Non-similar collapse of singular isothermal spherical molecular cloud cores with nonzero initial velocities

TL;DR

This paper investigates the non-spherical collapse of molecular cloud cores considering magnetic and rotational effects, revealing how these factors influence core shape and mass infall rates before expansion wave formation.

Contribution

It introduces a semi-analytical approach using the Adomian decomposition method to study non-symmetric collapse of SIS cores with magnetic and rotational influences, highlighting the role of parameter β.

Findings

Oblate spheroid shapes develop before expansion wave reaches the core.

Mass infall rate varies with radius and latitude, being higher near the poles.

Core elongation correlates with the magnetic and rotational parameter β.

Abstract

Theoretically, stars have been formed from the collapse of cores in the molecular clouds. Historically, the core had been assumed as an singular isothermal sphere (SIS), and the collapse had been investigated by a self-similar manner. This is while the rotation and magnetic field lead to non-symmetric collapse so that a spheroid shape may be occurred. Here, the resultant of the centrifugal force and magnetic field gradient is assumed to be in the normal direction of the rotational axis, and its components are supposed to be a fraction $\beta$ of the local gravitational force. In this research, a collapsing SIS core is considered to find the importance of the parameter $\beta$ for oblateness of the mass shells which are above the head of the expansion wave. We apply the Adomian decomposition method to solve the system of nonlinear partial differential equations because the collapse does not occur in a spherical symmetry with self-similar behavior. In this way, we obtain a semi-analytical relation for the mass infall rate $\dot{M}$ of the shells at the envelope. Near the rotational axis, the $\dot{M}$ decreases with increasing of the non-dimensional radius $\xi$, while a direct relation is observed between $\dot{M}$ and $\xi$ in the equatorial regions. Also, the values of $\dot{M}$ in the polar regions are greater than the equatorial values, and this difference is more often at smaller values of $\xi$. Overall, the results show that before reaching the head of expansion wave, the visible shape of the molecular cloud cores can evolve to oblate spheroids. The ratio of major to minor axes of oblate cores increases with increasing the parameter $\beta$, and its value can approach to the apparently observed elongated shapes of cores in the maps of molecular clouds such as Taurus and Perseus.