  It has recently been suggested that, in the field, $\sim\!\!56\%$ of Sun-like
stars ($0.8\,{\rm M}_{_\odot}\lesssim M_\star\lesssim 1.2\,{\rm M}_{_\odot}$)
are single. We argue here that this suggestion may be incorrect, since it
appears to be based on the multiplicity frequency of systems with Sun-like
primaries, and therefore takes no account of Sun-like stars that are secondary
(or higher-order) components in multiple systems. When these components are
included in the reckoning, it seems likely that only $\sim\!46\%$ of Sun-like
stars are single. This estimate is based on a model in which the system mass
function has the form proposed by Chabrier, with a power-law Salpeter extension
to high masses; there is a flat distribution of mass ratios; and the
probability that a system of mass $M$ is a binary is $\,0.50 +
0.46\log_{_{10}}\!\left(M/{\rm M}_{_\odot}\right)\,$ for $\,0.08\,{\rm
M}_{_\odot}\leq M\leq 12.5\,{\rm M}_{_\odot}$, $\,0\,$ for $\,M<0.08\,{\rm
M}_{_\odot}$, and $\,1\,$ for $\,M>12.5\,{\rm M}_{_\odot}$. The constants in
this last relation are chosen so that the model also reproduces the observed
variation of multiplicity frequency with primary mass. However, the more
qualitative conclusion, that a minority of Sun-like stars are single, holds up
for virtually all reasonable values of the model parameters. Parenthetically,
it is still likely that the majority of {\it all} stars in the field are
single, but that is because most M Dwarfs probably are single.
