Triggers:FUOri - Revision history

Aleks.scholz at 15:09, 24 July 2013

2013-07-24T15:09:23Z

2013-07-24T14:30:35Z

2013-07-19T14:18:14Z

2013-07-19T14:14:19Z

2009-12-14T15:59:31Z

2009-11-05T13:00:55Z

FU Orionis (FUors)

2009-11-05T12:15:35Z

EX Lupis (EXors)

2009-10-28T16:39:12Z

2009-10-28T15:59:59Z

EX Lupis (EXors)

2009-10-28T15:59:17Z

EX Lupis (EXors)

@@ Line 33: / Line 33: @@
 such accretion bursts on the properties of the dust and gas in the disks. Also, high cadence monitoring
 immediately after the event is useful for modeling the source.
 References:

@@ Line 21: / Line 21: @@
 * many details unknown, unbiased sample required
 * rise time varies from months to years
-* amplitude range from <1 mag to 5 mag
+* amplitude range from <1 mag to 5 mag (but 1mag cutoff is probably useful)
 * outburst last from months to decades, some are recurrent
 * extreme events like FU Ori are very rare
-* Spectra: F or G supergiants
+* Spectra: F or G supergiants, red, heavily veiled continuum with strong emission of <math>H_{\alpha}</math>
 * At maximum spectral types are in the range Ae(alpha) - Gpe(alpha)
 * 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)
 References:
 * Hartmann & Kenyon 1996 review: http://adsabs.harvard.edu/abs/1996ARA%26A..34..207H
-* Scholz et al. systematic survey: http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1301.3152
+* Scholz et al. 2013 systematic survey: http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1301.3152

@@ Line 3: / Line 3: @@
 Prototypes:
-FU Oris are an extreme subsample of eruptive classical T Tauri stars. Only one outburst observed, but lasts for decades. Only about a dozen FU Ori bursts observed. FU Ori itself (V1647 Ori) is illuminating a McNeil's nebula in the vicinity of NGC 2068 star-forming region.
+FU Oris are an extreme subsample of eruptive classical T Tauri stars. Only one outburst observed, but lasts for decades. Only about a dozen FU Ori bursts observed. V1647 Ori is illuminating a McNeil's nebula in the vicinity of NGC 2068 star-forming region.
 [[File:FUOri.png]]
 Plot from [http://www.ta3.sk/caosp/Eedition/FullTexts/vol36no3/pp149-157.pdf D.Chochol et al. 2006].
-EX Lupis (EXors) have smaller, shorter, recurrent outbursts
+EX Lupis (EXors) have smaller, shorter, recurrent outbursts.
 [[File:ExLupi.png|right|400px|thumb|EX Lupi photometry from the ASAS project.]]
@@ Line 18: / Line 18: @@
 Characteristics:
-* diverse zoo of lightcurves
+* diverse zoo of lightcurves, use of templates is risky
 * many details unknown, unbiased sample required
 * rise time varies from months to years
 * amplitude range from <1 mag to 5 mag
-* outburst last from months to decades
+* outburst last from months to decades, some are recurrent
 * extreme events like FU Ori are very rare
 * Spectra: F or G supergiants

@@ Line 1: / Line 1: @@
-== FU Orionis (FUors) ==
+== Eruptive YSOs ==
-FU Orionis (V1647 Ori) is young pre-main sequence stars, illuminating a McNeil's nebula in the vicinity of NGC 2068 star-forming region.
 [[File:FUOri.png]]
 Plot from [http://www.ta3.sk/caosp/Eedition/FullTexts/vol36no3/pp149-157.pdf D.Chochol et al. 2006].
 Characteristics:
-* Very rare
+* diverse zoo of lightcurves
-* Outbursts repeat with a time scale of 40 years (1978, 2003)
+* many details unknown, unbiased sample required
-* Amplitude: 5 mag over 4 months
+* rise time varies from months to years
-* Outbursts last for 2 years
+* amplitude range from <1 mag to 5 mag
 * 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
@@ Line 20: / Line 33: @@
 References:
-* The photometric evolution of FU Orionis objects: disc instability and wind-envelope interaction (http://ukads.nottingham.ac.uk/abs/2005MNRAS.361..942C)
+* Hartmann & Kenyon 1996 review: http://adsabs.harvard.edu/abs/1996ARA%26A..34..207H
+* Scholz et al. systematic survey: http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1301.3152

@@ Line 13: / Line 13: @@
 * 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

@@ Line 26: / Line 26: @@
 * Recurent eruptions
 * Amplitudes similar or smaller than in FUors
-* Balmer emission lines, He I and other lines as in active T Tauri stars
+* Balmer emission lines, He I and other lines as in active T Tauri stars (see also [[Triggers:TTau]])
 === OO Serpentis ===

@@ Line 20: / Line 20: @@
 === EX Lupis (EXors) ===
-[[File:ExLupi.png|right|400px|thumb|EX Lupi photometry from Herbig(2007).]]
+[[File:ExLupi.png|right|400px|thumb|EX Lupi photometry from the ASAS project.]]
 See Herbig (2007) [http://www.iop.org/EJ/article/1538-3881/133/6/2679/205809.text.html]