  We review important reactions in the big bang nucleosynthesis (BBN) model
involving a long-lived negatively charged massive particle, $X^-$, which is
much heavier than nucleons. This model can explain the observed $^7$Li
abundances of metal-poor stars, and predicts a primordial $^9$Be abundance that
is larger than the standard BBN prediction. In the BBN epoch, nuclei recombine
with the $X^-$ particle. Because of the heavy $X^-$ mass, the atomic size of
bound states $A_X$ is as small as the nuclear size. The nonresonant
recombination rates are then dominated by the $d$-wave $\rightarrow$ 2P
transition for $^7$Li and $^{7,9}$Be. The $^7$Be destruction occurs via a
recombination with the $X^-$ followed by a proton capture, and the primordial
$^7$Li abundance is reduced. Also, the $^9$Be production occurs via the
recombination of $^7$Li and $X^-$ followed by deuteron capture. The initial
abundance and the lifetime of the $X^-$ particles are constrained from a BBN
reaction network calculation. We estimate that the derived parameter region for
the $^7$Li reduction is allowed in supersymmetric or Kaluza-Klein (KK) models.
We find that either the selectron, smuon, KK electron or KK muon could be
candidates for the $X^-$ with $m_X\sim {\mathcal O}(1)$ TeV, while the stau and
KK tau cannot.
