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Early stage of stellar evolution where a contracting cloud of gas and dust has not yet reached conditions for nuclear fusion. Understanding protostars helps explain the formation of stars.

The matter and radiation that exist in the space between the star systems in a galaxy. It plays a crucial role in star formation and the evolution of the galaxy.

The life cycle of a star from its formation to its death. It's important for understanding the various stages stars go through, including main sequence, red giant, and supernova events.

The formation of chemical elements in stars through nuclear fusion and supernova explosions. It's important for creating the heavier elements in the universe.

A highly magnetized, rotating neutron star that emits beams of electromagnetic radiation out of its magnetic poles. Pulsars are important as precise cosmic clocks and for studying the physics of extreme environments.

A plot of stellar luminosity against surface temperature (or color). It’s a fundamental tool for classifying stars and understanding stellar evolution.

Massive stars that have left the main sequence and entered a phase of expansion and high luminosity. They are important for the role they play in supernovae and forming some of the heaviest elements.

Explosive events signifying the end stages of massive stars, resulting in the ejection of the star's outer layers. These events are important for dispersing elements into the cosmos and can trigger new star formation.

The balance between the outward pressure force and the inward gravitational force in a star. It's crucial to maintain a star's structure and prevent it from collapsing or expanding uncontrollably.

The process that powers stars by combining lighter elements into heavier ones, releasing energy in the process. It's the source of a star's energy and determines its lifecycle.

A region of spacetime exhibiting gravitational acceleration so strong that nothing—no particles or even electromagnetic radiation such as light—can escape from it. Vital for studying general relativity and the end states of massive stars.

The phase in stellar evolution where a star is fusing hydrogen into helium in its core. Represents a star's longest and most stable period, determining its position in the Hertzsprung-Russell diagram.

The radiation emitted by an object that absorbs all incident electromagnetic radiation regardless of frequency or angle of incidence. It’s essential for understanding stellar temperatures and luminosities.

The stage in a star's life characterized by its expansion and cooling after hydrogen in the core is exhausted. It's important for the eventual shedding of a star's outer layers and the seeding of interstellar medium with elements.

The incredibly dense remnants of supernova explosions, composed primarily of neutrons. They are important for extreme physics research, such as quantum degeneracy and relativistic effects.

A principle stating that the total energy radiated per unit surface area of a black body is proportional to the fourth power of its temperature. Key for understanding how brightness and temperature relate for stars.

Stellar remnants consisting mostly of electron-degenerate matter. They represent the final evolutionary state of low- to medium-mass stars, where no fusion occurs.

A system classifying stars based on their spectral characteristics and temperature. This classification aids in determining stellar temperatures, compositions, and evolutionary stages.

The maximum mass ($\approx 1.4$ solar masses) that a white dwarf star can have before collapsing into a neutron star or black hole. It is crucial for understanding the fate of intermediate-mass stars.