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25 April 2024 |
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Evidence for an FU Orionis Outburst from a Classical T Tauri Star | | Adam A. Miller
; Lynne A. Hillenbrand
; Kevin R. Covey
; Dovi Poznanski
; Jeffrey M. Silverman
; Io K. W. Kleiser
; Barbara Rojas-Ayala
; Philip S. Muirhead
; S. Bradley Cenko
; Joshua S. Bloom
; Mansi M. Kasliwal
; Alexei V. Filippenko
; Nicholas M. Law
; Eran O. Ofek
; Richard G. Dekany
; Gustavo Rahmer
; David Hale
; Roger Smith
; Robert M. Quimby
; Peter Nugent
; Janet Jacobsen
; Jeff Zolkower
; Viswa Velur
; Richard Walters
; John Henning
; Khanh Bui
; Dan McKenna
; Shrinivas R. Kulkarni
; Christopher R. Klein
; | | Date: |
9 Nov 2010 | | Abstract: | We present pre- and post-outburst observations of the new FU Orionis-like
young stellar object Lk Halpha 188-G4 (also known as HBC 722 and PTF 10qpf).
Prior to this outburst, Lk Halpha 188-G4 would have been classified as a
classical T Tauri star on the basis of its optical emission-line spectrum
superposed on a K8-type photosphere, and photometric variability. The
mid-infrared spectral index of Lk Halpha 188-G4 indicates a Class II type
object. Lk Halpha 188-G4 exhibited a steady rise by ~1 mag over ~11 months
starting in Aug. 2009, before a subsequent more abrupt rise of >3 mag on a time
scale of ~2 months. Observations taken during and after eruption exhibit all of
the defining characteristics of FU Orionis variables: (i) Lk Halpha 188-G4
increased in brightness by >4 mag, (ii) a bright optical/near-infrared
reflection nebula has now appeared (iii) optical spectra in the outburst phase
are consistent with a G supergiant and dominated by absorption lines, the only
exception being Halpha which is characterized by a P Cygni profile, (iv)
near-infrared spectra in the outburst phase resemble late K--M
giants/supergiants with enhanced absorption seen in the molecular bands of CO
and H_2O, and (v) outflow signatures in H, He, and low excitation metallic
lines are seen in the form of blue-shifted absorption profiles. Lk Halpha
188-G4 is the first member of the FU Orionis class with a well-sampled optical
to mid-infrared spectral energy distribution in the pre-outburst phase. The
association of the PTF 10qpf outburst with this previously identified classical
T Tauri star provides strong evidence that FU Orionis eruptions represent
periods of enhanced disk accretion and outflow, likely triggered by
instabilities in the disk. | | Source: | arXiv, 1011.2063 | | Services: | Forum | Review | PDF | Favorites | |
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