Difference between revisions of "Triggers:LBVs"

From Gaia Science Alerts Working Group
Jump to navigationJump to search
(Created page with 'Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Known example: Eta Carinae. [[File:ESO-Eta_Carinae-phot-17a-08-...')
 
Line 1: Line 1:
Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss.
+
Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Very heavy stars, often in binary systems, will evolve to W-R stars. Only a few is known.
Known example: Eta Carinae.
+
Known example: '''Eta Carinae'''.
  
[[File:ESO-Eta_Carinae-phot-17a-08-normal.jpg|200px]]
+
[[File:ESO-Eta_Carinae-phot-17a-08-normal.jpg|200px|right|thumb|Eta Carinae, ESO]]
  
 
<math>M_V \sim -11 \ldots -8</math> mag
 
<math>M_V \sim -11 \ldots -8</math> mag
Line 10: Line 10:
 
* Giant eruptions ("Eta Carinae type") of around 8 mag, once a few centuries!!
 
* Giant eruptions ("Eta Carinae type") of around 8 mag, once a few centuries!!
 
* After giant eruption and fade, the star recovers its brightness as the dust disperses.
 
* After giant eruption and fade, the star recovers its brightness as the dust disperses.
 +
* Spectroscopic variations with period of 5.5 years (probably due to binarity)
 +
* X-ray variability

Revision as of 15:29, 29 July 2009

Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Very heavy stars, often in binary systems, will evolve to W-R stars. Only a few is known. Known example: Eta Carinae.

Eta Carinae, ESO

<math>M_V \sim -11 \ldots -8</math> mag

  • Baseline micro-variability: P around 10-20 days, amplitude 0.1-0.2 mag
  • "normal eruptions": 1-2 mag (rise within few months), repeating with period of years or decades the brighter abs.mag the shorter period between eruptions)
  • Giant eruptions ("Eta Carinae type") of around 8 mag, once a few centuries!!
  • After giant eruption and fade, the star recovers its brightness as the dust disperses.
  • Spectroscopic variations with period of 5.5 years (probably due to binarity)
  • X-ray variability