1. Eclipsing binary systems with pulsating components.
Gamarova A. Yu., Mkrtichian D.E., Hatzes A.P., Lehmann H.
Liege, 2002

2. Eclipsing binaries with pulsating components (EBPC)
Detached systems:
Typical objects:
AI Hya, MM Cas, RS Cha etc.
(See Lampens & Boffin, 2000, ASP vol 210)
Eclipsing binaries with b Cep stars;
Eclipsing binaries with RR Lyr stars;
Eclipsing binaries with Cepheids
(See Szatmary K. 1990, JAAVSO, vol 19 )
Semi-detached Algol-type systems: oscillating EA (oEA)
(See Mkrtichian et al, 2002, ASP vol.259)
Known objects: AB Cas, RZ Cas,
Y Cam, AS Eri, R CMa, TW Dra, AB Per, RX Hya

3. Parameters of known oEA:
Name
Sp. type
Porb, d
Ppuls,min
AB Cas
A3 V+K0 IV
83.93
RZ Cas
1.1953
22.43, 25.44
Y Cam
A7 V+K1 IV
3.3055
95.74, 78.77, 97.17, 81.22
R CMa
F1 V+G2-K2 IV
1.1359
68.5
TW Dra
A6 V+K0 IV
2.8069 80
AS Eri
A3 V+K0 III
2.6642
24.39, 23.01, 23.34
RX Hya
A8 V+K5
2.2816
74.26
AB Per
A5 V+G9 IV
282.02

4. The description of oEA group:
Evolution:
low-mass progenitors of EBS  rapid mass transfer stage rapid evolution into the d Scu,  Boo ... instability strip  slow mass-transfer/accretion stage, evolution along the MS
and & pulsations
Features:
Mass accretion and pulsations ,
Multiperiodicity (RZ Cas, AS Eri, Y Cam)
the shortest known pulsation periods ford Scu–type pulsators are presented (RZ Cas, AS Eri) – high overtone modes;
SMT
RMT MS

5. The description of oEA group:
Features:
orbital modulation of pulsation RV amplitude (RZ Cas, top graph) – screening and attenuation of NRP by inhomogeneous circumbinary envelope & accretion stream
rapid changes (during several months) of the pattern of pulsation spectrum (RZ Cas);
Anomalous Schlesinger-Rossiter effect (RZ Cas) (Lehmann& Mkrtichian, 2002)
Expected Features:
Dependence of (dP/dt 1/P) on the accretion rate
Influence of rapid mass accretion episodes on pulsation properties and on mode selection mechanism
f=0.1
f=0.9

6. Advantages presented by EBPC:
Asteroseismology:
The possibility of the precise determination of parameters (masses, radii, effective temperatures);
The higher probability of the detection of the sectorial NRP modes;
The possibility of mode identification during primary eclipse (the method of spatial filtration);
The possibility of use of the circum-binary envelope as a spatial filter.
Evolution of eclipsing binaries:
The possibility of the precise determination of the asynchronism;
The possibility of the precise estimation of the accretion rate
and the status on a slow mass-transfer stage (i.e. the age of the system);
The possibility of the investigation of the gas envelope properties basing on the inspection of pulsations at different orbital phases.

7. Mode identification in the oEA AB Cas:
Considered pulsation characteristics:
Gain factor is the ratio of the observed pulsation amplitudes during the eclipse of pulsating component to the amplitude outside the eclipse:
Pulsational phase shift :
tmax - the time moment of observed maximum;
t predicted by the pulsation ephemeris time
of maximum;
Ppuls - the observed pulsation period.

8. Mode identification in the oEA AB Cas:

9. Prospects for future COROT investigation:
Pulsation mode spectra and doing seismology
Estimation of the accretion driven photometric noise
Hypothesis of synchronization & asynchronity in binary systems

10. Short summary on the EB in the COROT FOV:
Why are these objects suitable for COROT observations?
Situated in the possible COROT FOV;
The range of magnitudes matches with the range chosen for the COROT transit search;
COROT will provide the sufficient accuracy and time coverage for investigation of this type of pulsation variability and mode identifiction;
What is known about binaries in the COROT FOV?
Faint objects  poorly investigated;
No spectral types & effective temeratures are known;
No orbital elements are available;
No detections of pulsations!!!
What do we need to know for application of mode identification techniques and seismology?
Spectral types & effective temperatures;
Orbital parameters

11. The prospects for ground-based support:
Spectral type classification & effective temperature determination: TLS 2.0m, Calar-Alto, ESO
Photometric observations for the determination of the orbital elements and preliminary search for and study pulsations: Euro-Asian (Spain-Ukraine-Kazakhstan-Uzbekistan-South Korea) Network of Observatories.