Inter-Longitude Astronomy Project: Some Results and Perspectives

Андронов, И. Л.; Antoniuk, K.; Augusto, Pedro; Baklanov, A. V.; Chinarova, L. L.; Chochol, D.; Efimov, Yu. S.; Gazeas, K.; Halevin, A. V.; Kim, Y.; Колесников, С. В.; Kudashkina, L. S.; Marsakova, V. I.; Mason, Paul; Niarchos, P. G.; Nogami, Daisaku; Ostrova, N. I.; Patkos, L.; Павленко, Е. П.; Shakhovskoy, N. M.; Tremko, J.; Yushchenko, A. V.; Zoła, S.

doi:10.1080/1055679031000124501

Cited by 12 publications

(10 citation statements)

References 5 publications

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“…This article is a continuation of the work on the Atlas of the mean light curves and catalogue of the characteristics of the long-period variable stars (Kudashkina, 2003;Chinarova and Andronov, 2000;Marsakova and Andronov, 1998) and these works were done in a frame of activity of the "Ukrainian Virtual Observatory" (Vavilova et al, 2011(Vavilova et al, , 2012 and "Inter-Longitude Astronomy" (Andronov et al, 2003). The "Stellar Bell" (pulsating stars) part of this campaign was reported by Andronov et al (2014).…”

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confidence: 92%

The Mean Light Curves of the Mira-Type Stars in the H- And K-Bands

Kudashkina¹

2016

OAP

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Abstract. For nine Mira-type stars (o Cet, R Leo, S Car, U Her, X Oph, R Aql, RR Aql, S Ori, S Scl,) and one semi-regular star (L 2 Pup), the mean light curves have been obtained. The initial values of the brightness (observations) were fitted by a trigonometric polynomial of the statistically optimal order.The Fourier coefficients and the additional parameters (degree of the trigonometric polynomial, amplitude of the brightness, the maximal slope of ascending and descending branch, semi-amplitudes and initial epochs for the brightness maximum (minimum magnitude) of each harmonic contribution, etc., were given in the tables reported earlier (Kudashkina, 2015). In this study, we have received several interesting correlations between these parameters in the bands H and K. It was particularly noted the anomalous position on the figures of the star X Oph.The mean light curves of the investigated stars are commonly symmetric in the near infrared region (H and K).

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confidence: 92%

The Mean Light Curves of the Mira-Type Stars in the H- And K-Bands

Kudashkina¹

2016

OAP

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“…There are single-and multi-telescope projects on some selected stars. Among these projects, there is an international campaign ILA ("Inter-Longitude Astronomy", Andronov et al (2003)). The most recent review on highlights was presented by Andronov et al (2017).…”

Section: Introductionmentioning

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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“…In order to study the rotational evolution of magnetic white dwarfs in intermediate polars, a long time-base monitoring of the spin period variation is definitely needed. This object has been included in the list of key targets of the inter-longitude astronomy (ILA) project (Andronov et al 2003). As results of this project, deceleration and acceleration of the spin in the intermediate polars have already been detected: deceleration in BG CMi by Kim et al (2005b) and alternatively, acceleration in FO Aqr (Andronov et al 2005).…”

Section: Introductionmentioning

confidence: 99%