SETI public: Understanding our Origins: Star Formation in H II Region Environments

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From: LARRY KLAES (ljk4_at_msn.com)
Date: Fri Jun 10 2005 - 08:55:20 PDT

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    Paper: astro-ph/0506190
    Date: Thu, 9 Jun 2005 00:27:34 GMT (366kb)

    Title: Understanding our Origins: Star Formation in H II Region Environments

    Authors: J. Jeff Hester & Steven J. Desch (Dept. of Physics & Astronomy,
      Arizona State University)
    Comments: 25 pages, 10 figures. Refereed and accepted submission of an
    invited
      presentation to the Proceedings from the Workshop on Chondrites and the
      Protoplanetary Disk, Kaua'i Hawai'i, November 8-11, 2004. ASP conference
      series, editors A. Krot, E. Scott, & B. Reipurth. Higher quality copy
      available at http://eagle.la.asu.edu/hester/kauai/kauai_hester_final.pdf
    \\
      Recent analysis of the decay products of short-lived radiounclides (SLRs)
    in
    meteorites, in particular the confirmation of the presence of live 60Fe in
    the
    early Solar System, provides unambiguous evidence that the Sun and Solar
    System
    formed near a massive star. We consider the question of the formation of
    low-mass stars in environments near massive stars, presenting a scenario for
    the evolution of a star and its disk around the periphery of an expanding H
    II
    region. The stages in this scenario begin with compression of molecular gas
    around the edge of an H II region, continue as forming stars are overrun by
    the
    advancing ionization front, and culminate when ejecta from one or more
    nearby
    supernova explosions sweeps over YSO disks located in the low density
    interior
    of the H II region, injecting SLRs including 26Al and 60Fe. We review the
    evidence that this mode of star formation is more characteristic of
    formation
    of low-mass stars than is the mode of star formation seen in regions such as
    the Taurus-Auriga molecular cloud. We discuss the implications of this
    scenario
    for our understanding of star formation, as well as the effects of the young
    Sun's astrophysical environment on the formation and evolution of the Solar
    System. We conclude that low-mass stars and their accompanying disks form
    and
    evolve very differently near massive stars than they do in regions like
    Taurus-Auriga, and that these differences have profound implications for our
    understanding of our origins.

    \\ ( http://arXiv.org/abs/astro-ph/0506190 , 366kb)

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