Difference between revisions of "Triggers:Flares"

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* 1.3 flares per hour sq.deg with <math>\Delta u > 0.7</math> mag, with slightly more flares towards the galactic plane.
 
* 1.3 flares per hour sq.deg with <math>\Delta u > 0.7</math> mag, with slightly more flares towards the galactic plane.
  
[[File:Mflares-rates.png|left]]
+
[[File:Mflares-rates.png|400px|left]]
  
 
[[File:FlaresStripe82.png|400px|Ampitude distribution for Stripe82 flares.]]
 
[[File:FlaresStripe82.png|400px|Ampitude distribution for Stripe82 flares.]]

Revision as of 14:03, 9 October 2009

Statistical study of M dwarf flares in Stripe 82 is presented in Kowalski et al. 2009.

Flare example Stripe82.png
  • Colour range for M-dwarfs (r − i) > 0.53 and (i − z) > 0.3 and (u-r) > 3
  • The most flaring are late type M-dwarfs (M4-M6), earlier types (M2-M3) flare half as often as late types and M0-M1 dwarfs flare only 20% as often as late types.
  • flares are the most pronounced in u-band
  • around 35% of M-dwarfs are in binary systems - these have bluer u-g. Most single M-dwarfs will have u-g > 1.8
  • g - K > 4
  • amplitude in u > 0.7 mag up to 5 mag.
  • large and small flares possible
  • flaring fraction: 0.0108%, i.e. 1 of every 10,000 observation of a M-dwarf in Stripe 82 resulted in a flare
  • 1.3 flares per hour sq.deg with <math>\Delta u > 0.7</math> mag, with slightly more flares towards the galactic plane.
Mflares-rates.png

Ampitude distribution for Stripe82 flares.


Mdwarf flare Gl234AB.png Example of flares in Gl234AB (V577 Mon) from Doyle et al. 1989

FlareCNLeo-PioftheSky.png Example flare detected by Pi of the Sky project. From Sokolowski 2008.

FlareGJ3331A-PioftheSky.png High temporal resolution observations of a flare star by Pi of the Sky. From Sokolowski 2008.