So it's low in terms of "amount of energy in relation to amount of hydrogen in the star"? But wouldn't much of the un-fused hydrogen be eligible to fuse at some

So it's low in terms of "amount of energy in relation to amount of hydrogen in the star"? But wouldn't much of the un-fused hydrogen be eligible to fuse at some later time, if for instance convection streams pull it down into the deeper (=higher-pressure) zones of the star? So it seems to me the relevant measurement ought to be the ratio of energy per hydrogen atoms fused, not hydrogen atoms total. (Certainly in a reactor, where presumably all or most of them should be.)