Difference between revisions of "Triggers:FUOri"
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=== OO Serpentis === | === OO Serpentis === | ||
| − | OO Ser was discovered in | + | OO Ser was discovered in 1994 and is similar to FUors and EXors, but is so deeply embedded, that at its brightest was not visible in J band ([http://ukads.nottingham.ac.uk/abs/1996ApJ...468..861H Hodapp et al. 1996]). |
It was observed in infrared with ''Infrared Space Observatory'' and Spitzer ([http://arxiv.org/abs/0705.1231 Kospal et al. 2007]). | It was observed in infrared with ''Infrared Space Observatory'' and Spitzer ([http://arxiv.org/abs/0705.1231 Kospal et al. 2007]). | ||
| + | It has different time scales than FUors and EXors (more similar to V1647 Ori). | ||
Revision as of 13:08, 10 July 2009
FU Orionis (FUors)
FU Orionis (V1647 Ori) is young pre-main sequence stars, illuminating a McNeil's nebula in the vicinity of NGC 2068 star-forming region.
Plot from D.Chochol et al. 2006.
Characteristics:
- Very rare
- Outbursts repeat with a time scale of 40 years (1978, 2003)
- Amplitude: 5 mag over 4 months
- Outbursts last for 2 years
- Spectra: F or G supergiants
- Spectrum: red, heavily veiled continuum with strong emission of <math>H_{\alpha}</math>; in blue consistent with an early B spectral type
- X-ray variability present
- FU Ori and V1057 Cyg rise over 1 yr, whereas V1515 Cyg rise over 20 years
- FU Ori and V1515 Cyg decline over 20-100 years, V1015 Cyg decays faster (10 yrs)
Similar types to FU Ori
EX Lupis (EXors)
OO Serpentis
OO Ser was discovered in 1994 and is similar to FUors and EXors, but is so deeply embedded, that at its brightest was not visible in J band (Hodapp et al. 1996). It was observed in infrared with Infrared Space Observatory and Spitzer (Kospal et al. 2007). It has different time scales than FUors and EXors (more similar to V1647 Ori).
