Resolving the Thermal Conduction Front in the Bubble S308

Details Resolving the Thermal Conduction Front in the Bubble S308 Resolving the Thermal Conduction Front in the Bubble S308

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004hst..prop10162c&link_type=abstract

HST Proposal ID #10162

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #10162 Ism

Scientific paper

Heat conduction is one of the most fundamental processes in the interstellar and intergalactic media. Many astronomical systems contain cool {<10^4 K} gas in contact with hot {10^6 -10^8 K} gas; at the contact surfaces, heat conduction occurs and may play an essential role in the thermal structure and evolution of the system. Observations of thermal conduction fronts have been extremely limited. Conventionally observations use absorption lines of collisionally ionized high ions as tracers of 1-3x10^5 K gas in the conduction front. Such observations allow the determination of column densities but not the relative locations of these tracer ions. Emission-line observations of a clear-cut, edge-on conduction front are needed to study the physical structure of a thermal conduction front. We have identified a clean-cut, edge-on conduction front in the circumstellar bubble S308, using XMM-Newton X-ray observations and ground-based optical images and spectra. We request HST STIS spectroscopic observations of the NV and CVI emission lines in the transition region from the hot interior gas to the cool nebular shell. These observations, combined with our complementary observations at optical, FUV, and X-ray wavelength, allow us to determine the spatially-resolved temperature profile of a thermal conduction front. Comparisons with models further allow us to assess the efficiency of thermal conduction.

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