Titlebook: Shocks in Astrophysics; Proceedings of an In T. J. Millar,A. C. Raga Conference proceedings 1995 Kluwer Academic Publishers 1995 Galaxy.Sup

Magisterial

B. T. Drainezed by highly variable geology, geomorphology, soils, climate, vegetation and land use. Human activity proved to be the main factor affecting changes in this environment. This chapter deals with erosion forms and processes, as reflected in the fluvial system morphology. The effects of erosion are of

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老巫婆

S. D. Taylor,A. C. Ragaove the Sea of Galilee and the Yarmouk River. It is part of the Harrat Ash Shaam volcanic field, which is the largest volcanic field in western Arabia. The volcanics of the Golan Heights cover a syncline, which is located between the anticlines of Ajlun and Mt. Hermon on its southern and northern si

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Garrelt Mellema,Adam Frankd with epeirogenic movements and eustatic fluctuations close to the sea-land transition. The Syrian Arc folding, active since the Santonian, has some implications on the present-day relief. During the late Eocene–Oligocene, an extensive regression and regional uplift shifted the coast to the NW expo

albuminuria

C. Dominik,A. P. Jones,A. G. G. M. Tielensd in Italian landscapes.Presents more than thirty case studi.The book deals with the most striking landscapes and landforms of Italy. Attention is given to landform diversity and landscape evolution through time which has been controlled by very diverse geological conditions and dramatic climate cha

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Conference proceedings 199595. The study of interstellar and circumstellar gas dynamics has a long and distinguished history in Manchester and has been almost entirely concentrated in the school founded by Franz Kahn in the Astronomy Department, University of Manchester. In January 1993, one of us (AR) was appointed to the fa

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Multifluid Models of Shocks in Magnetized Interstellar Molecular Clouds,ud shock. Models of shocks in which continuous dissipation is important have been developed in studies of the origins of CH. in diffuse clouds, H. emission features with widths of around 100 km s. in Orion and OH masers around young stars, but CH. and such broad H. features may arise in boundary layers between molecular regions and fast flows.

花争吵

Observations of Shocked H2 And [FeII] Line Profiles in Orion Bullet Wakes, Observations of broad, singly-peaked H. 1–0 S(l) profiles in the most clearly resolved bullet wakes challenge our understanding of molecular shocks. It may be necessary to model the effects of instabilities and turbulence in the Orion bullet wakes in order to fit our observations.

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Models of Molecular Outflows, more complex and not yet fully understood, given the presence of time variability in the jet velocity and/or direction. Finally, I discuss constraints on wind properties (momentum, mass-loss rate, radius) that can be derived from molecular outflows driven by jet bowshocks.

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