We shouldn't overlook (pardon the pun) the role of magnetohydrodynamics (MHD) in PN and SN remnant formation. Filaments and threads are magnetic sheets that we can see, and MHD turbulence plays a major role in stellar evolution, from coalescing molecular clouds to final dispersion into the intergalactic medium. Without magnetic forces our sun would be a hot but very boring object. There are so many papers on how MHD affects both PN shapes and SN remnant dispersion that one can get a bit addlepated trying to keep up with it all. Google Scholar lists the following references for MHD in PNs:
http://scholar.google.co.za/scholar?...1%2C5&as_sdtp=
amid which this paper is a good starter kit:
http://www.annualreviews.org/doi/abs...rnalCode=astro
For MHD in SNrs:
http://scholar.google.co.za/scholar?...1%2C5&as_sdtp=
arXiv weighs in as well, though less voluminously:
http://arxiv.org/find/all/1/all:+AND.../0/1/0/all/0/1
http://arxiv.org/find/all/1/all:+AND.../0/1/0/all/0/1
Most of this stuff is a lot chewier than the books Robert recommends. The turgid prose of professional papers is redeemed by their up-to-the-minute data, but they sure are a handful to read.