Hydrogen is the most abundant element in the universe and constitutes the majority of the mass in nebulae. It serves as the raw material for star formation.

Star formation begins with the gravitational collapse of dense regions within nebulae, known as molecular clouds. As the cloud collapses, it accumulates mass and heats up, eventually triggering nuclear fusion at its core.

Dust particles in nebulae provide a surface for chemical reactions to occur, leading to the formation of complex molecules and eventually the building blocks of stars.

Dark nebulae are dense regions of gas and dust that block visible light, making them appear dark. They are often associated with the early stages of star formation, as they provide a suitable environment for the gravitational collapse of molecular clouds.

Accretion is the process by which a protostar accumulates mass from the surrounding nebula. As the protostar grows in size, its gravitational pull becomes stronger, attracting more gas and dust from the nebula.

M-type stars are low-mass stars, typically referred to as red dwarfs. They are not typically formed within nebulae, which are more conducive to the formation of massive stars.

The mass of a star formed in a nebula is primarily determined by the initial density of the molecular cloud. Denser regions collapse more rapidly and form more massive stars.

Emission nebulae emit intense ultraviolet radiation due to the presence of ionized hydrogen gas. This radiation excites the surrounding gas, causing it to emit light.

Bipolar outflows are powerful jets of gas and dust ejected from the protostar along its rotational axis. They help expel excess angular momentum from the protostar, allowing it to continue accreting mass and grow in size.

Sodium Chloride (NaCl) is not a common type of molecule found in nebulae. It is a salt compound typically found in terrestrial environments.

During its early stages of formation, a protostar typically has a temperature range of 1,000 - 10,000 Kelvin.

Planetary nebulae are not star clusters. They are the remnants of evolved stars that have shed their outer layers, revealing their hot cores.

Main Sequence Ignition is the process by which a protostar becomes a fully-fledged star. It occurs when the protostar reaches a critical mass and temperature, triggering nuclear fusion reactions in its core.

The distance to the nearest galaxy is not a direct factor that influences the rate of star formation in a nebula.