Stellar Formation Processes in Molecular Clouds

Star formation unfolds within the cold, dense regions of molecular clouds, vast accumulations of gas and dust that permeate galactic discs. Turbulent motions and magnetic fields within these clouds induce the formation of filamentary structures, within which local density enhancements—known as dense cores—undergo gravitational collapse. As a core contracts, conservation of angular momentum leads to the development of a rotating protostellar disc and the onset of accretion onto a central protostar. Radiative feedback from the nascent star, together with outflows and winds, regulates further accretion and can disperse surrounding material, thereby terminating growth and influencing neighbouring cores. The interplay of gravity, turbulence, magnetic pressure and feedback determines the mass distribution of newly formed stars, or the initial mass function, which in turn shapes the evolution of stellar clusters and entire galaxies. Observations across the electromagnetic spectrum—from infrared tracers of warm dust to radio lines of molecular gas—have revealed that star formation often proceeds in multiple episodes within a single region, giving rise to hierarchical clusters. Recent advances in high-resolution imaging and spectroscopy have deepened our understanding of how feedback mechanisms sculpt molecular clouds, how filaments channel material into cores and how environmental factors such as cloud mass and external pressure influence the efficiency and timescale of stellar birth. The study of these processes is central not only to astrophysics but also to our comprehension of planetary system origins and the chemical enrichment of the interstellar medium.

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Stellar Formation Processes in Molecular Clouds publication trend

The graph below shows the total number of articles in stellar formation processes in molecular clouds across all publications each year (not limited to Nature Index journals).

Technical terms

Molecular cloud: A cold, dense accumulation of gas and dust, primarily molecular hydrogen, serving as the birthplace of stars.

Dense core: A compact region within a molecular cloud where density has risen sufficiently for gravitational collapse to occur.

Protostar: A young stellar object still accreting material from its natal envelope and not yet undergoing sustained hydrogen fusion.

Filament: A elongated, thread-like structure within a molecular cloud that channels matter toward dense cores.

H II region: A volume of ionised gas surrounding hot, young stars, created by their ultraviolet radiation.

Feedback: Processes by which forming stars inject energy and momentum back into the surrounding medium, influencing further collapse and star formation.

References

1. Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49. The Astrophysical Journal Letters (2024).
2. Extension of HOPS out to 500 pc (eHOPS). I. Identification and Modeling of Protostars in the Aquila Molecular Clouds* * HOPS: Herschel Orion Protostar Survey.. The Astrophysical Journal Supplement Series (2023).
3. The SOFIA FEEDBACK [CII] Legacy Survey: Rapid molecular cloud dispersal in RCW 79⋆. Astronomy & Astrophysics (2023).