Structure, Dynamics, and Physical Properties of the Warm LISM Within the Local Bubble

Details Structure, Dynamics, and Physical Properties of the Warm LISM Within the Local Bubble Structure, Dynamics, and Physical Properties of the Warm LISM Within the Local Bubble

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1156..174l&link_type=abstract

THE LOCAL BUBBLE AND BEYOND II: Proceedings of the International Conference. AIP Conference Proceedings, Volume 1156, pp. 174-1

Astronomy and Astrophysics

Astronomy

Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus, Interplanetary Magnetic Fields, Astrometric And Interferometric Instruments, Quasars

Scientific paper

We describe our empirical model of warm gas in the local interstellar medium. High-resolution absorption-line spectra of 157 stars provide radial-velocity and physical parameter data for 270 interstellar velocity components. This extensive data set allowed us to piece together a detailed model of the partially ionized warm gas within the Local Bubble. We have identified velocity vectors and projected morphologies of 15 warm gas clouds located within 15 parsecs of the Sun. These clouds have diverse gas temperatures, turbulent velocities, and metal depletions. Cloud-cloud collisions may be responsible for the filamentary morphologies found in about 1/3 of the clouds. We explain the large-amplitude intraday and annular scintillation variability of several quasars seen at radio wavelengths by turbulent scattering screens located at cloud boundaries. Collisions between the clouds could produce the turbulence and ionization at the cloud boundaries. A nearby cold dense cloud is likely compressed and shielded by surounding warm clouds.

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