The Structure and Kinematics of Irradiated Disks and Associated High Velocity Features in Orion

Details The Structure and Kinematics of Irradiated Disks and Associated High Velocity Features in Orion The Structure and Kinematics of Irradiated Disks and Associated High Velocity Features in Orion

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8324b&link_type=abstract

HST Proposal ID #8324

Physics

Hst Proposal Id #8324 Young Stars And Circumstellar Material

Scientific paper

STIS provides us with a unique opportunity to study the early evolution of proto-planetary disks and their chances of survival in the harsh irradiated environments of OB associations where most stars form. We seek to test new circumstellar disk photo-erosion models for the Orion Nebula proplyds {proto-planetary disks}, to measure the disk mass loss rates, the nature of their tails, and the high excitation upstream bow shocks {HAlpha + ionO3 arcs}. We will obtain long-slit low dispersion UV spectra to measure the relative intensities of a variety of UV lines that trace the excitation conditions in the circumstellar disk, neutral outflow, and in the ionized zone and to search for OH emission predicted by a recent model of photo-chemical excitation of the 6300Angstrom ionO1 line. We will obtain moderate resolution long slit visible spectra to constrain the sub-arcsecond structure and excitation conditions in the proplyds, search for disk rotation, estimate disk wind velocities, and measure the flow velocities as a function of position, excitation, and ionization and in various portions of the photo-ablation flow. We will measure the velocity fields of several supersonic micro-jets powered by the Orion proplyds. Our data will constrain the survival time of irradiated disks, address their potential for forming planetary systems, and shed light on the planetary system formation frequency.

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