Chondrules are one of the most primitive elements that can serve as a fundamental clue as to the origin of our Solar system .
We investigate a formation scenario of chondrules that involves planetesimal collisions and the resultant impact jetting .
Planetesimal collisions are the main agent to regulate planetary accretion that corresponds to the formation of terrestrial planets and cores of gas giants .
The key component of this scenario is that ejected materials can melt when the impact velocity between colliding planetesimals exceeds about 2.5 km s ^ { -1 } .
The previous simulations show that the process is efficient enough to reproduce the primordial abundance of chondrules .
We examine this scenario carefully by performing semi-analytical calculations that are developed based on the results of direct N -body simulations .
As found by the previous work , we confirm that planetesimal collisions that occur during planetary accretion can play an important role in forming chondrules .
This arises because protoplanet-planetesimal collisions can achieve the impact velocity of about 2.5 km s ^ { -1 } or higher , as protoplanets approach the isolation mass ( M _ { p,iso } ) .
Assuming that the ejected mass is a fraction ( F _ { ch } ) of colliding planetesimals ’ mass , we show that the resultant abundance of chondrules is formulated well by F _ { ch } M _ { p,iso } , as long as the formation of protoplanets is completed within a given disk lifetime .
We perform a parameter study and examine how the abundance of chondrules and their formation timing change .
We find that the impact jetting scenario generally works reasonably well for a certain range of parameters , while more dedicated work would be needed to include other physical processes that are neglected in this work and to examine their effects on chondrule formation .