Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aj....114.2700r&link_type=abstract
Astronomical Journal v.114, p.2700
Astronomy and Astrophysics
Astronomy
68
Stars: Pre-Main Sequence, Stars: Formation, Infrared: Stars
Scientific paper
Herbig-Haro energy sources are, as a class, among the youngest stars known. Based on the presence of multiple working surfaces in many HH flows, it has previously been argued that repetitive FU Orionis disk accretion events power the Herbig-Haro flows emanating from newborn stars. Since the dynamical time scales for HH flows are mostly rather longer than the expected time scales for high luminosity FU Orionis stars to decay to their low (presumably T Tauri) states, it follows that a fraction - but certainly not all - of HH energy sources might show FU Orionis characteristics. All but one of the known FU Orionis stars for which near-infrared spectroscopy is available show pronounced 2.3 μm CO absorption bands; the one exception shows very weak CO emission. Apart from FU Orionis stars, deep CO absorption is seen only in the photospheric spectra of late K or M type stars. We present 2.0-2.5 μm spectroscopy of 14 Herbig-Haro energy sources plus, for comparison, of 4 known FU Orionis stars. Of these 14 HH sources, 9 have been deliberately selected to have luminosities equal or higher than that (28 Lsun) of the lowest luminosity FU Orionis star known, L1551 IRS5. Among these 9 more luminous sources, 5 have CO absorption, 2 have CO emission, and 2 have continuous spectra. Among the five lower luminosity sources, 1 has CO absorption, 2 have CO emission and 2 show continuous spectra. Altogether, it appears that the majority of the high luminosity HH sources observed are likely to be presently in elevated FU Orionis states.
Aspin Colin
Reipurth Bo
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