Reconstructing the Mass-loss History of Parsamian 21

Details Reconstructing the Mass-loss History of Parsamian 21 Reconstructing the Mass-loss History of Parsamian 21

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0809m&link_type=abstract

American Astronomical Society, AAS Meeting #212, #8.09; Bulletin of the American Astronomical Society, Vol. 40, p.529

Astronomy and Astrophysics

Astronomy

Scientific paper

Parsamian 21 is a cometary Nebula located about 400 parsecs away in Cloud A, a molecular cloud very close to the galactic plane. The star lies within a reflection nebula, part of which has been excavated by the star's bipolar jet. The circumstellar disk has an
inclination of about 86 deg which affords an unobstructed view of 3 associated Herbig-Haro (HH) knots. We combine narrow-band imagery from the Goddard Fabry-Perot Interferometer and long-slit optical spectra taken with the Dual Imaging Spectrograph (both at at Apache Point Observatory) with epoch 1992 long-slit spectra from the literature to produce a mass-loss history of the system using the HH knots. Application of the planar-shock model of HH knots yields mass-loss rates of 6.9*10-6 and 8.3*10-7 Msun/yr for the
northernmost and southernmost knots, respectively. Assuming that the mass loss rate is about 10% of the accretion rate we estimate
accretion rates of 6.9*10-5 and 8.3*10-6 Msun/yr. The space for the northernmost and southernmost knots are 120 and 530 km/s
respectively. This yields kinematic ages of 80 yr for the northernmost knot and 40 years for the southernmost knot. Parsamian 21 has been characterized as undergoing an FU Orionis outburst. If knot production is concurrent with the beginning of the outburst then these
kinematic ages indicate that the duration of the outburst is typical of of FU-Orionis outbursts. However these mass-loss rates are around an order magnitude lower than those typical of FU-Orionis outbursts.

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