Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...447..257t&link_type=abstract
Astrophysical Journal v.447, p.257
Astronomy and Astrophysics
Astronomy
30
Ism: Structure, Ism: Planetary Nebulae: Individual Alphanumeric: Sh 2-216
Scientific paper
We have obtained mosaics of images of the giant planetary nebula, Sh 2-216, in Hα and [N II], covering the entire 1°.6 diameter. These show the interaction with the interstellar medium (ISM) in unprecedented detail. While the restriction of the [O III] zone to the region close to the central star is as expected for the O + + Strömgren sphere in a uniform-density nebula, the lower ionization lines are clearly strongly influenced by the interaction with the ISM. There is much filamentary structure: for example, there are long, thin features in the obvious interaction region to the east (seen in Hα) and much wider structures across the face of the nebula (which are substantially brighter in [N II]). We interpret this as showing that the nebula has a thick outer region which is bright in [N II] and has deep outer corrugations. Over this lies a thin sheet of material that is brighter in Hα and is also the main location of low-ionization emission such as [O I]. Thus, the different characteristics of the filaments are due to projection effects of the same basic structure. Two considerations seem to indicate that the general ISM magnetic field is a significant factor in molding the shape of the nebula: first, the corrugations across the face of the nebula are fairly parallel; second, the planetary nebula ram pressure matches the expected ambient ISM magnetic pressure. We discuss the possibilities for using ancient planetary nebulae as probes of the ISM.
Martos Marco A.
Noriega-Crespo Alberto
Tweedy Richard W.
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