Physics
Scientific paper
Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11674m&link_type=abstract
HST Proposal ID #11674. Cycle 17
Physics
Scientific paper
Circumstellar debris disks provide the principle window for investigating planet formation and evolution on timescales of 10-100 Myr. Unlike their younger counterparts, debris disks no longer contain primordial material. The dust observed in these objects is instead produced by collisional erosion of larger parent bodies in the developing planetary system. Currently, only five confirmed debris disks have detected circumstellar gas, studied primarily through UV absorption spectroscopy. The exact production mechanisms for this replenished gas are presently poorly constrained. However, the few objects studied so far have revealed a wide range of intruiging properties, including a stable Keplerian gas disk maintained by its high carbon abundance {Beta Pic}, and a rapidly expelled population of gas produced in collisions between unstable planetesimals {Sigma Her}. To add to this important set of observations, we propose to obtain NUV STIS spectroscopy of the debris disk host, HD 61005, a nearly edge-on debris disk notable for its swept asymmetric morphology. These observations allow the likely detection of circumstellar gas, making HD 61005 the first solar-type debris disk host with gas detected in this way. Thus, the proposed observations provide the unique opportunity to study gas in a debris disk analogous to our early solar system. In addition to potentially detecting circumstellar gas associated with this system, HD 61005 offers the possibility of tracing interstellar bow-shocked gas. HD 61005 is a unique debris disk in terms of its significant interaction with the interstellar medium. The proposed observations will, therefore, be the first to directly probe the interaction between a debris disk and its surrounding interstellar material. STIS is ideally suited for this experiment, providing sensitive NUV spectra with the required balance between spectral resolution and wavelength coverage.;
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