Structure and spectrum of quiescent prominences. III. Application of theoretical models in helium abundance determinations

Journal Article · Sat Apr 15 04:00:00 EST 1978 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/156072· OSTI ID:6931543

Heasley, J N; Milkey, R W

The solar helium abundance has been investigated by using spectra of quiescent prominences. The physical parameters (T, P, y, xi, M) describing an isothermal and isobaric model of the prominence can be determined from observations of hydrogen, helium, and ionized calcium lines. Given these parameters, it may be shown that low values of the helium abundance, such as those inferred from solar wind data, are inconsistent with the prominence data. The helium-to-hydrogen ratio is indicated to be 0.10 +- 0.025 by number.

• Research Organization: Kitt Peak National Observatory
• OSTI ID: 6931543
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 221:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABUNDANCE
ATOMIC IONS
ATOMIC MODELS
CALCIUM IONS
CHARGED PARTICLES
CHEMICAL COMPOSITION
CRYOGENIC FLUIDS
ELEMENTS
ENERGY SPECTRA
FLUIDS
HELIUM
HYDROGEN
IONS
MATHEMATICAL MODELS
NONMETALS
PLASMA
RARE GASES
SOLAR ACTIVITY
SOLAR PROMINENCES
SOLAR WIND
SPECTRA
STAR MODELS