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Die Bestimmung der Dichte des interstellaren Gases aus 21-cm-Beobachtungen (German, Paperback, 1966 ed.)
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Die Bestimmung der Dichte des interstellaren Gases aus 21-cm-Beobachtungen (German, Paperback, 1966 ed.)
Series: Forschungsberichte des Landes Nordrhein-Westfalen, 1704
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Einleitung und Inhaltsi.ibersicht . . . . . . . . . . . . . . . . .
. . . . . . . . . . . . . . . . . . . . 9 1. Die Struktur und
Geschwindigkeitsverteilung der interstellaren Materi- eine
Ubersicht . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
. . . . . 11 . . . . . . . . . . . . . . . . 2. Der Zusammenhang
der Intensitat der 21-cm-Linie mit Dichte und Temperatur des
interstellaren Mediums . . . . . . . . . . . . . . . . . . . . 19 .
. . . . . . . 3. Die V erteilungsfunktion der kinetischen
Wolkentemperaturen . . . . . . . 23 . A. Die V erteilung der
StoBzeiten . . . . . . . . . . . . . . . . . . . . . . . 24 . . . .
. . . . . . B. Die Abki.ihlungsfunktion des interstellaren Gases .
. . . . . . . . . . . . 29 . . . . C. Die Verteilung der
Wolkentemperaturen . . . . . . . . . . . . . . . . . 31 . . . . . .
. 4. Dichtebestimmung bei endlichem Winkelauflosungsvermogen . . .
. . . . 35 . . 5. Wolkenstruktur und Dichtebestimmung . . . . . . .
. . . . . . . . . . . . . 40 . . . . . . . . 6. Ein Poisson-Modell
der Wolkenverteilung 43 Literaturverzeichnis . . . . . . . . . . .
. . . . . . . . . . . . . . . . . . . . . . 49 . . . . . . . . . .
. . . . . 5 Summary One of the main tasks of 21-cm investigations
consists in the determination of the density of interstellar
Hydrogen gas. This has usually been done with the assumption that
the Hydrogen gas forms a stratum of more or less uniform density.
If Hydrogen clouds exist, they were believed to be transparent for
the 21-cm radiation, and the density gradients were supposed to be
small. However, in the last years observations accumulated which
indicate this picture to be incorrect. The interstellar material
seems to be concentrated in clouds of rather high density and
considerable opacity but of small diameter. The kinetic
temperatures of these clouds need not to be the same for all
clouds, in the contrary, rather large temperature variations are
indicated. These facts make it necessary to reconsider the
derivation of the formulae connecting the measured intensity of the
21-cm radiation with the density of the Hydrogen gas and the
kinetic temperature. This paper intends to lead to an improvement
for the solution of this problem.
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