The similarity of the H line in the spectra of different types of active stars Seminar at AP Krakow,

1
The similarity of the H? line in the spectra of
different types of active starsSeminar at AP
Krakow, November 29 2005D. Kjurkchieva D.
MarchevWe 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).
2
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
3

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

4

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

5
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 .
6
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
7
The results of our cooperationsince 1987I. 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

8
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

9
III. The W UMa stars

• Kreiner J. et al., 2003, AA 412, 465, Physical
  parameters of components in close binary stars.
  I
• Contribution in the photometric observations of
  the stars

10
Results 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

11
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.

12
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 configurationmain star -
source of the absorption reversalextended
half-illuminated disk - source of the
emission peaksSAE source of the additional
emissionSAA - source of the additional
absorptionsecondary star source of the
illumination of the disk FK
Com double star
13
Results from the investigation of UV
LeoKjurkchieva D., Marchev D., 2005, AA
submitted, New spectroscopic solution of the
star UV LeoThe main problem which of the star
components is larger?

• H? observations with S/N100
• 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

14
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
15
Results from the investigation of EM
CepKjurkchieva 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)

16
?he H? profiles at Be and B state differ but
their full widths and depths are almost the
sameIt look as the emission wings at Be state
convert to absorption at B state
17
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
18
The irregular times of the minima ? O-C0.01d
for a couple of daysConfirmation of secular
linear decreasing of the period
19
Similarity of the H? profile of EM Cep with that
of disk-like star FK Com in a) positions of
the emission peaksb) whole width
20
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
21
The subtracted spectra (individual spectrum minus
the spectrum at phase 0.48) at Be state show
only ADEM around quadratures
22
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 0.19-0.23Is this an
indication of the contribution of the secondary
star?
23
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
24
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

25
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?

26
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

27
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!!!