Terrence W. Rettig
Astronomy and Astrophysics
B.A., Physics, Mathematics, Defiance College, 1968
M.S., Physics, Ball State University, 1970
Ph.D., Astrophysics, Indiana University, 1976
E-mail: trettig (at) nd (dot) edu
Address: Nieuwland Science Hall 330
Phone: (574) 631-7732
Fax: (574) 631-5952
Planet formation has been known for many years to be tied to the accretion and evolution of gas and dust in disks around young HAeBe and T Tauri stars. This early stage of stellar evolution occurs after the shell around an embedded protostar collapses to form a preplanetary disk, revealing a pre-main-sequence star representative of the Sun when our solar system was forming. This research program uses high-resolution spectra of ices, dust, and gas phase molecules in the disks of these pre-main sequence stars to study the physical conditions in young stars in the planet forming regions. The abundance and excitation of these molecules can be used to clarify the time scales and initial conditions for planet building. Infrared spectroscopic data are obtained from the Infrared Telescope (IRTF) and the 10 meter Keck Telescope on Mauna Kea.
Using high-resolution infrared observations of CO, we are providing the first direct observational verification of the stratification of gas and dust in disks around young stellar objects (YSOs). How dust settles to the midplane is essential to understanding the initial constraints on planetesimal and planet formation. The physical structure of extended flared disks around YSOs depends on a variety of parameters including the extent of gas and dust mixing (i.e. turbulence), the rate of dust settling and the process of grain coagulation. In general, dust settling and grain growth are expected to occur throughout the upper disk atmosphere until a balance is reached with diffusion (turbulence) near the midplane. Even theoretically, these processes are only superficially understood as observational constraints have remained elusive.
We also have begun a program to observe and model the outbursting young stars referred to as FU Ori and EX Lup objects. The IR CO emission lines provide excellent ways to monitor the temperature and structure of the inner disk and we use several atomic lines to provide a measure of the wind velocities and accretion rate. These objects provide a unique insight into how the disk forms and mass accretes onto the star.
“Dust Settling in Magnetorotationally Driven Turbulence,” D.S. Balsara, D.A. Tilley, T. Rettig, and S.A. Brittain, MNRAS (2009) astro-ph/arXiv:0810.0246
“Post-Outburst Observations of V1647 Orionis: Detection of a Brief Warm Molecular Outflow,” S. Brittain, T.W. Rettig, T. Simon, D.S. Balsara, D. Tilley, E. Gibb, and K.H. Hinkle, Astrophysical Journal 670, L29-L32 (2007)
“Warm Gas in the Inner Disks around Young Intermediate-Mass Star,” S.D. Brittain, T. Simon, J.R. Najita, and T.W. Rettig, ApJ 659, 685 (2007)
“Dust Stratification in Young Circumstellar Disks,” T. Rettig, S. Brittain, T. Simon, E. Gibb, D.S. Balsara, D.A. Tilley, and C. Kulesa, Astrophysical Journal 646, 342-350, (2006)
“CO Emission and Absorption toward V1647 Orionis (McNeil’s Nebula),” T.W. Rettig, S.D. Brittain, E.L. Gibb, T. Simon, and C. Kulesa, Astrophysical Journal 626, 245-252 (2005)
“Discovery of CO Gas in the Inner Disk of TW Hydrae,” T.W. Rettig, J. Haywood, T. Simon, S.D. Brittain, and E. Gibb, Astrophysical Journal 616, L163-L166 (2004)
Full Curriculum Vitae (pdf)
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