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It is dark matter composed of constituents with an FSL much smaller than a protogalaxy. This is the focus for dark matter research, as hot dark matter does not seem capable of supporting galaxy or galaxy cluster formation, and most particle candidates slowed early. The constituents of cold dark matter are unknown.
To play the role of dark matter, the darkon field must interact weakly with the standard matter field sector and should not rapidly decay into particles. The simplest way of introducing the darkon is to demand that they can only be annihilated or created in pairs and to make it stable against decay.
Dark matter is called ‘dark’ because it’s invisible to us and does not measurably interact with anything other than gravity. It could be interspersed between the atoms that make up the Earth ...
It is due to dark matter that galaxies are able to keep their shape, with the mass of dark matter creating enough gravitational force to hold the stars that make up a galaxy together. Dark energy, however, is a substance or force responsible for the accelerating expansion of the universe over time. [2]
The founding principle of direct dark matter detection is that since dark matter is known to exist in the local universe, as the Earth, Solar System, and the Milky Way Galaxy carve out a path through the universe they must intercept dark matter, regardless of what form it takes. Direct detection of dark matter faces several practical challenges.
Dark matter makes up most of the universe and decides how it grows – but still remains mostly mysterious
The dark matter can be modeled as a scalar field using two fitted parameters, mass and self-interaction. [4] [5] In this model the dark matter consists of an ultralight particle with a mass of ~10 −22 eV when there is no self-interaction.
The discrepancies could also be explained by particular properties (stellar masses or effective volume) of the candidate galaxies, yet unknown force or particle outside of the Standard Model through which dark matter interacts, more efficient baryonic matter accumulation by the dark matter halos, early dark energy models, [102] or the ...