Peremennye Zvezdy

Publications

Section: PZ: main journal

Другое GSC 00143-00813, a New Triple-mode Classical Cepheid
PZ, vol. 42, N 7 (6.08.2022) | A. V. Khruslov / Tula, Russia | DOI

I present my detection of a new triple-mode Classical Cepheid, pulsating in the fundamental mode, first- and second-overtone modes. I analyzed all observations available for the star in the ASAS-SN and ZTF online public archives using the period-search software developed by Dr. V.P.~Goranskij for Windows environment. Light elements and parameters of the light curves for the three oscillations were obtained.


Другое Third Body in GSC 3937 2349, a New W UMa Variable
PZ, vol. 42, N 6 (30.06.2022) | I. M. Volkov / SAI, Moscow | DOI

The analysis of minima timings of the newly discovered W UMa variable GSC 3937 2349 (V=13.2m, P=0.2875d) revealed the light time effect that can be assigned to the third body in the system. Parameters of the third body orbit were derived and its mass was estimated, which turned out to be comparable to the mass of the components of the eclipsing system.


Другое A Study of Double-mode High-amplitude delta Scuti Variable Stars Pulsating in the Fundamental and First Overtone Modes. II
PZ, vol. 42, N 5 (14.06.2022) | A. V. Khruslov / Tula, Russia | DOI

I present a detection of 44 new double-mode high-amplitude delta Scuti variable stars, HADS(B) type, pulsating in the fundamental and first overtone modes. We analyzed all observations available for these stars in the ASAS-SN online public archive using the period-search software developed by Dr. V.P. Goranskij for Windows environment. Additionally, in individual cases, I used data of the SuperWASP, CSS, and ASAS-3 surveys. Light elements and parameters of the light curves of both oscillations were obtained.


Другое Photometric Elements, Apsidal Motion, Brightness Variations, and Light-time Effect in the Eclipsing Binary System V957 Cephei
PZ, vol. 42, N 4 (8.06.2022) | V. S. Kozyreva, A. V. Kusakin, A. Bogomazov, C. Omarov, A. Krylov | DOI

We obtained several light curves of V957 Cep in 2009, 2011, 2013, 2016, and 2019 at the Crimean Astronomical Station of M.V. Lomonosov Moscow State University and at the Tien Shan Observatory of the V.G. Fesenkov Astrophysical Institute. Using the TESS satellite observations, we found brightness variations of V957 Cep with the period P_p=0.664 d and amplitude A_p=0.0076 mag. For our light curves (2009-2019) and TESS light curves (2019-2020), orbital elements were computed and a new value of the apsidal motion rate d(omega)/dt=1.47 deg +/- 0.15 deg per year was derived. We found a possible light-time effect that can indicate gravitational influence of one or several additional bodies in the system on the central binary. Based on the currently available data, the amplitude and period of the light-time effect still cannot be reliably estimated.


Другое PZ Mon: Influence of Spots on Radial Velocity Measurements
PZ, vol. 42, N 3 (31.03.2022) | Y. Pakhomov, N. Gorynya | DOI

We present calculations of radial velocity corrections along the phase curve due to influence of the spotted surface of the active giant, PZ Mon. The maximum deviation from a relatively uniformly-bright stellar disk is about 0.20 - 0.25 km/s.


Другое An Attempt to Identify Classical Cepheid Candidates in the LAMOST Spectroscopic Survey
PZ, vol. 42, N 2 (22.02.2022) | D. Kovaleva, N. N. Samus, G. Zhao | DOI

We describe our attempt to find new candidate classical Cepheids and other pulsating variable stars in the LAMOST spectroscopic survey using GAIA EDR3 data and existing photometric archives. Several stars deserve dedicated photometric observations.


Другое V961 Cep: A New Eclipsing Variable with a delta Sct Component
PZ, vol. 42, N 1 (16.02.2022) | I. Volkov / SAI, INASAN | DOI

New observations of V961 Cep, an eclipsing star with elliptical orbit (P=7.04 d, V=10.14 m, e=0.03, F0 V+F5 V) revealed that its primary component was a delta Sct variable with the period P=0.0482603 d and a pulsation amplitude of 0.009 m in the V band.


Другое A Study of Double-Mode High-Amplitude Delta Scuti Variable Stars Pulsating in the Fundamental and First Overtone Modes. I
PZ, vol. 41, N 8 (24.12.2021) | A. V. Khruslov / Tula, Russia | DOI

I present a detection of 118 new double-mode high-amplitude Delta Scuti variable stars, HADS(B) type, pulsating in the fundamental and first overtone modes. We analyzed all observations available for these stars in the ASAS-SN online public archive using the period-search software developed by Dr. V.P. Goranskij for Windows environment. Additionally, in individual cases, I used data of the SuperWASP, CSS, ASAS-3, and NSVS surveys. Light elements and parameters of the light curves of both oscillations were obtained.


Другое The 84th Name-List of Variable Stars. Globular Clusters (Third Part) and Novae
PZ, vol. 41, N 7 (3.12.2021) | N. N. Samus, E. N. Pastukhova, O. V. Durlevich, E. V. Kazarovets, N. Kireeva | DOI

We present a new Name-List of variable stars containing information on 779 variable stars in globular star clusters (constellations Lynx - Ophiuchus; 27 clusters in 4 constellations) that now get their names in the system of the General Catalogue of Variable Stars (GCVS). Also, GCVS names are assigned to eleven recent Novae in our Galaxy. A correction to the 83rd Name-list of variable stars is announced.


Другое New Cataclysmic Variable in Pisces: A WZ Sge-subtype Star with Rebrightenings
PZ, vol. 41, N 6 (17.11.2021) | S. Shugarov, S. Malashevich | DOI

In September, 2021, we obtained about 1100 UBVRcIc CCD observations of the dwarf nova with coordinates RA=23h11m10.9s; Dec=+01deg30'03" (J2000) during its outburst. Our analysis of this photometric series showed that the studied variable star had superhumps at stage "B"; two rebrightenings were detected after the end of the outburst. The mass component ratio q = 0.06 was estimated; color temperature variations during the outburst were studied. The variable is a typical WZ Sge star with a short superhump period, 0.0516days. The detected period is close to the lower limit for the WZ Sge variables.


1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 | 10 | NextLast page ]

Main Page | Search
Astronet | SAI | INASAN

Report problems