Boron in the Lithium-Rich K-Giants: A Critical Test of Deep Stellar Mixing Versus Brown-Dwarf Ingestion

Details Boron in the Lithium-Rich K-Giants: A Critical Test of Deep Stellar Mixing Versus Brown-Dwarf Ingestion Boron in the Lithium-Rich K-Giants: A Critical Test of Deep Stellar Mixing Versus Brown-Dwarf Ingestion

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8612d&link_type=abstract

HST Proposal ID #8612

Computer Science

Hst Proposal Id #8612 Cool Stars

Scientific paper

We will observe the B I 2500Angstrom lines in four Li-rich K- giants using HST with STIS/G230M in order to test two different evolutionary scenarios invoked to explain the high Li abundances: the cool bottom process {CBP} versus the possible accretion of brown dwarfs/planets. This test utilizes the two following properties of boron: among the three light elements {Li, Be, and B} which are easily destroyed in stars by {p, Alpha} reactions, B is the least fragile to nuclear destruction. In addition, unlike Li which can be created under certain conditions in stellar mixing, B can only be destroyed. The hypothetical mixing mechanism, CBP, produces Li by introducing deeper mixing to hotter layers such that ^7Li is created via ^3He{alpha, Gamma}^7Be{e^-, anti- Nu}^7Li. A by-product of CBP is the total destruction of pre- existing Be and B. If B I is absent from the spectra, we will prove that deep mixing has occurred. In an accretion scenario, the increase in the Li abundance caused by the deposition of fresh material onto the red giant from a substellar mass companion will also result in an increase in the Be and B abundances. Because B is more robust to nuclear burning than Be, as well as initially being 20 times more abundant, spectroscopy of the B I lines will provide a solid and definitive test of whether the process that creates these chemically peculiar giants is a new type of internal mixing, or the ingestion of a substellar mass companion.

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