Reviews in Modern Astronomy: Variabilities in Stars and by B. Wolf (auth.), Dr. Gerhard Klare (eds.)

By B. Wolf (auth.), Dr. Gerhard Klare (eds.)

The overseas clinical Spring assembly of the Astronomische Ge­ sellschaft (AG) held at Bamberg in April 1991 used to be dedicated to "Vari­ talents in Stars and Galaxies". Time-dependent phenomena are saw in quite a lot of as­ tronomical items. they're because of various actual mechanisms (for instance via pulsation, by means of accretion, or by means of dramatic eruptive occasions in reference to mass outflow) generating observable depth vari­ ations via all wavelengths. a few of the papers during this quantity are considering galactic stars displaying such behaviour (for ex­ considerable cataclysmic variables, symbiotic stars, luminous blue variables (LBVs) and novae). Intrinsic diversifications of the, magnetic box struc­ ture on observable time scales are, for example, a peculiarity of cool, solar-like stars and symbolize a useful gizmo to check differential rotation and cycles of task. contemporary effects at the research of fuel motions within the internal areas of the Milky approach method, a research of the bipolar galaxy M eighty two, observations of variable extragalactic radio resources, the range of emission traces in energetic galactic nuclei (AGN) in addition to continuum diversifications of quasars and AGN are mentioned by means of numerous authors. The yearbook sequence reports in sleek Astronomy of the AG to carry the medical occasions of the used to be verified in 1988 so as conferences of the society to the eye of the global astronomical community.

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The assumed mechanism taken as a basis, the main problem with symbiotic novae or symbiotic stars in general is accretion. Before the outburst the material must be provided by the cool component by mass loss. 55 The question is weather a sufficient amount of material will reach the white dwarf. Because of the large separation of the components in those systems Roche overflow is mostly impossible. Only wind accretion may be the ongoing mechanism for mass transfer. g. are there magnetic fields? what role do they play?

8: VY Aqr, superposition of the 1986, 1988 and 1990 supermaxima 5m • I~ •• b •• 6 I 7 mv 0 8 0 10 I I 11 12 JD2436 0 2427 2414 .... ·'. ""ocP o 0 •••• +0. 0 o 00 &3 I J • •• 0 00 0 o 0 •••'" t> ~ • ~iP. + OPo J 400 298 459 410 308 469 420 318 479 430 328 489 440 338 499 450 460 348 358 509 519 470 368 529 Fig. 9: Recurrent nova RS Oph (dates collected'c:f'rom bibliography, mostly observations from Prager and Oragg) 35 ,1\ mpg 9m 11 I 13 v vv : I I 15 'I • USeo ~ ~r:s/J 1987 •• ....... - ... p 17 2444 2446 1979 = a = < D • 070 950 ........

This process may be going on in Z And and similar objects. Mass accretion and fluctuations of it may directly influence the nuclear burning on the surface of the white dwarf and appear respectively as variability in brightness or fluctuations of the surface temperature. o. Variable mass loss may also directly cause fluctuations in ~e brightness of the system. This is explained by NUSSBAUMER and VOGEL (1990) as follows: The cool stellar wind from the red giant interacts with the photons of high energy of the hot component, turning UV-photons into visible light.

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