Further evidence for the FU Orionis nature of PP 13S

Details Further evidence for the FU Orionis nature of PP 13S Further evidence for the FU Orionis nature of PP 13S

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.328..751a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 328, Issue 3, pp. 751-761.

Astronomy and Astrophysics

Astronomy

9

Stars: Formation, Stars: Individual: Pp 13S, Stars: Mass-Loss, Stars: Pre-Main-Sequence, Ism: Jets And Outflows

Scientific paper

We present optical and near-infrared images and spectroscopy together with submillimetre images of the candidate FU Orionis pre-main-sequence star PP 13S. A comparison of historical plates with our new images shows that PP 13S has dimmed and changed optical morphology significantly over the last half-century. In addition, its optical spectrum has undergone dramatic changes over a period of 18yr from one dominated by strong continuum emission to one showing only ionized, shock-excited emission lines. The current association with several features indicative of both accretion and outflow suggests that, within the last few hundred years, PP 13S passed through an elevated emission state characteristic of the high-accretion events of known FU Orionis-type stars, and has since declined, over the last few decades, to a more quiescent state. The result of the outburst may well have been the formation of the shock-excited Herbig-Haro jet seen to extend from the obscured young star. We additionally see significant morphological evolution of the source PP 13N. Its apparent association with a Herbig-Haro flow suggests that it also is actively accreting and driving a bipolar outflow.

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