Please use this identifier to cite or link to this item:
|Title:||”Asymptotic parabola” fits for smoothing generally asymmetric light curves|
|Authors:||Andrych, K. D.|
Andronov, Ivan L.
Chinarova, L. L.
Marsakova, V. I.
|Citation:||Odessa Astronomical publications = Одесские астрономические публикации = Одеські астрономічні публікації|
|Publisher:||Одеський національний університет імені І. І. Мечникова|
|Keywords:||Stars: variable – stars|
binary – stars
cataclysmic – stars: pulsating
|Series/Report no.:||;Vol. 28, iss. 2.|
|Abstract:||A computer program is introduced, which allows to determine statistically optimal approximation using the "Asymptotic Parabola" fit, or, in other words, the spline consisting of polynomials of order 1,2,1, or two lines ("asymptotes") connected with a parabola. The function itself and its derivative is continuous. There are 5 parameters: two points, where a line switches to a parabola and vice versa, the slopes of the line and the curvature of the parabola. Extreme cases are either the parabola without lines (i.e.the parabola of width of the whole interval), or lines without a parabola (zero width of the parabola), or "line+parabola" without a second line. Such an approximation is especially effective for pulsating variables, for which the slopes of the ascending and descending branches are generally different, so the maxima and minima have asymmetric shapes. The method was initially introduced by Marsakova and Andronov (1996OAP.....9...127M) and realized as a computer program written in QBasic under DOS. It was used for dozens of variable stars, particularly, for the catalogs of the individual characteristics of pulsations of the Mira (1998OAP....11...79M) and semi-regular (200OAP....13..116C) pulsating variables. For the eclipsing variables with nearly symmetric shapes of the minima, we use a "symmetric" version of the "Asymptotic parabola". Here we introduce a Windows-based program, which does not have DOS limitation for the memory (number of observations) and screen resolution. The program has an user-friendly interface and is illustrated by an application to the test signal and to the pulsating variable AC Her.|
|Appears in Collections:||Odessa Astronomical Publications|
Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.