The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution
The Magellanic Stream (MS) is the nearest example of agaseous trail formed by interacting galaxies. While the substantial gas masses in these kinds of circumgalactic structures are postulated to represent important sources of fuel for future star formation, the mechanisms whereby this material might...
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Astronomical Observatory, Department of Astronomy, Belgrade
2010-06-01
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doaj-1a0d22e2074841d6a1f210fc0f5d0b9a2020-11-24T21:06:06ZengAstronomical Observatory, Department of Astronomy, BelgradeSerbian Astronomical Journal1450-698X2010-06-01180110The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy EvolutionNigra, L.Gallagher, J. S., IIIStanimirovic, S.The Magellanic Stream (MS) is the nearest example of agaseous trail formed by interacting galaxies. While the substantial gas masses in these kinds of circumgalactic structures are postulated to represent important sources of fuel for future star formation, the mechanisms whereby this material might be accreted back into galaxies remain unclear. Recent neutral hydrogen (HI) observations have demonstrated that the northern portion of the MS, which probably has been interacting with the Milky Way's hot gaseous halo for close to 1000~Myr, has a larger spatial extent than previously recognized, while also containing significant amounts of small-scale structure. After a brief consideration of the large-scale kinematics of the MS as traced by the recently-discovered extension of the MS, we explore the aging process of the MS gas through the operation of various hydrodynamic instabilities and interstellar turbulence. This in turn leads to consideration of processes whereby MS material survives as cool gas, and yet also evidently fails to form stars.Parallels between the MS and extragalactic tidal features are briefly discussed with an emphasis on steps toward establishing what the MS reveals about the critical role of local processes in determining the evolution of these kinds of systems.http://saj.matf.bg.ac.rs/180/pdf/001-010.pdfGalaxy: haloGalaxies: evolutionMagellanic CloudsHydrodynamicsInstabilities |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Nigra, L. Gallagher, J. S., III Stanimirovic, S. |
spellingShingle |
Nigra, L. Gallagher, J. S., III Stanimirovic, S. The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution Serbian Astronomical Journal Galaxy: halo Galaxies: evolution Magellanic Clouds Hydrodynamics Instabilities |
author_facet |
Nigra, L. Gallagher, J. S., III Stanimirovic, S. |
author_sort |
Nigra, L. |
title |
The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution |
title_short |
The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution |
title_full |
The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution |
title_fullStr |
The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution |
title_full_unstemmed |
The Small-Scale Structure of the Magellanic Stream as a Foundation for Galaxy Evolution |
title_sort |
small-scale structure of the magellanic stream as a foundation for galaxy evolution |
publisher |
Astronomical Observatory, Department of Astronomy, Belgrade |
series |
Serbian Astronomical Journal |
issn |
1450-698X |
publishDate |
2010-06-01 |
description |
The Magellanic Stream (MS) is the nearest example of agaseous trail formed by interacting galaxies. While the substantial gas masses in these kinds of circumgalactic structures are postulated to represent important sources of fuel for future star formation, the mechanisms whereby this material might be accreted back into galaxies remain unclear. Recent neutral hydrogen (HI) observations have demonstrated that the northern portion of the MS, which probably has been interacting with the Milky Way's hot gaseous halo for close to 1000~Myr, has a larger spatial extent than previously recognized, while also containing significant amounts of small-scale structure. After a brief consideration of the large-scale kinematics of the MS as traced by the recently-discovered extension of the MS, we explore the aging process of the MS gas through the operation of various hydrodynamic instabilities and interstellar turbulence. This in turn leads to consideration of processes whereby MS material survives as cool gas, and yet also evidently fails to form stars.Parallels between the MS and extragalactic tidal features are briefly discussed with an emphasis on steps toward establishing what the MS reveals about the critical role of local processes in determining the evolution of these kinds of systems. |
topic |
Galaxy: halo Galaxies: evolution Magellanic Clouds Hydrodynamics Instabilities |
url |
http://saj.matf.bg.ac.rs/180/pdf/001-010.pdf |
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