Evolution of First Cores and Formation of Stellar Cores in Rotating Molecular Cloud Cores

Details Evolution of First Cores and Formation of Stellar Cores in Rotating Molecular Cloud Cores Evolution of First Cores and Formation of Stellar Cores in Rotating Molecular Cloud Cores

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...674..997s&link_type=abstract

The Astrophysical Journal, Volume 674, Issue 2, pp. 997-1014.

Astronomy and Astrophysics

Astronomy

20

Accretion, Accretion Disks, Methods: Numerical, Stars: Formation

Scientific paper

We followed the collapse of cloud cores with various rotation speed and density frustrations using three-dimensional hydrodynamical simulations by assuming a barotropic equation of state and examined the comprehensive evolution paths from the rotation molecule cloud core to stellar core. We found that the evolutionary paths depend only on the angular velocity of initial cloud core Ωc0. These evolutionary paths agree well with predictions of Saigo and Tomisaka's quasi-equilibrium axisymmetric models and SPH calculations of Bate. Evolutionary paths are qualitatively classified into three types. (1) A slowly rotating cloud with Ωc0<0.01/tff=0.05(ρc0/10-19 g cm-3)1/2 rad Myr-1 shows spherical-type evolution, where ρc0 is the initial central density. Such a cloud forms a first core which is mainly supported by the thermal pressure. The first core has a small mass of Mcore~0.01 Msolar and a short lifetime of a few ×100 yr. After exceeding the H2 dissociation density ρ~=5.6×10-8 g cm-3, it begins the second collapse, and the whole of the first core accretes onto the stellar core/disk within a few free-fall timescales. (2) A rotating cloud with 0.01/tff<Ωc0<~0.05/tff shows disk-type evolution. In this case, the first core becomes a centrifugally supported massive disk with Mcore~a few×0.01-0.1 Msolar and the lifetime is a few thousand years. The first core is unstable against nonaxisymmetric dynamic instability and forms spiral arms. The gravitational torque through spiral structure extracts angular momentum from the central region to the outer region of the first core. And only a central part with r~1 AU begins the second collapse after exceeding dissociation density. However, the outer remnant disk keeps its centrifugal balance after stellar core formation. It seems that this remnant of the first core should control the mass and angular momentum accretion onto the newborn stellar system. (3) A rotating cloud with 0.05/tff<~Ωc0 tends to fragment into binary or multiple during the first core phase.

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