On the properties of the local interstellar medium

Journal Article · Wed Jan 01 04:00:00 EST 1986 · Astrophysics (Engl. Transl.); (United States)

DOI:https://doi.org/10.1007/BF01011123· OSTI ID:5112598

Suchkov, A A

The mechanisms of formation of ions whose absorption lines are observed in the spectra of nearby (d < 50 pc) white dwarfs are considered. It is shown that the interstellar ion Si III is partly formed in the heat conduction region between the H I cloud (T = 10/sup 4/ degrees K) in which the Sun is situated and the coronal gas (T > 10/sup 5/ degrees K) surrounding it and partly in the H II region around the observed star. The line-of-sight ion density ratio N (Si IV) /N (Si III) > 10 observed in the direction of the white dwarf G191-B2B can be best explained in a model of an unsteady H II region around this star.

• Research Organization: Rostov State Univ.
• OSTI ID: 5112598
• Journal Information: Astrophysics (Engl. Transl.); (United States), Journal Name: Astrophysics (Engl. Transl.); (United States) Vol. 23:1; ISSN ATPYA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics &amp; Cosmology-- Stars &amp; Quasi-Stellar
Radio &amp; X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABSORPTION SPECTRA
ATMOSPHERES
CHARGED PARTICLES
CHEMISTRY
COSMIC GASES
COSMIC RADIO SOURCES
COSMOCHEMISTRY
DWARF STARS
FLUIDS
GASES
H1 REGIONS
H2 REGIONS
INTERSTELLAR GRAINS
ION DENSITY
IONIC COMPOSITION
IONIZATION
IONS
MATHEMATICAL MODELS
PARTICLES
PHOTOIONIZATION
REMOTE SENSING
SILICON IONS
SOLAR CORONA
SPECTRA
STARS
STELLAR ATMOSPHERES
STELLAR CORONAE
WHITE DWARF STARS