Circumstellar Disks in the IR: Identification of New Systems and Evidence of Complex Density Structures

Details Circumstellar Disks in the IR: Identification of New Systems and Evidence of Complex Density Structures Circumstellar Disks in the IR: Identification of New Systems and Evidence of Complex Density Structures

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.0803w&link_type=abstract

American Astronomical Society Meeting 206, #08.03; Bulletin of the American Astronomical Society, Vol. 37, p.440

Astronomy and Astrophysics

Astronomy

Scientific paper

We use 0.8-2.4 micron spectroscopy to explore the circumstellar environments of a small sample of stars in the Galactic clusters NGC 2186 and NGC 2439 that were previously identified as excess Hα emitters from 2-color diagram photometric observations. We detect both H I and various metal emission lines in ˜60% of our sample, indicating that these objects do have circumstellar disks. Analysis of line profile morphologies suggests the presence of a one-armed spiral density wave in at least one circumstellar disk system. Furthermore, we find the V/R ratios of the H I Brackett emission lines are opposite those of the Fe II emission lines in this particular system, implying that our observations may be used to probe the structure of the spiral density wave as a function of disk radius.
We also present initial results of near contemporaneous optical and 0.8-2.4 micron spectroscopic observations of several known Galactic classical Be stars. Theoretical line profile calculations (Waters & Marlborough 1992) predict scenarios in which one should observe the V/R ratios of the optical Hα and IR H lines to be oppositely oriented; we believe we have found conclusive evidence of this in our observations of Zeta Tau. We discuss our efforts to use these line strengths and profiles to constrain the density structure and fundamental parameters of these circumstellar disks.
Observations were obtained using the SpeX instrument at the NASA IRTF on Mauna Kea, Hawaii. This work has been supported in part by grants from the NASA LTSA, NASA GSRP, Sigma Xi GIAR, and NSF REU programs. KSB is a Cottrell Scholar of the Research Corporation and gratefully acknowledges their support.

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