Masses and pulsations of BL Herculis variables

Conference · Thu Jan 01 00:00:00 EST 1981

OSTI ID:5790443

Hodson, S W; Cox, A N; King, D S

From linear results, the masses of BL Her variables must be nearer to 0.55 M /sub sun/ than 0.75 M /sub sun/ if the bump phase transition (resonance) is to be located anywhere near the observed period range of 1./sup d/5 to 1./sup d/7. The nonlinear results are consistent with the Simon resonance concept, but demonstrate that light and velocity curve shapes are a nonlinear phenomenon that require nonlinear period ratios to display the resonances only in the narrow, observed range of 1./sup d/5 to 1./sup d/7. The mass near 0.55 M /sub sun/ is in good agreement with evolution calculations (Sweigart and Gross, 1976) and nonlinear pulsation studies of Carson, Stothers, and Vemury (1981) and Stothers (1981).

• Research Organization: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
• DOE Contract Number: W-7405-ENG-36
• OSTI ID: 5790443
• Report Number(s): LA-UR-81-3250; CONF-8110131-2; ON: DE82002347; TRN: 82-005444
• Resource Relation: Conference: IAU colloquium 68, Schenectady, NY, USA, 7 Oct 1981
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
VARIABLE STARS
MASS
PULSATIONS
EXPERIMENTAL DATA
HERTZSPRUNG-RUSSELL DIAGRAM
RADIAL VELOCITY
STAR EVOLUTION
DATA
DIAGRAMS
INFORMATION
NUMERICAL DATA
STARS
VELOCITY
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources