Interstellar Matter, Galaxy, Universe by P.L. Biermann, G. Börner, M. Camenzind, K.J. Fricke, B.

By P.L. Biermann, G. Börner, M. Camenzind, K.J. Fricke, B. Fuchs, R. Genzel, W.K. Huchtmeier, H. Jahreiß, A.R. Just, B.F. Madore, H. Netzer, H. Schwan, B.. Wiebel-Sooth, A. Witzel, Zimmermann

Astronomy and Astrophysics have been first handled in quantity III of the sixth variation of Landolt-Börnstein in 1952, then in volumes VI/1 and VI/2 of the hot sequence, 1965 and 1981/82 respectively. the current quantity VI/3 is an extra supplementation of quantity VI/1. The decimal class scheme of the 1st complement volumes, VI/2, has been maintained, fields with no major new advancements are truly indicated. A synoptic checklist of contents over all 3 volumes presents a good evaluate for the consumer in addition to a entire Index within the impending final subvolume of VI/3.

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Instit. Ser. Vol. 487. Dordrecht: Kluwer (1996). : in [96G1], p. 43. : in [96G1], p. 1. : in [96G1], p. 133. 1 General references List of LB VI/2c subsect. 1. p. 126, updated. F. : Molecular Astrophysics - State of the Art and Future Directions. Dordrecht: Reidel (1985). : Molecular Collisions in the Interstellar Medium. Cambridge: Univ. Press (1990). A. ): Interstellar Processes, Proceed. Symp. on Interstellar Processes, Astrophys. Space Sci. Libr. Vol. 134. Dordrecht: Reidel (1987). A. ): Rate Coefficients in Astrochemistry.

P. 5 18 30 SiC Silicates MgS ? A detailed spectroscopic discussion of observed emission bands is given by Allamandola et al. [89A1]. Dust-related visual continuous emission The Extended Red Emission band, usually between about 6000 and 8000 Å, takes the form of a broad band peaking near 6700 Å with about 1200 Å FWHM [89W] and can be fitted well with the measured band-gap emission from hydrogenated amorphous carbon [90W]. 4 Grain models Table 3. Materials suggested as constituents of interstellar grains, in addition to the materials listed in LB VI/2c subsect.

L. 75…2 m2) scintillator stations, ionization calorimeter, several gas discharge hodoscopes. l. Energy range: 300 TeV…70 PeV Operating: since 1996 Technique: 13 Cherenkov counters. Landolt-Börnstein New Series VI/3C Ref. p. l. Energy range: 300 TeV…30 PeV Technique: 13 open Cherenkov counters. l. 25 m2) scintillator stations, 6 × (20 m2) muon detectors, 53 Cherenkov detectors, 7 Cherenkov pulse form detectors, 10 radio antennas (32 MHz). 5 The main elements in the TeV range Plotting the data of individual nuclei as provided by the direct experiments so far, without using further adjustments, shows in general a fair correspondence in overlapping energy ranges.

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