Peremennye Zvezdy


Section: PZ: main journal

Другое GSC 02693-00926 and USNO-B1.0 1587-0201409, Two New Doubly Eclipsing Systems
PZ, vol. 38, N 3 (23.05.2018) | A. V. Khruslov / Tula, Russia

I present my detection of two new doubly eclipsing systems, GSC 02693-00926 and USNO-B1.0 1587-0201409 (types EA+EB and EB+ELL). I analyzed all observations available for these stars in the NSVS and ASAS-SN online public archives using the period-search software developed by Dr. V.P. Goranskij for Windows environment. The light elements of both variations and the parameters of light curves are obtained.

Другое New Eclipsing Cataclysmic Variable Candidate in the Period Gap
PZ, vol. 38, N 2 (19.04.2018) | D. Panov, D. Denisenko

We report the discovery of a blue eclipsing variable Dan V1 in Sagittarius with the orbital period P=0.094277 days (2.2626 hours). The object is also an UV source, indicating the presence of a white dwarf in the binary system. We consider two possibilities: a cataclysmic (nova-like) variable and an eclipsing hot subdwarf of the HW Vir type. Our analysis favors the first (CV) scenario. If confirmed, Dan V1 is a very rare eclipsing cataclysmic variable in the period gap.

Другое A Study of Double-Mode Variables
PZ, vol. 38, N 1 (13.04.2018) | A. V. Khruslov / Tula, Russia

I present a detection of 44 new double-mode variable stars, of which 25 variables are high-amplitude Delta Scuti stars, HADS(B) type, and 19 stars are RR Lyrae variables, RR(B) type. For two of the HADS(B) stars, their detection was the variability discovery. We analyzed all observations available for these stars in the Catalina Surveys and SuperWASP online public archives using the period-search software developed by Dr. V.P. Goranskij for Windows environment. In two cases, we also used data of the ASAS-SN archive. According to these data, one star, GSC 02900-00317, is possibly pulsating in the first- and second-overtone modes; the other stars are pulsating in the fundamental and first-overtone modes.

Другое Novae in 2015 - 2017: Official Announcement of GCVS Names
PZ, vol. 37, N 4 (29.12.2017) | E. V. Kazarovets, N. N. Samus

GCVS names are announced for 20 galactic Novae discovered in 2015 - 2017.

Другое A Photometric Study of GSC 01374-01131, a HADS Variable Star with an Eclipsing Component
PZ, vol. 37, N 3 (12.10.2017) | A. V. Khruslov, R. I. Kokumbaeva, A. V. Kusakin, I. Reva

We present the results of our new observations of GSC 01374-01131, a recently discovered high-amplitude delta Scuti (HADS) star for which, in 2013, we detected an eclipsing component of the light curve in the Catalina Surveys data. We acquired new CCD photometry in Johnson's B, V, and R bands for this star, improved the periods of the eclipses (P_e = 5.96857 days) and of the pulsation (P_p = 0.08494573 days) and other parameters of the light curves. GSC 01374-01131 is an eclipsing binary of the Algol type (EA); one of its components is a pulsating HADS star. Currently, GSC 01374-01131 has the lowest depth of the main eclipse (A_e = 0.13 mag) among all known HADS stars in eclipsing binary systems, comparable to the observed pulsation amplitude.

Другое Photometric Observations of Supernovae 2011df, 2011ek and 2012ea
PZ, vol. 37, N 2 (6.10.2017) | D. Y. Tsvetkov, N. Pavlyuk, V. Lipunov, E. Gorbovskoy, V. V. Krushinsky

CCD BVRI photometry is presented for two type Ia supernovae, SN 2011df and 2011ek, and for a supernova of type Ia-1991bg, SN 2012ea. The light curve parameters and absolute magnitudes at maximum light are estimated. It is shown that SNe 2011df and 2012ea are typical for their classes considering the shape of their light curves and maximum luminosity. SN 2011ek shows some properties of 1991bg-like supernovae: red color at maximum and low luminosity, but the shape of the light curves is typical of normal SNe Ia.

Другое Unusual Short-period Cepheid with a Prominent Bump
PZ, vol. 37, N 1 (8.06.2017) | D. Denisenko / IKI

I report my discovery of a peculiar short-period Type II Cepheid in Centaurus. The new variable is pulsating with the period of 2.918 days, yet it is showing a distinctly double-peaked light curve with two nearly equal maxima. The "bumps" are normally observed in long-period Cepheids with periods ranging from 6 to 16 days, but there are exceptions for stars with shorter P values. The new variable resides in the halo, more than 3 kpc above the Galactic plane, and belongs to population II Cepheids of the BL Her type (CWB).

Другое Cataclysmic and RCB Type Candidates for Identification of Three Suspected Variables
PZ, vol. 36, N 2 (23.12.2016) | E. V. Kazarovets

I report the discovery of two cataclismic variable stars as probable candidates for identification of the Luyten's variable HV 9251 (NSV 10231) and Wolfs' object AN 115.1905 (NSV 12542). I also suggest the possible RCB variability type for Hoffmeister's star S 9384 (NSV 11988).

Другое MASTER OT J190519.41+301524.4: A New Eclipsing Cataclysmic Variable of the VY Scl Type
PZ, vol. 36, N 1 (18.11.2016) | F. Martinelli, D. Denisenko

MASTER OT J190519.41+301524.4 was discovered as a 15m.7 optical transient by the Mobile Astronomical System of TElescope-Robots (MASTER) in March, 2014. We report the results of photometric observations of this variable performed at the Lajatico Astronomical Center in June - July, 2015. The light curve shows deep V-shaped eclipses with an amplitude of two magnitudes. The orbital period was determined to be 0d.129694 (3h.113). Based on the archival observations and the shape of the orbital curve, we suggest that MASTER OT J190519.41+301524.4 is a new cataclysmic variable of VY Scl type ("anti-nova"), with an inclination angle close to 90 degrees.

Другое New RRC variables with an additional non-radial pulsation
PZ, vol. 35, N 5 (11.12.2015) | A. V. Khruslov / Tula, Russia

We present a new study of 14 known RR Lyrae variable stars from the Catalina surveys periodic variable star catalog. We analyzed all observations available for these stars in the Catalina Surveys online public archives using the period-search software developed by Dr. V.P. Goranskij for Windows environment. According to these data, the stars are RRC variables with an additional non-radial pulsation.

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