Helium preenrichment in the star-forming regions

Abstract

We show that element diffusion can produce large fluctuations in the initial helium abundance of the star-forming clouds. Diffusion time-scale, which in stars is much larger than the Hubble time, can fall below 10^8 years in the neutral gas clouds dominated by collisionless dark matter or with dynamically important radiation or magnetic pressure. Helium diffusion may therefore explain the recent observations of globular clusters, which are inconsistent with initially homogeneous helium distribution.

arXiv comment4 pages, accepted by MNRAS (Letters)

References in corpus (6)

• Relativistic gravitation theory for the MOND paradigm
• Omega Centauri: The Population Puzzle Goes Deeper
• Metallicities on the Double Main Sequence of omega Centauri Imply Large Helium Enhancement
• Super Helium-Rich Population and the Origin of Extreme Horizontal-Branch Stars in Globular Clusters
• The origin of the double main sequence in Omega Centauri: Helium enrichment due to gas fueling from its ancient host galaxy ?
• Helium self--enrichment and the second parameter problem in M3 and M13

Cited by in corpus (6)

• Horizontal Branch Stars: The Interplay between Observations and Theory, and Insights into the Formation of the Galaxy
• Origin of multiple stellar populations in globular clusters and their helium enrichment
• Deep FORS1 observations of the double Main Sequence of omega Centauri
• On the Origin of Bimodal Horizontal-Branches in Massive Globular Clusters: The Case of NGC 6388 and NGC 6441
• The chemical evolution of Omega Centauri's progenitor system
• Testing the AGB Scenario as the Origin of the Extreme-Helium Population in omega Centauri