The Structure and Dynamics of the Protoplanetary Nebula M1-92

Details The Structure and Dynamics of the Protoplanetary Nebula M1-92 The Structure and Dynamics of the Protoplanetary Nebula M1-92

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...504..915b&link_type=abstract

Astrophysical Journal v.504, p.915

Astronomy and Astrophysics

Astronomy

54

Stars: Circumstellar Matter, Stars: Agb And Post-Agb, Ism: Planetary Nebulae: Individual Alphanumeric: M1-, 2, Ism: Jets And Outflows

Scientific paper

We present high-resolution (1."0) maps of 13CO J = 2-1 in the proto-planetary nebula M1-92, Minkowski's Footprint, obtained with the Institut de Radioastronomie Millimetrique (IRAM) interferometer at Plateau de Bure. We confirm the main components found in our previous works: a central disklike condensation, a bipolar double-shell structure with axial outward velocity increasing with the distance to the star, and two opposed features at the tips of the nebula where the maximal deprojected velocity is attained, ~70 km s-1. The major quality of the present data allows us to estimate the very small width of the double-shell walls, ~0."6 (2 x 1016 cm), and the diameter of the central disk, 2"-3" (1017 cm). The whole structure is probably the remnant of the previous asymptotic giant branch (AGB) shell after being shocked by the bipolar post-AGB jets. The mass of the molecular envelope is about 0.9 M&sun;, and its kinetic momentum and energy (released by the wind interaction) are ~3 x 1039 g cm s-1 and ~7 x 1045 ergs, respectively. Since the interaction time must be significantly smaller than the age of the nebula, 900 yr, these figures imply very energetic post-AGB jets that cannot be driven by radiation pressure. We also notice that the inner disklike structure is too large for collimating the very narrow post-AGB jets. We propose that reaccretion of material, ejected during the previous AGB phase, is the most likely mechanism to explain the strongly bipolar and very energetic post-AGB ejections.

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