Astronomy and Astrophysics – Astronomy
Scientific paper
May 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...190.0702h&link_type=abstract
American Astronomical Society, 190th AAS Meeting, #07.02; Bulletin of the American Astronomical Society, Vol. 29, p.786
Astronomy and Astrophysics
Astronomy
1
Scientific paper
This video shows the observed [O III] spatial structure of the jet and surrounding ovoid nebulosity in the R Aqr system as a function of 41 velocity planes spaced at 12 km s(-1) intervals (Fabry-Perot observations at the Palomar 60"). The ovoid nebulosity, due to an explosion ~ 660 years ago, is modeled as a circular ring expanding at 55 km s(-1) as seen at an inclination angle i =~ 70(deg) . The similarly inclined bipolar jet is modeled as a superposition of two opening helical structures -- a small-scale helix with an apex angle of 16(deg) which has undergone ~ 2-5 turns, and a large-scale helix with an apex angle of 60(deg) which has undergone ~ 1/3 of a turn. One possible explanation for the small-scale jet structure is the following process (Koupelis & Van Horn, 1988, ApJ, 324, 93): a parcel of ejected dust and gas is emitted along the rotation axis of the rotating star-accretion disk system which anchors a magnetic field that is frozen into the rotating parcel as well as the central source; since the parcel is free to expand, its rotation rate decreases, and the field is twisted into a helix; the consequent increase in the azimuthal component of the magnetic field builds up a strong magnetic pressure behind the parcel and accelerates it along the jet. The large-scale structure of the jet may simply be due to precession of the accretion disk. Jet radial velocities are in the range +/-175 km s(-1) , suggesting an outward accelerated flow maximum of ~ +/-512 km s(-1) . The video shows the model and data for comparison.
Dorband John E.
Hollis Jan. M.
Lyon Richard G.
Strong J. P.
van Buren Dale
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