At present , the best model for the evolution of the cosmos requires that dark matter make up approximately 25 \% of the energy content of the Universe .
Most approaches to explain the microscopic nature of dark matter , to date , have assumed its composition to be of intrinsically weakly interacting particles ; however , this need not be the case to have consistency with all extant observations .
Given decades of inconclusive evidence to support any dark matter candidate , there is strong motivation to consider alternatives to the standard particle scenario .
One such example is macro dark matter , a class of candidates ( macros ) that could interact strongly with the particles of the Standard Model , have large masses and physical sizes , and yet behave as dark matter .
Macros that scatter completely inelastically could have altered the primordial production of the elements , and macro charge-dependent constraints have been obtained previously .
Here we reconsider the phenomenology of inelastically interacting macros on the abundance of primordially produced ^ { 4 } \text { He } and revise previous constraints by also taking into account improved measurements of the primordial ^ { 4 } \text { He } abundance .
The constraints derived here are limited in applicability to only leptophobic macros that have a surface potential V ( R _ { \text { \tiny X } } ) \gtrsim 0.5 \text { MeV } .
However , an important conclusion from our analysis is that even neutral macros would likely affect the abundance of the light elements .
Therefore , constraints on that scenario are possible and are currently an open question .