We present a review of highlights of our photometric and photo-polarimetric monitoring and mathematical modeling of interacting binary stars of different types classical, asynchronous, intermedi ate polars with 25 timescales corresponding to differ ent physical mechanisms and their combinations (part "Polar"); negative and positive superhumpers in nova-like and dwarf novae stars ("Superhumper"); symbiotic ("Symbiosis"); eclipsing variables with and without ev idence for a current mass transfer ("Eclipser") with a special emphasis on systems with a direct impact of the stream into the gainor star's atmosphere, which we propose to call "Impactors", or V361 Lyr-type stars. Other parts of the ILA project are "Stellar Bell" (pul sating variables of different types and periods - M, SR, RV Tau, RR Lyr, Delta Sct) and "New Variable".

Andronov, I. L.

Antoniuk, K. A.

Baklanov, A. V.

Breus, V. V.

Burwitz, V.

Chinarova, L. L.

Chochol, D.

Dubovsky, P. A.

Han, W.

Hegedus, T.

Henden, A.

Hric, L.

Kim, Chun-Hwey

Kim, Yonggi

Kolesnikov, S. V.

Kudzej, I.

Liakos, A.

Niarchos, P. G.

Oksanen, A.

Patkos, L.

Petrik, K.

Pit, N. V.

Shakhovskoy, N. M.

Virnina, N. A.

Yoon, J.

Zoła, Stanisław

Odessa Astronomical Publications

English

Jagiellonian Univeristy Repository

8 Odessa Astronomical Publications, vol. 23 (2010)”INTER-LONGITUDE ASTRONOMY” (ILA) PROJECT:CURRENT HIGHLIGHTS AND PERSPECTIVES.I. MAGNETIC VS. NON-MAGNETICINTERACTING BINARY STARSI.L.Andronov1,2, K.A.Antoniuk2, A.V.Baklanov2, V.V.Breus1,3, V.Burwitz4,L.L.Chinarova3, D.Chochol5, P.A.Dubovsky6, W.Han7, T.Hegedus8, A.Henden9,L.Hric5, Chun-HweyKim10, YonggiKim10,11, S.V.Kolesnikov3, I. Kudzej6,A. Liakos12, P.G.Niarchos12, A.Oksanen13, L. Patkos14, K. Petrik15, N.V.Pit’2,N.M. Shakhovskoy2, N.A.Virnina1, J. Yoon10, S. Zola16,171 Department ”High and Applied Mathematics”,Odessa National Maritime University, Odessa, Ukraine, tt ari@ukr.net2 Crimean Astrophysical Observatory, Nauchny, Ukraine3 Department of Astronomy and Research Institute ”Astronomical Observatory”,Odessa National University, Odessa, Ukraine4 Max-Planck Institut für Extra-Terrestische Physik, Garching, Germany5 Astronomical Institute of the Slovak Academy of Sciences, Stara Lesna, Slovakia6 Vihorlat Astronomical Observatory, Humenne, Slovakia7 Korea Astronomy and Space Science Institute, Daejeon, Korea8 Baja Astronomical Observatory, Baja, Hungary9 American Association of Variable Stars Observers, Harvard, USA10 University Observatory, Chungbuk National University, Cheongju, Korea11 Institute for Basic Science Research, Chungbuk National University, 361-63, Korea12 Department of Astrophysics, Astronomy and Mechanics, University of Athens, Greece13 Hankasalmi Observatory, Hankasalmi, Finland14 Konkoly Observatory, Hungarian Academy of Sciences, Budapest, Hungary15 Astronomical Observatory, Hlohovec, Slovakia16 Astronomical Observatory, Jagiellonian University, Cracow, Poland17 Mt. Suhora Observatory, Pedagogical University, Cracow, PolandABSTRACT. We present a review of highlights ofour photometric and photo-polarimetric monitoringand mathematical modeling of interacting binary starsof different types classical, asynchronous, intermedi-ate polars with 25 timescales corresponding to differ-ent physical mechanisms and their combinations (part”Polar”); negative and positive superhumpers in nova-like and dwarf novae stars (”Superhumper”); symbiotic(”Symbiosis”); eclipsing variables with and without ev-idence for a current mass transfer (”Eclipser”) with aspecial emphasis on systems with a direct impact ofthe stream into the gainor star’s atmosphere, which wepropose to call ”Impactors”, or V361 Lyr-type stars.Other parts of the ILA project are ”Stellar Bell” (pul-sating variables of different types and periods - M, SR,RV Tau, RR Lyr, Delta Sct) and ”New Variable”.Key words: Variable stars: cataclysmic, pulsating,eclipsing, interacting binaryThe monitoring of the first star of our sample AMHer was initiated by Prof. V.P.Tsessevich (1907-1983).More than 300 papers were published, with a totalnumber of studied variable stars exceeding 1400. Theprevious review of the ”Inter-Longitude Astronomy”(”ILA”) campaign was published by Andronov et al.(2003). For the CCD observations, we mainly use theBVRI calibration of A.Henden.Odessa Astronomical Publications, vol. 23 (2010) 9The ”top of the top” of the recent highlighs are:• TT Ari (nova-like superhumper): discoveries of aback switch between the states of positive and neg-ative superhumps (Andronov et al., 1999, 2005a);of a ”loop” at the ”Period of Quasi-Periodic Os-cillations (QPO) brightness”, contrary to a pre-vious suggestion on dependence of characteristicsof superhumps and QPOs on brightness (Kim etal., 2009); of drastic brightness variations up to2 mag during a prolonged exotic ”low luminositystate” started in October, 2009 and continued forone year, finished just before final version of thispaper, passing through stages (with increasing lu-minosity) of positive superhumps, double wave ofpositive superhumps; negative superhumps.• DO Dra (an ”outbursting intermediate polar”or a ”magnetic dwarf nova”): discoveries of thenew type of variability ”Transient Periodic Oscil-lations” (TPO), which are interpreted by modelof plasma blobs spiralling down to the magneticwhite dwarf; correlation of the decay rate and out-burst brightness; out-of-outburst luminosity vari-ations (Andronov et al., 2008);• V1432 Aql (asynchronous polar): discovery of athird type of eclipses in the system, self-consistentmodel for the arc-shaped accretion structure (An-dronov and Baklanov, 2007); determination of themost accurate value of the synchronization time of96.5 ± 1.5 years (Andronov and Baklanov, 2006)in an excellent agreement with former theoreticalprediction for another system AM Her with similarphysical parameters (Andronov, 1987ab);• AM Her (synchronous polar): Discovery of two-component nature of the ”shot noise” with char-acteristic time-scales of 9.8 and 170 sec basedon the 24117 seconds of CHANDRA observa-tions, which justifies the ”Z-pinch”-type magneto-hydrodynamic instability in falling plasma blobs”spaghetti” (Andronov et al., 2003, 2005b). Moredetailed self-review was published by Andronov(2008);• BY Cam (asynchronous polar): detailed study ofpreviously discovered switching of accretion frompole to pole with a phase of spin-orbital beat; cor-relation between the color index and brightness,which is an agreement with a cyclotron emissionof the accretion column (Andronov et al., 2008);detection of drastic changes of the amplitude ofvariations of polarization which may be explainedby variations of the accretion structure dependenton periodically changing angle between the line ofcenters and the magnetic axis (Breus et al., 2007);• Intermediate polars (BG CMi, MU Cam=1RXS J062518.2+733433, FO Aqr, AO Psc,1RXS J063631.9 +353537, 1RXS J070407.9+262501, 1RXS J180340.0 +401214, 1RXSJ192626.8 +132153, 1RXS J213344.1 +510725,PQ Gem, V405 Aqr): study of the rotational evo-lution of magnetic white dwarfs in these systemsbased on long-term monitoring; some systems ex-hibit acceleration (Andronov, Ostrova and Bur-witz, 2005) or deceleration (Kim et al., 2005) ofrotational acceleration (i.e. negative or positived2P/dt2), for interpretation of which a model ofprecession was proposed (Andronov, 2005); thestatistical dependence of phases of spin pulses onorbital phase was detected in MU Cam, indicat-ing modulation of the accretion structure with aperiodically changing angle between the magneticaxis and the line of centers (Kim et al., 2005);• OT J071126.0+440405 (synchronous polarwith 3 types of eclipses): discovery of 3 distinctlyseparate luminosity states based on 100+ nightsof mono and multi-color observations; determina-tion with best accuracy of the parameters of thelight curve; elaboration of self-consistent theoret-ical model for structure of the system, which isdependent on luminosity (i.e. the accretion rate);• Eclipsing nova-like variables (DW UMa, BHLyn, PX And, other SW Sex stars): besides su-perhumps and QPOs, they exhibit an ultra-violetexcess (seen in the U-B color index) at the eclipse(e.g. Andronov et al., 2001), indicating an ex-tended hot emission region (like an accretion diskcorona) and thus a physical unreliability of thindisk models;• Positive vs. Negative Superhumps in non-eclipsing Nova-Like variables: besides a large in-ternational campaign on TT Ari, we arrange oc-casional campaigns for V603 Aql. In 2004 the sys-tem was found to ehxibit either positive super-hump with a period 0.14813(10), or the statisti-cally significant waves with 3d9, 1d4, 0d135, whichmay be interpreted as the negative superhump-orbital, the beat periods (negative superhump -positive superhump) and the negative superhumpwith low amplitude, respectively (Andronov et al.,2005c). Similarly to TT Ari, another star MVLyr showed dependence of colors of variations withtime scale - the most “blue” spectral energy dis-tribution correspond to the quasi-periodic oscil-lations (QPO), the most “red” is time-averagedemission and the negative superhumps are inter-mediate in color temperature (Andronov and An-toniuk 2005). Using advanced methods for math-ematic modeling of multi-component signals, fromthe observations obtained during 6 nights follow-ing “the king of superoutbursts” in WZ Sge, wesucceeded to detect not only a orbital variablity10 Odessa Astronomical Publications, vol. 23 (2010)with prominent eclipses of the accretion disk, butalso “early superhumps”, which have become dom-inating only two weeks later (Andronov et al.,2002).• Symbiotic stars: photographic photometry andtime series analysis was made for dozens stars dur-ing an international campaign initiated by Hricand Skopal (1989). For recent studies of thesestars, we use different methods: periodogram,wavelet, scalegram analysis and global (polyno-mial + trigonometric polynomial fits) and local(running parabolae, running sine fits), see e.g. An-dronov and Chinarova (2003).• New Eclipsing and Pulsating variables: fromthe database of BV Hipparcos-Tycho observations,we have found 863 new variables (Andronov etal., 1999), the majority of which are eclipsing orpulsating variables. For such a study, we haveused trigonometric polynomial fits of 1, 2, 3 ordersand than specially developed algorithms of ”EAC”(”EA catcher”, which is effective for noisy obser-vations not only of the EA-type systems, but alsofor the types EB and EW) and ”RR Catcher” (An-dronov, Cuypers and Piquard, 2010). More thanfifty new variable stars were discovered, studiedand classified by N.Virnina. From those, 27 dis-coveries were reported separately in this volume(Virnina, 2010b). It should be noted that, fromthis sample, 10 systems (i.e. ∼ 37%) exhibit sta-tistically significant difference between the bright-ness at maxima arguing for a presence of spots.• VSX J052807.9+725606: discovery of largeasymmetry of the newly detected variable (Vir-nina, 2010a, Virnina and Andronov, 2010) with anamplitude increasing towards shorter wavelengths,which were interpreted in terms of the modelproposed for V361 Lyr (Andronov and Richter,1987), i.e. an extremely bright hot spot causedby a direct impact of an accretion stream fromthe donor to the accretor’s atmosphere at a pre-contact stage; this allows to propose a new classof ”Impactors”.ReferencesAndronov I.L.: 1987a, ApSS, 131, 557Andronov I.L.: 1987b, SvA, 31, 49Andronov I.L.: 2005, ASPC, 334, 447Andronov I.L.: 2008, JPhSt, 12, 2902Andronov I.L., Antoniuk K.A.: 2005,ASPC, 330, 505Andronov I.L., Antoniuk K.A., Augusto P., BaklanovA.V., Chinarova L.L., Chochol D., Efimov Yu.S.,Gazeas K., Halevin A.V., Kim Y., Kolesnikov S.V.,Kudashkina L.S., Marsakova V.I., Mason P.A.,Niarchos P.G., Nogami D., Ostrova N.I., Patkos L.,Pavlenko E.P., Shakhovskoy N.M., Tremko J.,Yushchenko A.V., Zola S.: 2003, AAT, 22, 793Andronov I.L., Antoniuk K.A., Breus V.V., ChinarovaL.L., Han Wonyong, Jeon Young Beom,Kim Yonggi, Kolesnikov S.V., Oh Joon Young,Pavlenko E.P., Shakhovskoy N.M.: 2008, CEJPh,6, 385Andronov I.L., Arai K., Chinarova L.L., DorokhovN.I., Dorokhova T.N., Dumitrescu A., NogamiD., Kolesnikov S.V., Lepardo A., Mason P.A.,Matsumoto K., Oprescu G., Pajdosz G., PassueloR., Patkos L., Senio D.S., Sostero G., SuleimanovV.F., Tremko J., Zhukov G. V., Zola S.,: 1999,AJ, 117, 574Andronov I.L., Baklanov A.V.: 2006, AA, 452, 941Andronov I.L., Baklanov A.V.: 2007, Ap, 50, 105Andronov I.L., Burwitz V., Reinsch K., Barwig H.,Chinarova L.L., Kolesnikov S.V., ShakhovskoyN.M., Hambaryan V., Beuermann K., YukhanovD.A.: 2003, OAP, 16, 7Andronov I.L., Burwitz V., Chinarova L.L., GazeasK., Kim Y., Niarchos P.G., Ostrova N.I., PatkosL., Yoon J.N.: 2005a, IBVS, 5664, 1Andronov I.L., Burwitz V., Reinsch K., Barwig H.,Chinarova L.L., Kolesnikov S.V., ShakhovskoyN.M., Hambaryan V., Beuermann K., YukhanovD.A.: 2005b, ASPC, 330, 407Andronov I.L., Chinarova L.L.: 2003, ASPC, 292, 211Andronov I.L., Chinarova L.L., Han W., Kim Y.,Yoon J.-N.: 2008, AA, 486, 855Andronov I.L., Cuypers J., Piquard S.: 2000, ASPC,203, 64Andronov I.L., Kolesnikov S.V., Niarchos P.G.,Shakhovskoy N.M., Zola S.: 2001, OAP, 14, 15Andronov I.L., Ostrova N.I., Burwitz V.: 2005, ASPC,335, 229Andronov I.L., Ostrova N.I., Kim Yong-Gi, BurwitzV.: 2005c, JASS, 22, 211Andronov I.L., Richter G.A.: 1987, AN, 308, 235Andronov I.L., Yushchenko A.V., Niarchos P.G.,Gazeas K.: 2002, ASPC, 261, 459Breus V.V., Andronov I.L., Kolesnikov S.V.,Shakhovskoy N.M.: 2007, AAT, 26, 241Hric L., Skopal A.: 1989, IBVS, 3364, 1Kim Y.G., Andronov I.L., Park S.S., Jeon Y.-B.: 2005,AA, 441, 663Kim Y., Andronov I.L., Cha S.M., Chinarova L.L.,Yoon J.N.: 2009, AA, 496, 765Kim Yong-Gi, Andronov I.L., Park Sung-Su,Chinarova L.L., Baklanov A.V., Jeon Young-Beom:2005, JASS, 22, 197Virnina N.A.: 2010a,http://sas.astro.sk/docs/bezpoz10eng3.pdfVirnina N.A.: 2010b, OAP, 23, 143Virnina N.A., Andronov I.L.: 2010, OEJV, 119, 1

"Inter-Longitude Astronomy" (ILA) project : current highlights and perspectives : I. Magnetic vs. non-magneticinteracting binary stars

Pit', N. V.

Zola, S.

Наукова періодика України

"INTER-LONGITUDE ASTRONOMY" (ILA) PROJECT: CURRENT HIGHLIGHTS AND PERSPECTIVES. I. MAGNETIC VS. NON-MAGNETIC INTERACTING BINARY STARS

https://ruj.uj.edu.pl/xmlui/bitstream/handle/item/76117/zola_et-al_inter-longitude_astronomy_ila_project_current_highlights_and_perspectives_2010.pdf?sequence=1&isAllowed=y

"Inter-Longitude Astronomy" (ILA) project : current highlights and perspectives : I. Magnetic vs. non-magneticinteracting binary stars

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