Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Андронов, И. Л.; Kim, Yonggi; Kim, Young‐Hee; Yoon, Joh-Na; Chinarova, L. L.; Tkachenko, Mariia G.

doi:10.5140/jass.2015.32.2.127

Cited by 8 publications

(7 citation statements)

References 35 publications

(40 reference statements)

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“…The second-order trigonometrical polynomial is typically sufficient to describe the effects of reflection, ellipticity and asymmetry (O'Connell effect), and the H− functions describe the shapes of the minima, with a parameter β, which is generally different for the primary (β 1 = C 2 ) and secondary (β 2 = C 3 ) minima. Generally, there may be a shift φ 0 = C 4 .. Phenomenological modeling of multi-color observations of a newly discovered eclipsing binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331 is presented in [11]. In Fig.…”

Section: The Methods Of Calculations: the Nav Algorithmmentioning

confidence: 99%

The structure of the test function for the phenomenological modelling of eclipsing binaries

Tkachenko¹

2016

Adv.Astron.Spa.Physics

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The dependence of the test function on the phenomenological parameters used in the "NAV" ("New Algol Variable") algorithm (Andronov, 2012Ap.....55..536A) is studied. Due to a presence of local minima, the method of minimization contains two steps: the "brute force" minimization at a grid in the 4D parameter space, and further iterations using the differential corrections. This method represents an effective approximation of the light curve using the special pattern (shape) separately for the primary and secondary minima. The application of the method to concrete stars is briefly reviewed.

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Section: The Methods Of Calculations: the Nav Algorithmmentioning

confidence: 99%

The structure of the test function for the phenomenological modelling of eclipsing binaries

Tkachenko¹

2016

Adv.Astron.Spa.Physics

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“…Для виявлення повiльних змiн перiоду та амплiтуди, часто використовують вейвлет-аналiз (wavelet analysis) [44][45][46], який iнодi називають ''спалах-аналiз" та його модифiкацiю -"ковзаючi синуси" (Running Sine, RS) [47]. Комбiнацiя тригонометричного полiнома iз локальним профiлем затемнення [48][49][50] теж не ефективна для розглянутого типу коливань, як i визначення "характерних точок", як перетину постiйного рiвня [51][52].…”

Section: Iншi методи аналIзу спостережень пульсуючої зорI Z Umaunclassified

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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“…For another eclipsing binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331 (currently named as V1517 Her) in the field of the intermediate polar V1323 Her, Andronov et al (2015) estimated physical parameters of the components, using two-color photometry and a statistical mass-radius-color index relation.…”

Section: Phenomenological Modellingmentioning

confidence: 99%

Poorly Studied Eclipsing Binaries in the Field of DO Dra: V0455 Dra and V0454 Dra

Kim,

Andronov,

Andrych

et al. 2020

Preprint

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We report an analysis of two poorly studied systems GSC 04396-00605 and GSC 04395-00485, which were recently named as V0455 Dra and V0454 Dra, respectively. For two eclipsing stars, the periods and epochs were significantly corrected using our extensive data. The phenomenological characteristics of the mean light curves were determined using the New Algol Variable (NAV) algorithm. The individual times of Maxima/Minima (ToM) were determined using the newly developed software MAVKA, which outputs the accurate parameters using the "asymptotic parabola" approximations. The light curves were approximated using the Wilson-Devinney model, the best fit parameters are listed. For both systems, the presence of the dark spot is justified, the parameters are estimated. Both systems classified to be overcontact binaries of EW type. The observations were obtained using the 1-m Korean telescope of the LOAO while monitoring the cataclysmic variable DO Dra within the Inter-Longitude Astronomy" (ILA) project.

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Phenomenological Modeling of Newly Discovered Eclipsing Binary 2MASS J18024395 + 4003309 = VSX J180243.9+400331

Cited by 8 publications

References 35 publications

The structure of the test function for the phenomenological modelling of eclipsing binaries

The structure of the test function for the phenomenological modelling of eclipsing binaries

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

Poorly Studied Eclipsing Binaries in the Field of DO Dra: V0455 Dra and V0454 Dra

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