THE UV X-RAY EMISSION OF THE SYMBIOTIC STAR AG DRACONIS DURING QUIESCENCE AND THE 1994/1995 OUTBURSTS/

We present the results of an extensive campaign of coordinated X-ray ( ROSAT) and UV (IUE) observations of the symbiotic star AG Dra during a long period of quiescence followed recently by a remarkable phase of activity characterized by two optical outbursts. The major optical out burst in June 1994 and the secondary outburst in July 1995 were covere d by a number of target of opportunity observations (TOO) with both sa tellites. Optical photometry is used to establish the state of evoluti on along the outburst. Our outburst observations are supplemented by a substantial number of X-ray observations of AG Dra during its quiesce nt phase between 1990-1393. Near-simultaneous IUE observations at the end of 1992 are used to derive the spectral energy distribution from t he optical to the X-ray range. The X-ray flux remained constant over t his three year quiescent phase. The hot component (i.e. X-ray emitting compact object) turns out to be very luminous: a blackbody fit to the X-ray data in quiescence with an absorbing column equal to the total galactic NH in this direction gives (9.5 +/- 1.5) x 10(36) (D/2.5 kpc) (2) erg/s. This suggests that the compact object is burning hydrogen-r ich matter on its surface even in the quiescent (as defined optically) state at a rate of (3.2 +/- 0.5) x 10(-8) (D/2.5 kpc)(2) M./yr. Assum ing a steady state, i.e. burning at precisely the accretion supply rat e. this high rate suggests a Roche lobe filling cool companion though Bondi-Hoyle accretion from the companion wind cannot be excluded. With ROSAT observations we have discovered a remarkable decrease of the X- ray flux during both optical maxima, followed by a gradual recovering to the pre-outburst flux, In the UV these events were characterized by a large increase of the emission line and continuum fluxes, comparabl e to the behaviour of AC Dra during the 1980-81 active phase. The anti correlation of X-ray/UV flux and optical brightness evolution is very likely due to a temperature decrease of the hot component. Such a temp erature decrease could be the result of an increased mass transfer to the burning compact object, causing it to slowly expand to about twice its original size during each optical outburst.