By A. G. G. M. Tielens (auth.), Isabelle Cherchneff, Tom J. Millar (eds.)
ISBN-10: 9048150183
ISBN-13: 9789048150182
ISBN-10: 9401713073
ISBN-13: 9789401713078
Dust and molecules are present in a wide number of astrophysical environments, particularly within the circumstellar fabric ejected by means of advanced stars. This ebook brings jointly the best astronomers and astrophysicists within the box of molecular astrophysics and stellar physics to debate the $64000 problems with airborne dirt and dust and molecular formation, the function of solids in circumstellar environments, molecules as probes of circumstellar parameters, the stellar contribution to the enrichment of the Galaxy, and the most recent observational facts in a number of wavelength domain names, in partiular within the infrared with effects from the Infrared area Observatory. The astrophysical senarios comprise late-type stars, novae, Wolf-Rayet stars, Luminous Blue Variables and supernovae.
Audience: Researchers and graduate scholars within the fields of stellar physics, stellar evolution and astrochemistry.
Read Online or Download Dust and Molecules in Evolved Stars: Proceedings of an International Workshop held at UMIST, Manchester, United Kingdom, 24–27 March, 1997 PDF
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New PDF release: Dust and Molecules in Evolved Stars: Proceedings of an
Dirt and molecules are present in a wide number of astrophysical environments, specifically within the circumstellar fabric ejected via advanced stars. This booklet brings jointly the major astronomers and astrophysicists within the box of molecular astrophysics and stellar physics to debate the $64000 problems with airborne dirt and dust and molecular formation, the function of solids in circumstellar environments, molecules as probes of circumstellar parameters, the stellar contribution to the enrichment of the Galaxy, and the newest observational info in quite a few wavelength domain names, in partiular within the infrared with effects from the Infrared house Observatory.
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Additional resources for Dust and Molecules in Evolved Stars: Proceedings of an International Workshop held at UMIST, Manchester, United Kingdom, 24–27 March, 1997
Sample text
In Eqs. T8 and Cf are the amplitudes of temperature and density-compression factors, respectively, between pre- and post-shocked gas; < To > and < n 0 > are the average temperature density at a point in the radio photosphere; and ifJs is "phase" of the propagating shock or disturbance. We chose a constant propagation speed, Vs, and defined ifJs by the equation (2) where P is the period of the star. For more details regarding this model consult Reid & Menten (1997); note that this model is completely empirical and is only constrained near the radio photosphere.
1994), the low CN/HCN abundance ratios (Olofsson et al. 1991; Bachiller et al. 1997), and the low abundances ofH2CO (Olofsson, unpubl. data), C2H and CHaOH {Charnley & Latter 1997) with respect to HCN. Finally, let us remark that as long as there exist no detailed maps of brightness distributions of various molecular line emissions our comparison with theory must be regarded as only tentative. An interesting example of this is the overlap of the C2H, C3 H, and C4H regions in ffiC+ 10216 (Guelin et al.
No molecular emission Jines have ever been seen in LWS offset spectra. Dalgarno: Comment (Barlow) -The predicted abundance of HeH+ is directly proportional to the assumed rate coefficient for the dissociative recombination of HeH+ which is the dominating destruction mechanism. Its value is still highly uncertain. ISO-SWS SPECTRA OF AGB STARS K. JUSTTANONT, I. YAMAMURA AND T. M. WATERS University of Amsterdam Kruislaan 403,1098 SJ Amsterdam, The Netherlands Abstract. In this contribution, we present a few highlights of the guaranteed time program to observe AGB stars with differing chemical compositions and mass loss rates using ISO 1 SWS.
Dust and Molecules in Evolved Stars: Proceedings of an International Workshop held at UMIST, Manchester, United Kingdom, 24–27 March, 1997 by A. G. G. M. Tielens (auth.), Isabelle Cherchneff, Tom J. Millar (eds.)
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