Testing of Shocked Interstellar Cloud Models Using Deep Hα Images of the Cygnus Loop

Details Testing of Shocked Interstellar Cloud Models Using Deep Hα Images of the Cygnus Loop Testing of Shocked Interstellar Cloud Models Using Deep Hα Images of the Cygnus Loop

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.7003f&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #70.03; Bulletin of the American Astronomical Society, Vol. 24, p.1232

Astronomy and Astrophysics

Astronomy

Scientific paper

New Hα images of selected regions of the Cygnus Loop supernova remnant taken at MDM Observatory are used to test 2D and 3D numerical shocked cloud simulation features including multiple leading shock fronts, cloud deformation, formation of R-T and K-H instabilities on the cloud front and sides, gas stripping, and shock reflection and diffraction around the rear of an ISM cloud. A relatively isolated cloud in the SNR's southwestern sector imaged at both low- and high-resolution provides an excellent look at a real cloud-shock interaction at an earlier stage than shown in Fesen, Downes, & Kwitter (1992, A.J., 104, 719). These new data: 1) indicate that the onset of K-H instabilities along the cloud face and sides may occur surprisingly soon (t_cc =~ 1) after shock front contact, 2) show that multiple shocks fronts form inside the cloud leading to a highly complex filamentary internal cloud structure, and 3) successfully detect the extremely faint reflected and diffracted shocks downstream around the rear of the cloud. Wide-field images taken with the KPNO Burrell Schmidt also show an unexpectedly far western displacement of nonradiative shock emission along the remnant's western limb, and extensive diffuse emission coincident with the line of nonradiative emission filaments east of NGC 6992/5.

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