The similarity of the HThe similarity of the H line in the spectra of line in the spectra of different types of active starsdifferent types of active stars

Seminar at AP Krakow, November 29 2005Seminar at AP Krakow, November 29 2005D. Kjurkchieva & D. MarchevD. 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 3Binary Maker 3 bases on the paper

“Spectroscopic and photometric observations of the short period RS CVn Spectroscopic and photometric observations of the short period RS CVn star RT Andstar RT And”

(Kjurkchieva, Marchev, Ogloza, 2001, A & A 378, 102).

The photometric observations of RT AndRT And are made by two-channel electrophotometer

mounted on the 60-cm telescope of Mt. Suhora Mt. Suhora observatoryobservatory (Poland)

The beginning of Chapter 5 of the Binary Maker 3 Manual

The high quality V light curve of

RT AndRT And shown in the

Binary Maker 3 Binary Maker 3 ManualManual

The spectral observations

of RT AndRT And are made at National National

Astronomical Astronomical ObservatoryObservatory (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 the loved spots …… as usuallyas usually …. ….

If you open the

Catalog and Catalog and Atlas of Atlas of

Eclipsing Eclipsing Binaries Binaries

of of Binary Maker 3Binary Maker 3

you will see that the first star in

the list is RT AndRT And and … the references

is to our paper - result of our

collaboration

The results of our cooperationThe results of our cooperationsince 1987

I. RS CVn starsRS 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 starsThe 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 starsThe W UMa stars

• 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 AndW UMa V1130 TauV353 PegV357 Peg

BB PegET BooV357 AndFG HyaV776 Cas

Results from the last paper on FK ComResults from the last paper on FK ComKjurkchieva 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 ComFK Com and cataclysmic star UX UMaUX UMa in intensity, width and position of the emission peaks

Our model of the FK ComFK Com H emission configurationmain star - source of the absorption reversalextended 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 ComFK Com = = double stardouble star

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 CepKjurkchieva D., Marchev D., “Photometric and Ha observations of the star

EM CepEM Cep” (in preparation)

The main questions The main questions Single or double Single or double star is EM Cep?star is EM Cep? Is there some Is there some

phase variability phase variability of the spectra?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 - indicationindication of alternation between of alternation between two states??? two states???

Which is the mechanism of alternation?Which is the mechanism of alternation?

Forthcoming attempt for fitting of the light curves

The irregular times of the minima O-C=0.01d for a couple of daysConfirmation 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 Search for a variability of the spectraspectra

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!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 0.47The 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 radial velocities of the two ADABS show the two ADABS show

the opposite motion of the opposite motion of their sources with their sources with

velocity equal to the velocity equal to the star rotational velocitystar rotational velocity

The ADABS The ADABS compensate ADEM at compensate ADEM at

minimaminima The sources of The sources of

ADABS are near the ADABS are near the star surfacestar surface

The angle between The angle between the line-of-sight and the line-of-sight and star rotational axis is star rotational axis is

smallsmall

Main resultsMain 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 The angle between the line-of-sight and star rotational axis is smallsmall

• Such a configuration with two opposite sources of ADABS can explain the sinusoidal light variability

Open questionsOpen questions• Why the HWhy the H emission peaks in the spectra of different emission peaks in the spectra of different

types objects (Be stars, FK Com stars, cataclysmic stars) types objects (Be stars, FK Com stars, cataclysmic stars) have the same velocities? have the same velocities?

• Why the full width of the HWhy the full width of the H line in the spectra of different line in the spectra of different types objects (Be stars, FK Com stars, cataclysmic stars) types objects (Be stars, FK Com stars, cataclysmic stars) are the same? are the same?

• Do the foregoing facts mean that there is some Do the foregoing facts mean that there is some mechanism of creating of similar gaseous structure with mechanism of creating of similar gaseous structure with almost equal velocities in the different types of stars?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

So… stars, disks, spots and So… stars, disks, spots and peoplepeople, mainly people , mainly people and and friendsfriends……

……Heavy winter, snow, slipperyHeavy winter, snow, slippery and broken bus…and broken bus………And three friends pass through the border to And three friends pass through the border to

help us…help us…

We will remember this always!We will remember this always!To our polish colleagues and true friends with To our polish colleagues and true friends with

large appreciation and love!!!large appreciation and love!!!

ConclusionConclusion