Other
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.1003b&link_type=abstract
American Astronomical Society Meeting 208, #10.03; Bulletin of the American Astronomical Society, Vol. 38, p.89
Other
Scientific paper
A significant number of the nearby single active dwarf stars are members of the Local Association, which is a widespread aggregate of young stars related to star formation in the Sco-Cen association. The ages of stars within the Local Association span a range of 8-150 Myr, but the subgroups have much narrower age spreads. The older portions of the Local Association include the Pleiades and Alpha Per clusters. Younger subgroupings of the Local Association include the Beta Pic [age 12Myr] and Tucana-Horologium [age 30Myr] moving groups. By ages of 12 Myr, circumstellar disks and associated protoplanetary systems are at an extremely interesting stage of evolution with gas giant formation well under way and terrestrial planets starting to form. The high energy radiation and particle (wind+flare) emission from the central star plays an important role in the evolution of these disks. The crucial EUV radiation field that photoioizes protoplanetary disks and atmospheres is dominated by transition region ( 105 K) emission lines, such as He I 584, 537 A, He II 304 A, N III 686 A, O III 600, 703 A, O IV 556, 610, 790 A, O V 630, 760 A, Ne VIII 780 A, and sub-coronal emissions such as Mg IX 368 A and Mg X 610, 625 A. These emission lines are unobservable because of strong absorption by the interstellar medium and their strengths must be estimated from UV observations of other emission lines from the same ions or ions formed at similar temperatures. We are currently undertaking a FUSE Cycle 6/7 Legacy project to study the Beta Pic moving group and a large Cycle 7 Survey project to investigate the Tucana-Horologium moving group. We present the current status of these projects and discuss the O VI and C III emission line properties observed.
Ayres Thomas R.
Brown Alexander
Harper Graham M.
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