  Helium variations are common features of globular clusters (GCs) with
multiple stellar populations. All the formation scenarios predict that
secondary population stars are enhanced in helium but the exact helium content
depends on the polluters. Therefore, searching for helium variations in a star
cluster is a straightforward method to understand if it hosts multiple
populations or not, and constrain the formation scenario. Although this topic
has been well explored for Galactic GCs, GCs beyond the Milky Way are
challenging to study because of their large distances. This work studies the
helium distribution of GK-type main sequence dwarfs in an old ($\sim$12.5 Gyr)
GC in the Large Magellanic Cloud, NGC 2210, using the deep photometry observed
by the {\sl Hubble Space Telescope}. We compare the observed morphology of the
MS with that of synthetic populations with different helium distributions. We
confirm that NGC 2210 dwarfs have a helium spread, with an internal dispersion
of $\delta{Y}\sim$0.06--0.07. The fraction of helium enriched stars depends on
the $\delta{Y}$ distribution. A continuous $\delta{Y}$ distribution would
indicate that more than half of MS stars are helium enriched ($\sim$55\%). If
the $\delta{Y}$ distribution is discrete (bimodal), a fraction of $\sim$30\%
enriched stars is able to explain the observed morphology of the MS. We also
find that the He-enriched population stars are more centrally concentrated than
He-normal stars.
