English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

A recent paper by Stanimirovic etal (2008) presents quit interesting resultsfrom HI observations of the Magellanic Stream (MS) tip. The high spatialresolution of the data reveals rich and complex morphological and kinematicstructures; notably four coherent HI substreams extending over angular size ofabout 20 deg were found.  We use the position-velocity images of Stanimirovic etal (2008) to derivespatial power spectra for the velocity residuals. These, indicate the presenceof a large scale turbulence with size comparable to that of the streamsthemselves. The turbulent velocity on the largest scale is estimated to beabout 15 km/s . Adopting, a distance of 120 kpc, implies a turbulent largestscale of 40 kpc and timescale for decay of about 3 Gyr. For a turbulence withscale that large, the natural energy source is the tidal interaction betweenthe Magellanic Clouds, and between them and the Milky Way galaxy. The shape ofderived turbulence spectrum is used here to obtain constraints on theinclination of the streams and on the density of the emitting neutral hydrogen.

Turbulence: A Probe of the Dynamics and Physics of the Magellanic Stream