Star formation is the process by which dense regions within molecular clouds in interstellar space—sometimes referred to as "stellar nurseries" or "star-forming regions"—collapse and form stars. [1]

2024年10月22日 · Stars are giant balls of hot gas – mostly hydrogen, with some helium and small amounts of other elements. Every star has its own life cycle, ranging from a few million to trillions of years, and its properties change as it ages. Stars form in large clouds of gas and dust called molecular clouds.

2025年2月11日 · Star - Formation, Evolution, Lifecycle: Throughout the Milky Way Galaxy (and even near the Sun itself), astronomers have discovered stars that are well evolved or even approaching extinction, or both, as well as occasional stars that must be very young or still in the process of formation.

A star’s mass significantly shapes its formation process. Bigger stars develop faster and burn brighter, and smaller ones take their time and shine steadily. Let’s see how much effect mass has on the formation of stars.

2023年2月2日 · A star is a giant sphere of extremely hot, luminous gas (mostly hydrogen and helium) held together by gravity. A few examples of well-known stars are Pollux, Sirius, Vega, Polaris, and our own Sun. Stars are essentially the building blocks of galaxies and are the source of all the heavier elements.

2023年9月28日 · Webb is addressing several key questions to help us unravel the story of the star and planet formation: How do clouds of gas and dust collapse to form stars? Why do most stars form in groups? Exactly how do planetary systems form?

2023年5月8日 · Outlined below are the steps involved in a star’s evolution, from its formation in a nebula, to its death as a white dwarf or a neutron star. Nebula: a cloud of gas (mostly hydrogen and helium) and dust in space. Nebulae are the birthplaces of stars. Protostar: an early stage of a star formation where nuclear fusion is yet to begin.

Star formation happens in interstellar molecular clouds: opaque clumps of very cold gas and dust. The process starts when some of those clumps reach a critical mass, allowing them to collapse under their own gravity.

Once a star has reached its main-sequence stage, it evolves relatively slowly, fusing hydrogen nuclei in its core to form helium nuclei. Continued fusion not only releases the energy that is radiated but also results in nucleosynthesis, the production of heavier nuclei.

The Orion Nebula is a region of star formation in the Milky Way. Hubble images have revealed "proplyds", discs of dust around newly born stars that are thought to be planetary systems in the early phases of their creation