscillations (188.88(3), 197.89(4) days and halves of both) and significant variability of the amplitudes and phases of individual oscillations are shown. Approximation using the parabolic spline is only slightly better than the asymptotic parabola, for our sampling of the complete interval. It is expectedly better for larger subintervals. The use of different complementary methods allows to get a statistically optimal phenomenological approximation.

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Section: вступunclassified

MAVKA: Program of statistically optimal determination of phenomenological parameters of extrema. Parabolic spline algorithm and analysis of variability of the semi-regular star Z UMa

Andrych¹,

Андронов²,

Chinarova³

2020

J. Phys. Stud.

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“…That procedure was done for our own observations and those taken from the AAVSO database or from the NSVS, if there was not enough data in AAVSO. Phenomenological modeling of eclipses was reviewed by Andronov, Tkachenko & Chinarova (2017).…”

Section: Observational Data and Moments Of Minimamentioning

confidence: 99%

Effects of the Mass Transfer and Presence of the Third Components in Close Binary Stellar Systems

Tvardovskyi¹,

Marsakova²,

Андронов³

2017

OAP

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In our research, we have studied 6 close binary stellar systems which are eclipsing variables of β Lyrae and W Ursae Majoris types of variability. We have studied their O-C curves. To build them, we used moments of minima, listed in the BRNO database. Also, we used ones, which we obtained as the result of processing of observational data taken from AAVSO database. As the result of the O-C analysis, we detected that all of these stars have parabolic O-C curves, which might be caused by mass transfer from one component to another. In an addition, 3 from researched stars (U Peg, V0523 Cas and WZ Cyg) have superimposed parabolic and cyclic O-C changes that could be caused by presence of the third components in the systems. Also, we calculated minimal possible masses of third components, rates of the mass transfer for these systems and corrected the ephemerides.

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“…As the shape parameters β are often equal to the minimal limit 1.5 for the examined stars, as well as for the previously studied stars, we have applied approximations with additional parameters. The dozens of modified functions were tested by [17], [18]. In Figure 4, there are shown the part of the approximation near the primary minimum with the main set of parameters listed in Table 1, as well as modifications.…”

Section: Improved Approximationsmentioning

confidence: 99%

“…This triangle makes an apparent enlarging of the eclipse depth, however, which is not statistically different from the previous approximation. Another modification was found to be the best by [18]. It redefines z in Eq.…”

Section: Improved Approximationsmentioning

confidence: 99%

Phenomenological parameters of the prototype eclipsing binaries Algol, β Lyrae and W UMa

Tkachenko¹,

Андронов²,

Chinarova³

2016

J. Phys. Stud.

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The phenomenological parameters of eclipsing binary stars, which are the prototypes of the EA, EB and EW systems are determined using the expert complex of computer programs, which realizes the NAV ("New Algol Variable") algorithm (Andronov , 2012 and its possible modifications are discussed, as well as constrains for estimates of some physical parameters of the systems in a case of photometric observations only, such as the degree of eclipse, ratio of the mean surface brightnesses of the components. The half-duration of the eclipse is 0.0617 (7), 0.1092(18) and 0.1015 (7) for Algol, β Lyrae and W UMa, respectively. The brightness ratio is 6.8±1.0, 4.9±1.0 and 1.15±0.13. These results show that the eclipses have distinct begin and end not only in EA (as generally assumed), but also in EB and EW -type systems as well. The algorithm may be applied to classification and study of the newly discovered (or poorly studied) eclipsing variables based on own observations or that obtained using photometric surveys.

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Comparative Analysis of Phenomenological Approximations for the Light Curves of Eclipsing Binary Stars with Additional Parameters

Cited by 8 publications

References 19 publications

MAVKA: Program of statistically optimal determination of phenomenological parameters of extrema. Parabolic spline algorithm and analysis of variability of the semi-regular star Z UMa

MAVKA: Program of statistically optimal determination of phenomenological parameters of extrema. Parabolic spline algorithm and analysis of variability of the semi-regular star Z UMa

Effects of the Mass Transfer and Presence of the Third Components in Close Binary Stellar Systems

Phenomenological parameters of the prototype eclipsing binaries Algol, β Lyrae and W UMa

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