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Study of variable stars associated with maser sources: g025.65+1.05

Research in Astronomy and Astrophysics 2019年第3期19卷 47-52页

作者： Andrey M.Sobolev Anastasia P.Bisyarina Stanislav Yu.gorda Andrey M.tatarnikov Astronomical Observatory of the Ural Federal University Sternberg Astronomical Institute of Moscow State University

We report variation of K-band infrared(IR) emission in the vicinity of the g025.65+1.05 water and methanol maser source. New observational data were obtained with the 2.5 m telescope at the Caucasian Mountain Observatory(CMO) of Moscow State University on 2017–09–21 during a strong water maser flare. We found that the IR source situated close to the maser position had decreased brightness in comparison to archive data. This source is associated with a massive young stellar object(MYSO) corresponding to the compact IR source IRAS 18316–0602(RAFgL 7009 S). A similar decrease in K-brightness of the IR source close to the maser position was observed in March 2011 when the water maser experienced a period of increased activity. The dips in MYSO brightness can be related to the maser flare phases. Maser flares that are concurrent with dips in the IR emission can be explained if the lower IR radiation field enables a more efficient sink for the pumping cycle by allowing IR photons to escape the maser region.

关键词： techniques photometric-infrared stars-masers

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Spectroscopic and photometric observations of symbiotic nova PU Vul during 2009–2016

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Research in Astronomy and Astrophysics 2018年第8期18卷 83-88页

作者： Anna tatarnikova Marina Burlak Eugene Kolotilov Natalia Metlova Victor Shenavrin Sergei Shugarov Taisija Tarasova Andrey tatarnikov Sternberg Astronomical Institute Moscow State UniversityMoscow 119234Russia Astronomical Institute of the Slovak Academy of Sciences 05960 Tatranska LomnicaSlovakia Federal State Budget Scientific Institution"Crimean Astrophysical Observatory of RAS" Nauchny298409Russia

A new set of low-resolution spectral and UBVJHKL-photometric observations of the symbi- otic nova PU Vul is presented. The binary has been evolving after its symbiotic nova outburst in 1977 and now it is in the nebular stage. It is found that the third orbital cycle （after 1977） was characterized by great changes in associated light curves. Now, PU Vul exhibits a sine-wave shape in all the light curves （with an amplitude in the U band of about 0.7 mag）, which is typical for symbiotic stars in the quiescent state. Brightness variability due to pulsations of the cool component is now clearly visible in the VRI light curves. The amplitude of the pulsations increases from 0.5 mag in the V band to 0.8 mag in the I band. These two types of variability, as well as a very slow change in the physical parameters of the hot component due to evolution after the outburst of 1977, influence the spectral energy distribution （SED） of the system. The variability of emission lines is highly complex. Only hydrogen line fluxes vary with orbital phase. An important feature of the third orbital cycle is the first emergence of the OVI, 6828A Raman scattering line. We determine the temperature of the hot component by means of the Zanstra method applied to the He II, 4686A line. Our estimate is about 150000 K for the spectrum obtained near orbital maximum in 2014. The VO spectral index derived near pulsation minimum corresponds to M6 spectral class for the cool component of PU Vul.

关键词： binaries symbiotic - novae - cataclysmic variables - stars individual (PU Vul)

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Photometric and Spectroscopic Analysis of LBV Candidate J004341.84+411112.0 in M31

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Research in Astronomy and Astrophysics 2022年第1期22卷 237-244页

作者： A.Sarkisyan Sholukhova Fabrika A.Valeev A.Valcheva P.Nedialkov A.Tatamikov Special Astrophysical Observatory of Russian Academy of Sciences Niznij Arkhyz 369167Karachai-CherkessiaRussia Crimean Astrophysical Observatory Russian Academy of SciencesNauchnyi 298409Russia Department of Astronomy Sofia University5 J.Bourchier BlvdSofia 1164Bulgaria Sternberg Astronomical Institute Moscow M.V.Lomonosov State UniversityUniversitetskiy Prospekt 13Moscow 119234Russia

We study Luminous Blue Variable(LBV)candidate J004341.84+411112.0 in the Andromeda *** present optical spectra of the object obtained with the 6 m telescope of BTA SAO *** candidate shows typical LBV features in its spectra:broad and strong hydrogen lines and the He I lines with P Cygni *** remarkable spectral resemblance to the well known LBV P Cygni suggests a common nature of the objects and supports LBV classification of J004341.84+*** estimate the temperature,reddening,radius and luminosity of the star using its spectral energy *** bolometric luminosity of the candidate(M_(bol)=-10.41±0.12 mag)is quite similar to those of known LBV stars in the Andromeda *** analyzed a ten year light curve of the object in R *** candidate demonstrates photometric variations of the order of 0.4 mag,with an overall brightness increasing trendΔR>0.1 ***,the corresponding color variations of the object are fully consistent with LBV behavior when a star become cooler and brighter in the optical spectral range with a nearly constant bolometric ***-type variability of the object,similarity of its spectrum and estimated luminosity to those of known LBVs allow us to classify J004341.84+411112.0 as an LBV.

关键词： stars:early-type stars:massive stars:variables:S Doradus stars:Wolf Rayet techniques:photometric techniques:spectroscopic galaxies:individual(KIC 8098300)

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