The similarity of the H line in the spectra of different types of active stars Seminar at AP Krakow, November 29 2005 D. Kjurkchieva & D. Marchev We all should be proud that the whole Chapter 5 of the Manual of the new educational and scientific software Binary Maker 3 bases on the paper “Spectroscopic and photometric observations of the short period RS CVn star RT And” (Kjurkchieva, Marchev, Ogloza, 2001, A & A 378, 102).

The beginning of Chapter 5 of the Binary Maker 3 Manual The photometric observations of RT And are made by two-channel electrophotometer mounted on the 60-cm telescope of Mt. Suhora observatory (Poland) The beginning of Chapter 5 of the Binary Maker 3 Manual

V light curve of RT And shown in the The high quality V light curve of RT And shown in the Binary Maker 3 Manual

The spectral observations of RT And are made at National Astronomical Observatory (Bulgaria)

The modeling of the photometric and spectral data were made during the stay of DK & DM at Mt. Suhora Observatory in 2001 by the loved spots … as usually ….

If you open the Catalog and Atlas of Eclipsing Binaries of Binary Maker 3 you will see that the first star in the list is RT And and … the references is to our paper - result of our collaboration

The results of our cooperation since 1987 I. RS CVn stars Pajdosz G., Kjurkchieva D., Zola S., 1989, IBVS No 3292 “UBV photometry of II Peg during October 1988” Kjurkchieva D., Marchev D., Ogloza W., 2000, A & A 354, 909, “Multicolor high-speed photometry and H spectroscopy of XY UMa” Kjurkchieva D., Marchev D., Ogloza W., 2000, AcA 50, 517, “Multicolor photometry of SV Cam in 1997” Kjurkchieva D., Marchev D., Ogloza W., 2001, A & A 378, 102, “Spectroscopic and photometric observations of the short period RS CVn star RT And” Kjurkchieva D., Marchev D., Zola S., 2002, A & A 386, 548, “Spectroscopic observations of the short period RS CVn star SV Cam” Kjurkchieva D., Marchev D., Ogloza W., 2003, A & A 400, 623, “Spectroscopic and photometric observations of the short period RS CVn star CG Cyg” Kjurkchieva D., Marchev D., Zola S., 2003, A & A 404, 611, “Spectroscopic and photometric observations of the short period RS CVn star ER Vul” Kjurkchieva D., Marchev D., Ogloza W., 2004, A & A 415, 623, “Spectroscopic and photometric observations of the short period RS CVn star WY Cnc”

II. The cataclysmic stars Kjurkchieva D., Marchev D., Ogloza W., 1997, Ap & SS 250, 261, “Multicolor photometry of RX And during 1994/95” Kjurkchieva D., Marchev D., Ogloza W., 1998, Ap & SS 262, 53, “High-speed BVRI photometry of SS Cyg at quiescence and outburst” Kjurkchieva D., Marchev D., Drozdz M., 1998, Ap & SS 262, 453, “Multicolor photometry of AM Her during 1994-96” Kjurkchieva D., Marchev D., Ogloza W., 1999, AcA 49, 585, “H observations of SSCyg at quiescence and outburst”

III. The W UMa stars CN And W UMa V1130 Tau V353 Peg V357 Peg BB Peg Kreiner J. et al., 2003, A&A 412, 465, “Physical parameters of components in close binary stars. I” Contribution in the photometric observations of the stars: CN And W UMa V1130 Tau V353 Peg V357 Peg BB Peg ET Boo V357 And FG Hya V776 Cas

Results from the last paper on FK Com Kjurkchieva D. , Marchev D Results from the last paper on FK Com Kjurkchieva D., Marchev D., 2005, A & A 434, 221, “H observations of the star FK Com” The spectra averaged in phase bins and the mean spectrum The individual spectra minus the mean spectrum

The main problem – single or double star is FKCom The main problem – single or double star is FKCom? The residuals of the individual spectra and the mean spectrum at the characteristic phase give information about the position of the sources of additional emission and absorption There is a bulk of emission and bulk of absorption at phase 0.25; There are additional sources of the emission and absorption that move in opposite directions in respect to the observer (best visible at phases 0.25 and 0.75); The contribution of the source of additional emission is larger than that of the additional absorption; The whole analysis leads to the conclusion that these two sources moves in anti-phase during the whole cycle.

The similarity of the H profile of FK Com and cataclysmic star UX UMa in intensity, width and position of the emission peaks Our model of the FK Com H emission configuration main star - source of the absorption reversal extended half-illuminated disk - source of the emission peaks SAE – source of the additional emission SAA - source of the additional absorption secondary star – source of the illumination of the disk FK Com = double star

Results from the investigation of UV Leo Kjurkchieva D. , Marchev D Results from the investigation of UV Leo Kjurkchieva D., Marchev D., 2005, A&A submitted, “New spectroscopic solution of the star UV Leo” The main problem: which of the star components is larger? H observations with S/N≈100 Fitting the profiles by two gaussians for measuring of the radial velocities New spectroscopic solution  determination of star masses and q From the measured rotational broadenings  equatorial velocities and star radii

Conclusions: - The more massive star is bigger in size - The two components are oversized for their masses - The two star lie within the MS band on the mass-radius diagram, close to the isochrone 9x1010yrs, develop convective envelopes and move to the TAMS

Results from the investigation of EM Cep Kjurkchieva D. , Marchev D Results from the investigation of EM Cep Kjurkchieva D., Marchev D., “Photometric and Ha observations of the star EM Cep” (in preparation) The main questions Single or double star is EM Cep? Is there some phase variability of the spectra? Spectroscopic observations at Be state in 2004 (H in emission) and B state in 2005 (H in absorption)

Тhe H profiles at Be and B state differ but their full widths and depths are almost the same It look as the emission wings at Be state convert to absorption at B state

The two type of light curves with exchanging places of the two minima Standstill at phase 0.83 in 2004 - indication of alternation between two states??? Which is the mechanism of alternation? Forthcoming attempt for fitting of the light curves

The irregular times of the minima  O-C=0 The irregular times of the minima  O-C=0.01d for a couple of days Confirmation of secular linear decreasing of the period

Similarity of the H profile of EM Cep with that of disk-like star FK Com in: a) positions of the emission peaks b) whole width

Search for a variability of the spectra The subtracted spectra (individual minus spectrum at phase 0.47)  central ADEM and two ADABS The subtracted H profile s mirror image of real H profile at Be state

The subtracted spectra (individual spectrum minus the spectrum at phase 0.48) at Be state show only ADEM around quadratures

Warning! The coincidence of the H profiles and the difference of the position and width of the HeI line at phases 0.75-0.82 and 0.47 The same effect at phase range 0.19-0.23 Is this an indication of the contribution of the secondary star?

The radial velocities of the two ADABS show the opposite motion of their sources with velocity equal to the star rotational velocity  The ADABS compensate ADEM at minima  The sources of ADABS are near the star surface The angle between the line-of-sight and star rotational axis is small

Main results It is found an indication of the alternation between the two types of light curves (with exchanging minima) Confirmation of secular linear decreasing of the period The phase variability of the spectra at Be and at B state are investigated It is found difference of the position and width of the HeI line in respect to H at phase ranges 0.75-0.82 and 0.19-0.23 It is established opposite motion of two sources of ADABS with velocities equal to star rotation velocity  sources of ADABS are near (or on) star surface The angle between the line-of-sight and star rotational axis is small Such a configuration with two opposite sources of ADABS can explain the sinusoidal light variability

Open questions Why the H emission peaks in the spectra of different types objects (Be stars, FK Com stars, cataclysmic stars) have the same velocities? Why the full width of the H line in the spectra of different types objects (Be stars, FK Com stars, cataclysmic stars) are the same? Do the foregoing facts mean that there is some mechanism of creating of similar gaseous structure with almost equal velocities in the different types of stars?

Future cooperation We expect your suggestions about joint projects (educational and scientific) We propose to sign an official contract between departments of physics of AP and SU We would like to continue our collaboration in the future

Conclusion So… stars, disks, spots and people, mainly people and friends… …Heavy winter, snow, slippery and broken bus… …And three friends pass through the border to help us… We will remember this always! To our polish colleagues and true friends with large appreciation and love!!!