•The concept of dark matter and the difficulty of measurement Oscuro matter is the name given to hypothetical substances in astrophysics that do not interact with electromagnetic waves and whose existence can only be determined by their gravitational effects on other matter. To determine the existence of these substances, we use the rotational speeds of galaxies, the orbital speeds of galaxies within other galaxies, the gravitational lensing properties they exert on background matter, and the temperature distribution of hot gases within galaxies.
Among the possible astrophysical objects in halos are stellar remnants, neutron stars, faint stars such as white dwarfs, even black holes and objects that never managed to become stars due to their small masses. These objects are ideal candidates for dark matter because they are either completely or almost completely invisible. Moreover, since their existence is known for certain, MACHOs are more suitable as dark matter candidates than WIMPs.
Oscuro matter is thought to exist in two forms: baryonic dark matter and non-baryonic dark matter. Although it is estimated to make up 90% of the mass of the universe, the nature of dark matter remains a mystery to astronomers. Non-baryonic dark matter is divided into two main categories: hot dark matter (HDM), which is the relativistic (near the speed of light) motion of non-baryonic particles, and cold dark matter (CDM), which is the non-relativistic motion of non-baryonic particles. Cold dark matter particles are also known as WIMPs.
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