By André Maeder (auth.), John Dyson, Susan A. Lamb, A. G. W. Cameron, A. M. Cherepashchuk, C.-G. Fälthammar, M. Kitamura, L. B. F. M. Waters, C. Waelkens, K. A. van der Hucht, P. A. Zaal (eds.)
The profitable release on November 17, 1995 of ESA's Infrared house Observatory (ISO) through an Ariane four provider, has set in movement a real revolution in quantitative infrared astronomy. For the 1st time because the very profitable IRAS venture in 1983, the astronomical neighborhood has uninterrupted entry to the infrared a part of the electromagnetic spectrum. The 4 focal aircraft tools on board of ISO ( the digicam ISOCAM, the photometerjcamera ISOPHOT, and the quick and lengthy wavelength spec trographs ISO-SWS and ISO-LWS), practice rather well and dwell as much as the excessive expectancies we all had at release. within the spring of 1996, Thijs de Graauw (principal investigator of the SWS) first prompt the belief to prepare a convention devoted to ISO re sults within the zone of stars and circumstellar subject, and coined the identify ISO 's View on Stellar Evolution. on the first clinical assembly to focus on the various early ISO effects which was once held in might of 1996 at ESA's laboratory ESTEC in Noordwijk, the Netherlands, the convention used to be introduced and a initial technology organizing committee was once shaped. The convention used to be held from July 1 to four, 1997, in convention centre de Leeuwenhorst, Noord wijkerhout, the Netherlands. The convention was once opened by means of the Director of ESA 's technology Programme, Professor R. Bonnet.
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The data analysis and observing procedures for these observations are described in Sitko et al. (1997). The remainder of this paper focusses on the 8-13 ţL region of the spectra. 3. 3 Figure 1. lffi continuum normalized silicate profiles for UXORs. ISO data for SV Cep and HR 5999 are shown, with the other data from BASS. b) Comparison of sili eate emission profiles with laboratory silicate spectra (Hallenbeck et al. 1997) annealed for 3 hours at 1027 K. SV Cep is compared with MgSiOx and BF Ori is compared with Mg-Fe-SiOx.
However, in general this will not be the case, and in edge-on systems the short-wavelength emission from the hot protostar may not be detected. Meyer: Will it be possible to distinguish observationally between prompt fragmentation of a cloud core (with large mass ratios) and the disk fragmentation mechanism you propose for giant planet/brown dwarf companion formation? Boss: Yes, to the extent that ages of the objects can be determined or constrained. Binary fragmentations should produce equal-age protostarsjcompanions, whereas the disk instability mechanism is envisioned as happening after the central star is essentially completely formed, and so produces companions that are younger than their primaries.
Et al. 1996, A&A 309, 474 Hallenbeck, S. et al. S. et al. 1995, ApJ 438, 250. Herbst, W. et al. A. et al. 1992, ApJ 397, 613. , & de Winter, D. G. et al. 1994, A&A 285, 883. F. et al. 1993, ApJ 418, 440. I. I. 1997b, ApJ (in press) Molster, F. S. 1994, ASP Conf. Ser. 62, 199. R. A. 1997, Space Science Rev. (in press). Pollack. B. et al. 1994, ApJ 421, 615. Russell, R. et al. 1997, Nature, (submitted). S. et al. L. et al. L. et al. 1996, in From Stardust to Planetesimals: Contributed Papers, eds.