Physical Structure of the Local Interstellar Cloud and Other Nearby Clouds
Abstract
The physical structure and morphology of the interstellar medium that surrounds our solar system directly effects the heliosphere and the interplanetary environment. High resolution ultraviolet absorption spectra of nearby stars and the intervening interstellar medium, observed by the Hubble Space Telescope, provide important information about the chemical abundance, ionization, temperature, kinematics, density, morphology, and turbulent structures of the local interstellar medium (LISM). Fortunately, nearly all observations of objects beyond the solar system contain LISM absorption lines. The number of useful observations is large enough that we can start analyzing the LISM as a three-dimensional object, as opposed to focusing on individual sightlines. We present the results of high resolution observations of the LISM obtained by the Hubble Space Telescope. Our focus will be on the ionization and kinematic structure of the Local Interstellar Cloud (LIC) and other nearby clouds. Fundamental issues we hope to address include: 1) a revised shape of the LIC; 2) a revised kinematic model of the LIC; 3) application of above analysis to other nearby clouds to produce a revised model of the structure of the LISM. Understanding the physical characteristics of these structures is necessary if we are to discuss the morphology of the LISM, its evolution, origin, and impact on the heliosphere and our solar system.
- Publication:
-
34th COSPAR Scientific Assembly
- Pub Date:
- 2002
- Bibcode:
- 2002cosp...34E1522R