”asymptotic Parabola” Fits for Smoothing Generally Asymmetric Light Curves

Andrych, Kateryna D.; Андронов, И. Л.; Chinarova, L. L.; Marsakova, V. I.

doi:10.18524/1810-4215.2015.28.70612

Cited by 17 publications

(14 citation statements)

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“…Для зручностi використання рiзних методiв у однiй програмi, було створено комп'ютерну програму MAVKA, у яку поступово додавалися рiзноманiтнi функцiї [19][20][21].…”

Section: вступunclassified

“…[30,16] При зменшеннi ширини iнтервалiв та ''чистому" сигналi (без шуму), очiкується, що усi апроксимацiї будуть асимптотично сходитися до параболи (чи полiному бiльшого ступеня, найчастiше, кубiчної параболи). Можливiсть апроксимацiї полiномом iз автоматичним вибором ступеня полiнома була реалiзована на рiзних мовах програмування [6,13,19,21], й також присутня й у програм MAVKA. Але, кiлькiсть точок зменшується, та шуми спостережень призводять до появи ''нефiзичних" хвиль на апроксимацiї, що нагадує ефект Гiбса для тригонометричнiх полiномiв (напр.…”

Section: параболIчний сплайн дефекту 1 (Parabolic Spline Ps)unclassified

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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

Section: параболIчний сплайн дефекту 1 (Parabolic Spline Ps)unclassified

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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“…Also, we processed all available observations by using the symmetrical polynomial fit (Andrych et al, 2015). 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.…”

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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“…Four minima were determined from our CCDobservations by applying the symmetrical polynomial fit of statistically optimal degree (Andrych et al, 2016).…”

Section: Observations and O-c Analysismentioning

confidence: 99%

Improved Ephemeris of Poorly Studied Eclipsing Binary GSC 3950-00707 = 2mass J20355082+5242136

Savastru¹,

Marsakova

Andrych

et al. 2017

OAP

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ABSTRACT. We made our CCD-observations of GSC 3950-00707 by using the telescope Celestron-14 of Vihorlat Observatory and Astronomical Observatory on Kolonica Saddle. The moments of minima were calculated by using the symmetrical polynomial fit. We also analyzed the observations from automated surveys ASAS-SN and found 3 mean minima by using trigonometrical polynomial fit. The analysis of our observations and data from the surveys allows to conclude that it is the W UMa-type variable and its published period value is not accurate. We analyzed the O-C curve and corrected the elements.

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”asymptotic Parabola” Fits for Smoothing Generally Asymmetric Light Curves

Cited by 17 publications

References 1 publication

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

Improved Ephemeris of Poorly Studied Eclipsing Binary GSC 3950-00707 = 2mass J20355082+5242136

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