Pre-main sequence sun: a dynamic approach

Conference · Mon Jan 01 00:00:00 EST 1979

OSTI ID:5521364

Newman, M J; Winkler, K H.A.

The classical pre-main sequence evolutionary behavior found by Hayashi and his coworkers for the Sun depends crucially on the choice of initial conditions. The Hayashi picture results from beginning the calculation with an already centrally condensed, highly Jeans unstable object not terribly far removed from the stellar state initially. The present calculation follows the work of Larson in investigating the hydrodynamic collapse and self-gravitational accretion of an initially uniform, just Jeans unstable interstellar gas-dust cloud. The resulting picture for the early history of the Sun is quite different from that found by Hayashi. A rather small (R approx. = 2 R/sub sun/), low-luminosity (L greater than or equal to L/sub sun/) protostellar core develops. A fully convective stellar core, characteristic of Hayashi's work, is not found during the accretion process, and can only develop, if at all, in the subsequent pre-main sequence Kelvin-Helmholtz contraction of the core. 3 figures, 1 table.

• Research Organization: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
• DOE Contract Number: W-7405-ENG-36
• OSTI ID: 5521364
• Report Number(s): LA-UR-80-22; CONF-7910123-1; TRN: 80-004787
• Resource Relation: Conference: Lunar and Planetary Institute topical conference on the ancient sun, Boulder, CO, USA, Oct 1979
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SUN
STAR EVOLUTION
BOUNDARY CONDITIONS
COSMIC DUST
COSMIC GASES
ELECTRON TEMPERATURE
GRAPHS
HERTZSPRUNG-RUSSELL DIAGRAM
LUMINOSITY
THEORETICAL DATA
DATA
DATA FORMS
DIAGRAMS
DUSTS
FLUIDS
GASES
INFORMATION
MAIN SEQUENCE STARS
NUMERICAL DATA
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
STARS
640104* - Astrophysics & Cosmology- Solar Phenomena