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Oscar Agertz. Profile photo.

Oscar Agertz

Assistant Professor / Associate senior university lecturer / Wallenberg Academy Fellow

Oscar Agertz. Profile photo.

The source of ionization along the magellanic stream

Author

  • Joss Bland-Hawthorn
  • Ralph Sutherland
  • Oscar Agertz
  • Ben Moore

Summary, in English

Since its discovery in 1996, the source of the bright Ha emission (up to 750 mR) along the Magellanic Stream has remained a mystery. There is no evidence of ionizing stars within the H I stream, and the extended hot halo is far too tenuous to drive strong shocks into the clouds. We now present a hydrodynamical model that explains the known properties of the Ha emission and provides new insights on the lifetime of the Stream clouds. The upstream clouds are gradually disrupted due to their interaction with the hot halo gas. The clouds that follow plow into gas ablated from the upstream clouds, leading to shock ionization at the leading edges of the downstream clouds. Since the following clouds also experience ablation, and weaker Ha (100-200 mR) is quite extensive, a disruptive cascade must be operating along much of the Stream. In our model, the clouds are evolving on timescales of 100-200 Myr, such that the Stream must be replenished by the Magellanic Clouds at a fairly constant rate. The ablated material falls onto the Galaxy as a warm drizzle, which suggests that diffuse ionized gas at 104 K may be an important constituent of galactic accretion. The observed Ha emission provides a new constraint on the rate of disruption of the Stream and, consequently, the infall rate of metal-poor gas onto the Galaxy. When the ionized component of the Stream is fully accounted for, the rate of gas accretion is 0.4 Modot; yr-1, roughly twice the rate deduced from H i observations alone.

Publishing year

2007-01-01

Language

English

Publication/Series

Astrophysical Journal

Volume

670

Issue

2 PART 2

Document type

Journal article

Publisher

American Astronomical Society

Topic

  • Astronomy, Astrophysics and Cosmology

Keywords

  • Galaxies: evolution
  • Galaxies: interactions
  • Hydrodynamics
  • Instabilities
  • Magellanic Clouds
  • Shock waves

Status

Published

ISBN/ISSN/Other

  • ISSN: 0004-637X