質問: この英文の和訳をお願いします。 the second feature seen from fig.11 is that the profile of r(e,0) does not depend significantly on r_p (for r_p=0.005 to 0.0002). only an exception is found near e≒1, but this is, in some sense, a singular point in r(e,0), which appears in a narrow region around e≒1 ( in fact, for e=0.9 and 1.2, there is no appreciable difference between r_p=0.005 and 0.0002). thus, neglecting such fine structures in r(e,0), we can conclude that r(e,0) does depend very weakly on r_p. in other words, the dependence on r_p of is well approximated by that of _2b given by eq. (28). now, we will phenomenalogically show what physical quantity is related to the peak at e≒1. we introduce the collisional flux f(e,e) for orbits with e and e, where e is the jacobi energy given by (see eq. (15)) e=e^2/2-(3b^2)/8+9/2. (31) the collisional flux f(e,e) is defined by f(e,e)=(2/π)∫【‐π→π】p_col(e,i=0, b(e), τ)dτ. (32) from eqs. (11) and (31), we obtain =∫f(e,e)de. (33) in fig.12, f(e,e) is plotted as a function of e for the cases of e=0, 0.5, 1.0, and 2.0. we can see from this figure that in the case of e=1 a large fraction of low energy planetesimals contributes to the collisional rate compared to other cases (even to the cases with e<1). in general, in the case of high energy a solution for the three-body problem can be well described by the two-body approximation: in other words, in the case of low energy a large difference would exist between a solution for the three-body problem and that in the two-body approximation. as shown before, this difference appears as an enhancement of the collisional rate. thereby an enhancement factor peak is formed at e≒1 where a large fraction of low-energy planetesimals contributes to the collisional rate. よろしくお願いいたします。
回答: ddeanaです。訳に間違いがありました。 ×planetesimal:原始惑星→〇微惑星 お詫びして、訂正いたします。