The millimeter-wave spectrum of highly vibrationally excited SiO. [In astronomical sources]

Journal Article · Fri Feb 01 04:00:00 EST 1991 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/185938· OSTI ID:5701268

Mollaaghababa, R; Gottlieb, C A; Vrtilek, J M; Thaddeus, P ^[1]

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1. Harvard Univ., Cambridge, MA (USA) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)

The millimeter-wave rotational spectra of SiO in high vibrational states (v = 0-40) in its electronic ground state were measured between 228 and 347 GHz in a laboratory discharge through SiH4 and CO. On ascending the vibrational ladder, populations decline precipitously for the first few levels, with a vibrational temperature of about 1000 K; at v of roughly 3, however, they markedly flatten out, and from there to v of roughly 40 the temperature is of the order of 10,000 K. With the Dunham coefficients determined here, the rotational spectrum of highly vibrationally excited SiO can now be calculated into the far-infrared to accuracies required for radioastronomy. Possible astronomical sources of highly vibrationally excited SiO are certain stellar atmospheres, ultracompact H II regions, very young supernova ejecta, and dense interstellar shocks. 16 refs.

• OSTI ID: 5701268
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 368; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ASTRONOMY
ATMOSPHERES
CHALCOGENIDES
CHEMICAL COMPOSITION
COSMIC RADIO SOURCES
ENERGY LEVELS
ENERGY-LEVEL TRANSITIONS
ERUPTIVE VARIABLE STARS
EXCITATION
H2 REGIONS
INTERSTELLAR SPACE
LABORATORIES
LASERS
MASS TRANSFER
MICROWAVE SPECTRA
OXIDES
OXYGEN COMPOUNDS
RADIOASTRONOMY
SHOCK WAVES
SILICON COMPOUNDS
SILICON OXIDES
SPACE
SPECTRA
STARS
STELLAR ATMOSPHERES
SUPERNOVAE
TEMPERATURE DEPENDENCE
VARIABLE STARS