Computer Science
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop..199h&link_type=abstract
Spitzer Proposal ID #199
Computer Science
Scientific paper
Massive stars ending in the Wolf-Rayet (WR) phase of advanced core-burning may drive star formation and dramatically influence the energy budget, kinematics, and chemistry of active star forming environments in galaxies, in the cores of some active galaxies, and our Galactic Center where the massive star content is high. The dust properties of these environments are affected by production of oxygen- and carbon-rich dust during the WN, WC, and related Luminous Blue Variable phases. However, the dust and gas in the compact carbonaceous dust shells around WC-type stars, and in the extended nebula around WN type stars (the precursors to WCs) are poorly studied. In particular, no thermal IR spectroscopy of O-rich dust in nebulae around WN stars is available, but there are indications from ISO observations of WR galaxies that they may be strong contributors of crystalline silicates, a possibility also supported by the dust content of less-evolved LBV nebulae. WC dust spectra are limited to only the 5 brightest WC9-type stars (ISO), and several additional late WC's at much reduced spectral coverage (SCORE, 8-13 micron). We are pursuing spectroscopy of previously unobserved dusty WR stars, including four compact dusty WC-type stars, with high resolution and SL spectroscopy to analyze the dust grain properties and composition along the early-type to late-type WC sequence. We can address the debate on the ISM vs. circumstellar nature of the 6.3um aromatic band. We will also do high resolution spectroscopy of the WN central stars, employng non-LTE model atmospheres to demonstrate how the mid-infrared spectrum can be quantatively analyzed to derive the fundamental stellar and wind parameters, and spectrally map the surrounding ring nebulae at low resolution for first results on WN dust. We can use H2 detections (reported only at 2.12 microns in one nebula thus far) to constrain the formation mechanism and abundances, allowing us to test the hypothesis the WR nebulae are the principal contributors of H2 in galaxies s
Houck James R.
Morris Pat
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