OH emission and the nature of Minkowski's footprint (M1-92)

Details OH emission and the nature of Minkowski's footprint (M1-92) OH emission and the nature of Minkowski's footprint (M1-92)

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...367..200s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 367, Jan. 20, 1991, p. 200-207.

Astronomy and Astrophysics

Astrophysics

16

Faint Objects, Hydroxyl Emission, Planetary Nebulae, Stellar Mass Ejection, Very Large Array (Vla), Interstellar Gas, Line Of Sight, Stellar Luminosity, Stellar Temperature

Scientific paper

VLA observations of the 1667 and 1612 MHz OH brightness distribution in the bipolar nebula M1-92 are presented. The OH emission originates in the circumstellar gas disk whose axis coincides with that of the bipolar lobes. No OH emission is found in the lobes themselves. A simple axisymmetric model which describes the main features of this emission consists of a fan-shaped disk undergoing pure radial expansion at a velocity of 18 km/s. In this model, the radius of the disk is 2.4 arcsec (1.6 x 10 to the 17th cm) and the opening angle of the fan is 70 deg (FWHM). The bipolar axis is inclined at 35 deg to the line of sight. The mass-loss rate in the disk is estimated to be 5.6 x 10 to the -6th solar mass/yr for an assumed distance of 4.5 kpc, and the kinematic age of the disk is about 3000 yr. The properties of M1-92 are reviewed, including the mass-loss rate, the kinematic age, the IR characteristics, and the radio continuum emission, and all are found to be consistent with the view that M1-92 is a young planetary nebula.

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