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While in the past spherodicity was assumed, and still is used in modeling of most nebulae, we know now that only a small number of planetary nebulae (PNe) are really spherical or at least nearly round. Round planetary nebulae are the minority of objects. In the case of those objects that underwent a very late helium flash (called VLTP objects or ``born-again'' PNe) it seems to be different. The first, hydrogen-rich PN, is more or less round. The ejecta from the VLTP event, in contrast, are extremely asymmetrical., Comment: to appear in the proceedings of HYDEF07, Tuebingen 2007

While in the past spheroidicity was assumed, and still is used in modeling of most nebulae, we know now that only a small number of planetary nebulae (PNe) are really spherical or at least nearly round. Round planetary nebulae are the minority of objects. In case of those objects that underwent a very late helium flash (called VLTP or "born-again" PNe) it seems to be different. The first, hydrogen rich PN, is more or less round. The ejecta from the VLTP event is extremely asymmetrically. Angular momentum is mostly assumed to be the main reason for the asymmetry in PNe. Thus we have to find processes either changing their behavior within a few hundred to a few thousands of years or change their properties dramatically due to the variation of the abundance. They most likely have a strong link or dependency with the abundance of the ejecta., Comment: will appear in the proceedings of "Asymmetrical Planetary Nebulae IV", Eds.: Romano L.M. Corradi, Arturo Manchado and Noam Soker

We derived the properties of V605 Aql before the final helium flash pulse by studying its surrounding PN A58. Photoionizing models of our spectral data together with a new distance estimate and a closer look at the recombination timescales lead to a consistent model. Comparing our findings with the only hydrogen-poor twin, namely Sakurai's Object, we conclude that these born-again objects have normal PNe core masses. We are able to prove V605 Aql indeed to be, similar to V4332 Sgr, a very late thermal pulse object and to put constraints for the evolutionary time scales for the transition back to the AGB., Comment: LaTeX, 5 pages, 3 figures, Accepted in Astron. & Astrophys

Intermediate resolution spectroscopy of NOVA Oph 2003 (V2573 Oph), which was first detected March 21th 2003 but reported July 19th} 2003, obtained 19th to 23rd of July is presented here. The photometry during the early phases of the object is shortly discussed. We also retrieved very accurate astrometry of the target in this crowded field. This is needed to be able to do further observations of the post-nova during the next years. The inspection of the sky survey plates gives a possible progenitor candidate and allows to derive a lower limit for the outburst magnitude of about 10.0 mag. The spectrum shows an overall expansion of 2200 km/s and has clearly complex outflow substructures. The spectroscopy identifies this object as classical nova, "Fe II" subclass., Comment: 4 pages, LaTeX, 8 figures, accepted for publication in Astronomy and Astrophysics Letters - Changed with respect to the original version due to doubts, raised by other scientists after the acceptance by A&A, about the photometry used here and taken from literature

We present a detailed spectroscopic investigation, spanning four winters, of the asymptotic giant branch (AGB) star IRAS 02091+6333. Zijlstra & Weinberger (2002) found a giant wall of dust around this star and modelled this unique phenomenon. However their work suffered from the quality of the optical investigations of the central object. Our spectroscopic investigation allowed us to define the spectral type and the interstellar foreground extinction more precisely. Accurate multi band photometry was carried out. This provides us with the possibility to derive the physical parameters of the system. The measurements presented here suggest a weak irregular photometric variability of the target, while there is no evidence of a spectroscopic variability over the last four years., Comment: 5 pages, Latex, 3 tables, 4 figures, Astron. & Astrophys. - in press