Magnetic Fields in Molecular Clouds: ARIES Study on Star Formation

Scientists have “seen” the skeleton of the magnetic field surrounding small molecular clouds L1604 and L121 for the first time.

• Study conducted by Aryabhatta Research Institute of Observational Sciences (ARIES), Department of Science and Technology (DST)  in collaboration with Assam University.
• Methodology: R-band polarimetry using ARIES Imaging Polarimeter (AIMPOL) on the 104-cm ARIES telescope, Nainital.

Key Findings

• Magnetic field strength: Both clouds are sub-critical, meaning magnetic energy dominates over turbulence and gravity at the envelope scale.
• Dense cores: Despite overall magnetic protection, gravity may dominate in the dense cores, making them sites for star formation.
• Differences between clouds:
  • L1604: Massive and dense, magnetic field less ordered.
  • L121: Less dense, magnetic field strong and orderly, less affected by gravitational collapse.
• Magnetic fields act as an invisible hand, slowing star formation and preventing rapid gas depletion in the galaxy.

Significance of the Study

• Star formation regulation: Shows that magnetism controls the pace of star birth in molecular clouds.
• Galaxy evolution: Prevents all gas from collapsing into stars simultaneously, maintaining a stable star formation rate.
• Observational breakthrough: First direct mapping of magnetic skeleton in small molecular clouds.
• Future research: Helps understand the interplay of gravity, turbulence, and magnetic fields in star formation.

About Molecular Clouds

• Molecular clouds are cold, dense regions of interstellar gas and dust where molecules, especially molecular hydrogen (H₂), form and survive.
• They are often called “stellar nurseries” because they are the primary sites of star formation in galaxies.

• For Example:
  • Orion Molecular Cloud Complex – Nearby star-forming region.
  • Taurus Molecular Cloud – Rich in low-mass star formation.
  • L1604 and L121 – Small molecular clouds recently studied for magnetic fields.

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L1604 and L121: Molecular Clouds

Key Features

• Temperature: Very cold, typically 10–30 K, allowing molecules to exist.
• Density: High compared to other interstellar regions, typically 100–1,000,000 particles per cm³.
• Composition: Mainly molecular hydrogen (H₂), with helium, CO, and traces of other molecules; dust grains make up 1% of the mass.
• Size: Range from small Bok globules (1–5 light-years) to giant molecular clouds (GMCs, 10–100 light-years).
• Mass: Can range from a few solar masses (small clouds) to millions of solar masses (GMCs).

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Importance of Molecular Clouds 

• Birthplace of Stars: Molecular clouds act as stellar nurseries, where gravitational collapse of dense regions leads to star formation.
  • They are essential for the continuous creation of new stars in galaxies like the Milky Way.
• Role in Planetary System Formation: The same collapsing cores that form stars also lead to the formation of protoplanetary disks, which eventually give rise to planets and solar systems.
• Regulation of Star Formation: Molecular clouds regulate the rate of star formation through the interplay of gravity, thermal pressure, turbulence, and magnetic fields.
  • This prevents rapid depletion of galactic gas reserves.
• Contribution to Galactic Evolution: They serve as reservoirs of gas and dust, influencing the structure and evolution of galaxies over time.
  • Star formation within these clouds determines the stellar population and lifecycle of galaxies.
• Chemical Enrichment of the Universe: Molecular clouds contain complex molecules (e.g., CO, organic compounds) that contribute to the chemical evolution of the universe.
  • They are sites where prebiotic molecules may form.

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