Indian Institute of Technology Palakkad&nbsp;(IIT Palakkad or IIT PKD) is a public autonomous&nbsp;engineering&nbsp;and&nbsp;research&nbsp;institute located in&nbsp;Palakkad,&nbsp;Kerala. It was&nbsp;one of the five new&nbsp;IITs&nbsp;proposed in the&nbsp;2014 Union budget of India. The campus was inaugurated on 3 August 2015. The institute has 94 faculty, 978 students, and 63 non-teaching staffs.

IT Palakkad currently offers four-year Bachelor of Technology (B.Tech) and two years MS programmes in 8 different engineering disciplines including&nbsp;Computer Science, Electrical, Mechanical, Civil among others.

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IIT Palakkad

We present two new primary mechanisms for the synthesis of the rare nucleus Be9, both triggered by ν-induced production of H3 followed by He4(H3,γ)Li7 in the He shells of core-collapse supernovae. For progenitors of ∼8MâŠ™, Li7(H3,n0)Be9 occurs during the rapid expansion of the shocked He shell. Alternatively, for ultra-metal-poor progenitors of ∼11-15MâŠ™, Li7(n,γ)Li8(n,γ)Li9(e-ν̄e)Be9 occurs with neutrons produced by He4(ν̄e,e+n)H3, assuming a hard effective ν̄e spectrum from oscillations (which also leads to heavy element production through rapid neutron capture) and a weak explosion (so the Be9 survives shock passage). We discuss the associated production of Li7 and B11, noting patterns in LiBeB production that might distinguish the new mechanisms from others. © 2013 American Physical Society.

Department of Physics

World University root node

Fulltext

Physical Review Letters

New primary mechanisms for the synthesis of rare be9 in early supernovae

Neutrino-Induced Production of 9Be in Core-Collapse Supernovae

University of Minnesota

Neutrino-induced Neucleosynthesis in Supernova Helium Shells

We revisit a ν-driven r-process mechanism in the He shell of a core-collapse supernova, finding that it could succeed in early stars of metallicity Z10 -3Z, at relatively low temperatures and neutron densities, producing A 130 and 195 abundance peaks over ∼10-20s. The mechanism is sensitive to the ν emission model and to ν oscillations. We discuss the implications of an r process that could alter interpretations of abundance data from metal-poor stars, and point out the need for further calculations that include effects of the supernova shock. © 2011 American Physical Society.