Do Young Stars Accrete Rocky Planetary Material?

Details Do Young Stars Accrete Rocky Planetary Material? Do Young Stars Accrete Rocky Planetary Material?

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009noao.prop..456d&link_type=abstract

NOAO Proposal ID #2009B-0456

Computer Science

Scientific paper

The accretion of rocky material in early stellar life could be an incisive new probe of planetary formation yet observational evidence for the process is lacking. We will use hectoechelle to seek abundance anomalies characteristic of accreted rocky material among many early F- stars in the 13 Myr old clusters h and (chi) Per. These are optimal as they have recently arrived on the main sequence, should be in the midst of planet formation and have thin convection zones, minimizing dilution of any accretion signatures. We will: (i) find accreted material, opening new windows on comparative planetary formation by studying its frequency, quantity and composition; or (ii) find nothing, concluding either that much less than an Earth mass of rocky material is accreted, contradicting current planetary formation ideas, or that hitherto neglected mixing mechanisms act on short timescales to dilute accreted material.

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