Silicate Emission in the TW Hydrae Association

@article{Sitko2000SilicateEI,
  title={Silicate Emission in the TW Hydrae Association},
  author={Michael L. Sitko and David K. Lynch and R. W. Russell},
  journal={The Astronomical Journal},
  year={2000},
  volume={120},
  pages={2609-2614}
}
The TW Hydrae association is the nearest young stellar association. Among its members are HD 98800, HR 4796A, and TW Hydrae itself, the nearest known classical T Tauri star. We have observed these three stars spectroscopically between 3 and 13 μm. In TW Hya, the spectrum shows a silicate emission feature that is similar to many other young stars' with protostellar disks. The 11.2 μm feature indicative of significant amounts of crystalline olivine is not as strong as in some young stars and… 
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References

SHOWING 1-10 OF 31 REFERENCES
Cometary Dust in the Debris Disks of HD 31648 and HD 163296: Two “Baby” β Pictoris Stars
The debris disks surrounding the pre-main-sequence stars HD 31648 and HD 163296 were observed spectroscopically between 3 and 14 μm. Both stars possess a silicate emission feature at 10 μm that
Discovery of Seven T Tauri Stars and a Brown Dwarf Candidatein the Nearby TW Hydrae Association
We report the discovery of five T Tauri star systems, two of which are resolved binaries, in the vicinity of the nearest known region of recent star formation: the TW Hydrae Association. The newly
Silicate Emission in T Tauri Stars: Evidence for Disk Atmospheres?
We present low-resolution mid-infrared spectra of nine classical T Tauri stars associated with the Cha- maeleon I dark cloud. The data were obtained with the PHOT-S instrument on board the Infrared
Disk Accretion in the 10 Myr Old T Tauri Stars TW Hydrae and Hen 3-600A.
TLDR
It is found that two members of the TW Hydrae association are still actively accreting, based on the ballistic infall signature of their broad Halpha emission profiles, and the first quantitative analysis of accretion in these objects is presented.
The Silicates in the Disk of beta Pictoris
We have obtained intermediate-resolution (R≃50) infrared (2.6-13.5 μm) spectra of the particles in the circumstellar disk of β Pic. The silicate dust feature near 10 μm is broader and contains more
NICMOS narrowband infrared photometry of TW Hydrae association stars
We have obtained 1.64, 1.90, and 2.15 μm narrowband images of five T Tauri stars in the TW Hya Association (TWA) using the Near-Infrared Camera and Multiobject Spectrometer aboard the Hubble Space
10 micron spectroscopy of younger stars in the rho Ophiuchi cloud
Spectra in the 10 micrometer region were obtained of 14 young stars associated with the central core of the rho Oph dark cloud complex. Silicate dust emission and absorption features can be fairly
X-ray and molecular emission from the nearest region of recent star formation.
TLDR
Being at least three times closer to Earth than any well-studied region of star formation, the TW Hya Association serves as a test-bed for the study of x-ray emission from young stars and the formation of planetary systems around sunlike stars.
An infrared spectral match between GEMS and interstellar grains.
TLDR
Infrared spectral properties of silicate grains in interplanetary dust particles were compared with those of astronomical silicates to provide a spectral match to astronomical "amorphous" silicates, one of the fundamental building blocks from which the solar system is presumed to have formed.
Spectral class distribution of circumstellar material in main-sequence stars
A detailed statistical evaluation of IRAS survey data of main-sequence stars within 25 pc indicates that the presence of cool shells around A, F, and G main-sequence stars is the rule, rather than
...
1
2
3
4
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