Triggers:RCrB - Revision history

Lukasz at 11:21, 18 June 2012

2012-06-18T11:21:25Z

2009-10-26T17:59:55Z

2009-10-12T13:46:24Z

2009-10-12T13:44:51Z

2009-10-12T13:44:32Z

2009-10-12T12:55:07Z

2009-10-12T12:54:50Z

2009-08-24T13:34:07Z

DY Persei

2009-08-24T13:33:54Z

DY Persei

2009-08-24T13:32:05Z

← Older revision		Revision as of 11:21, 18 June 2012
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	== R Corona Borealis stars ==		== R Corona Borealis stars ==
		+	Clayton's review on RCB stars: [http://xxx.lanl.gov/abs/1206.3448]
		+
	[[File:figure_rcrb_mag.png\|300px\|right\|thumb\|Example of RCrB star in the LMC as seen by OGLE-II]]		[[File:figure_rcrb_mag.png\|300px\|right\|thumb\|Example of RCrB star in the LMC as seen by OGLE-II]]

@@ Line 2: / Line 2: @@
 [[File:figure_rcrb_mag.png|300px|right|thumb|Example of RCrB star in the LMC as seen by OGLE-II]]
-Only around 50 known in the Galaxy and Magellanic Clouds. They are rare type of evolved carbon-rich supergiants that are thought to result from the merger of two white dwarfs, called the Double Degenerate  (DD) scenario. This scenario is also studied in context of SN Ia explosions, therefore better understanding of RCrB stars is crucial. [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009]
+Only around 50 known in the Galaxy and Magellanic Clouds. They are rare type of evolved carbon-rich and hydrogen-deficient evolved F and G supergiants that are thought to result from the merger of two white dwarfs, called the Double Degenerate  (DD) scenario. This scenario is also studied in context of SN Ia explosions, therefore better understanding of RCrB stars is crucial. [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009].
 Characteristics:

← Older revision		Revision as of 13:46, 12 October 2009
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	* near-infrared excess: between 0 and 3 in J-H and H-K		* near-infrared excess: between 0 and 3 in J-H and H-K

−	[[File:RCRB-nearIR.png\|~~500px~~]]	+	[[File:RCRB-nearIR.png\|700px]]

← Older revision		Revision as of 13:44, 12 October 2009
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	* near-infrared excess: between 0 and 3 in J-H and H-K		* near-infrared excess: between 0 and 3 in J-H and H-K

−	[[File:RCRB-nearIR.png\|500px]	+	[[File:RCRB-nearIR.png\|500px]]

@@ Line 2: / Line 2: @@
 [[File:figure_rcrb_mag.png|300px|right|thumb|Example of RCrB star in the LMC as seen by OGLE-II]]
-Only around 50 known in the Galaxy and Magellanic Clouds. They are rare type of evolved carbon-rich supergiants that are thought to result from the merger of two white dwarfs, called the Double Degenerate  (DD) scenario. This scenario is also studied in context of SN Ia explosions, therefore better understanding of RCrB stars is crucial.
+Only around 50 known in the Galaxy and Magellanic Clouds. They are rare type of evolved carbon-rich supergiants that are thought to result from the merger of two white dwarfs, called the Double Degenerate  (DD) scenario. This scenario is also studied in context of SN Ia explosions, therefore better understanding of RCrB stars is crucial. [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009]
 Characteristics:
@@ Line 10: / Line 10: @@
 * the "dark" stage can last from days to years
 * recovers slowly to the baseline
-RCrB can be distinguished from other Red Giants based on the fact that an RCB’s circumstellar shell seem thinner than that of most common AGB stars [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009].
+[[File:RCRB-nearIR.png|500px]
@@ Line 19: / Line 22: @@
 These are another Carbon stars. Their drops in magnitude are much smaller than in RCrBs and seem to be periodical (P~1000d).

← Older revision		Revision as of 12:55, 12 October 2009
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	RCrB can be distinguished from other Red Giants based on the fact that an RCB’s circumstellar shell seem thinner than that of most common AGB stars [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009].		RCrB can be distinguished from other Red Giants based on the fact that an RCB’s circumstellar shell seem thinner than that of most common AGB stars [http://arxiv.org/abs/0905.3224 Tisserand et al. 2009].
−		+	TBC...

@@ Line 14: / Line 14: @@
 == DY Persei ==
-[[File:DYPer.png|400px|right|thumb|Example OGLE light curve of DY Per-type candidate]]
+[[File:DYPer.png|300px|right|thumb|Example OGLE light curve of DY Per-type candidate]]
 Some people claim it is a similar type to RCrB, however the drops in magnitude are much smaller and seem to be periodical (P~1000d).