A&A 468, L41-L44 (2007)
Minkowski's footprint revisited
Planetary nebula formation from a single sudden event?J. Alcolea1, R. Neri2, and V. Bujarrabal3
1 Observatorio Astronómico Nacional (OAN-IGN), Calle Alfonso XII 3, 28014 Madrid, Spain
2 Institut de Radio Astronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 St. Martin d'Hères, France
3 Observatorio Astronómico Nacional (OAN-IGN), Apartado 112, 28803 Alcalá de Henares, Spain
(Received 18 December 2006 / Accepted 12 January 2007)
Context.M 1-92 can be considered an archetype of bipolar pre-planetary nebulae. It shows a clear axial symmetry, along with the kinematics and momentum excess characteristic of this class of envelopes around post-AGB stars.
Aims.By taking advantage of the new extended configuration of the IRAM Plateau de Bure interferometer, we wanted to study the morphology and velocity field of the molecular gas better in this nebula, particularly in its central part.
Methods.We performed sub-arcsecond resolution interferometric observations of the J = 2-1 rotational line of 13CO in M 1-92.
Results.We found that the equatorial component is a thin flat disk, which expands radially with a velocity proportional to the distance to the center. The kinetic age of this equatorial flow is very similar to that of the two lobes. The small widths and velocity dispersion in the gas forming the lobe walls confirm that the acceleration responsible for the nebular shape could not last more than 100-120 yr.
Conclusions.The present kinematics of the molecular gas can be explained as the result of a single brief acceleration event, after which the nebula reached an expansion velocity field with axial symmetry. In view of the similarity to other objects, we speculate on the possibility that the whole nebula was formed as a result of a magneto-rotational explosion in a common-envelope system.
Key words: stars: circumstellar matter: jets -- stars: AGB and post-AGB -- stars: individual: PN M 1-92 -- stars: mass-loss
© ESO 2007