Triggers:LBVs - Revision history

Lukasz at 15:49, 29 July 2009

2009-07-29T15:49:43Z

Lukasz at 15:33, 29 July 2009

2009-07-29T15:33:19Z

Lukasz at 15:31, 29 July 2009

2009-07-29T15:31:22Z

Lukasz at 15:31, 29 July 2009

2009-07-29T15:31:05Z

Lukasz at 15:29, 29 July 2009

2009-07-29T15:29:31Z

Lukasz: 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-...'

2009-07-29T15:22:41Z

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-...'

New page

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-normal.jpg|200px]]

<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.

← Older revision		Revision as of 15:49, 29 July 2009
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	* Spectroscopic variations with period of 5.5 years (probably due to binarity)		* Spectroscopic variations with period of 5.5 years (probably due to binarity)
	* X-ray variability		* X-ray variability
		+	* engine of outbursts is not well understood yet

← Older revision		Revision as of 15:31, 29 July 2009
Line 1:		Line 1:
−	Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Very heavy stars(30Msun), often in binary systems, will evolve to W-R stars. Only a few is known.	+	Known also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Very heavy stars(>30Msun), often in binary systems, will evolve to W-R stars. Only a few is known.
	Known example: '''Eta Carinae'''.		Known example: '''Eta Carinae'''.

← Older revision		Revision as of 15:31, 29 July 2009
Line 1:		Line 1:
−	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 also as S Dor stars. Exhibit slow changes in brightness with occasional outbursts of substantial mass loss. Very heavy stars(30Msun), often in binary systems, will evolve to W-R stars. Only a few is known.
	Known example: '''Eta Carinae'''.		Known example: '''Eta Carinae'''.

@@ Line 7: / Line 7: @@
 * 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!!

@@ 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
@@ Line 10: / Line 10: @@
 * 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.