Low-Mass Star Formation, Triggered by Supernova in Primordial Clouds

The evolution of a gas shell, swept by the supernova remnant of a massive first generation star, is studied with H2 and HD chemistry taken into account and with use of a semi-analytical approximation to the dynamics. When a first-generation star, formed in a parent pregalactic cloud, explodes as a supernova with explosion energy in the range of 10erg− 10 erg at redshifts of z = 10− 50, H2 and HD molecules are formed in the swept gas shell at fractional abundances of ∼ 10 and ∼ 10, respectively, and effectively cool the gas shell to temperatures of 32K− 154 K. If the supernova remnant can sweep to gather the ambient gas of mass 6× 10M⊙ − 8× 10 5 M⊙, the gas shell comes to be dominated by its selfgravity, and hence, is expected to fragment. The amount of swept gas necessary for fragmentation increases with the explosion energy and decreases with the [email protected] [email protected] [email protected] [email protected]