OVI, NV, and CIV in the Galactic Halo: I. Velocity-Dependent Ionization Models

Details OVI, NV, and CIV in the Galactic Halo: I. Velocity-Dependent Ionization Models OVI, NV, and CIV in the Galactic Halo: I. Velocity-Dependent Ionization Models

2004-03-16

arxiv.org/abs/astro-ph/0403388v1

Astrophys.J. 605 (2004) 205-215

Astronomy and Astrophysics

Astrophysics

ApJ in press 22 pages, 9 fig

Scientific paper

10.1086/382186

We explore theoretical models of the ionization ratios of the Li-like absorbers NV, OVI, and CIV, in the Galactic halo. These ions are believed to form in nonequilibrium processes such as shocks, evaporative interfaces, or rapidly cooling gas, all of which trace the dynamics of the interstellar medium. As a useful new diagnostic, we focus on velocity-resolved signatures of several common physical structures: (1) a cooling Galactic fountain flow that rises, cools, and recombines as it returns to the disk; (2) shocks moving toward the observer; (3) a conductive interface with the observer located in the hotter gas. This last geometry occurs with the solar system inside a hot bubble, or when one looks out through the fragmenting top shell of our local bubble blown into the halo as part of the Galactic fountain. In Paper II, these models are compared to ionization-ratio data from FUSE and Hubble Space Telescope.

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