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text=Detecting the core He flash through a rapid brightness variation%0a%0aEntry date: 21/01/2013%0a%0aStatus: Ongoing%0a%0aLead group: Pittsburgh (Carnegie)%0a%0aCollaborating groups: Columbus (Ohio St)%0a%0aContact person: Josh Simon%0a%0aCoordinating subchair: Dennis Stello%0a%0aKepler data: public time series of public red giants%0a%0aContent: %0a*Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash.%0a*If this fading occurs on a Kelvin-Helmholtz timescale as expected, a star in this phase of evolution will decrease in brightness by more than 10^-5 mag per year.%0a*We aim to detect such stars by searching for a steady long-term decline in brightness among the Kepler red giant sample.%0a%0aPrerequisites: %0a*Population classifications from project [59]%0a*Still waiting for Rafa's final detrended data.%0a%0aRemarks:%0a*The difference between [55] and this project, is that the former will use DeltaP as a diagnostic, and this one will use the Kepler magnitude.%0a%0aJournal:%0a*ApJ
time=1402385671
author:1402385671=stello
diff:1402385671:1399321021:=24d23%0a%3c *Still waiting for Rafa's final detrended data.%0a
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diff:1399321021:1399320982:=18,20c18,21%0a%3c *Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash.%0a%3c *If this fading occurs on a Kelvin-Helmholtz timescale as expected, a star in this phase of evolution will decrease in brightness by more than 10^-5 mag per year.%0a%3c *We aim to detect such stars by searching for a steady long-term decline in brightness among the Kepler red giant sample.%0a---%0a> *Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash. If this fading occurs on a Kelvin-Helmholtz timescale as expected, a star in this phase of evolution will decrease in%0a> brightness by more than 10^-5 mag per year. We aim to detect such stars%0a> by searching for a steady long-term decline in brightness among the Kepler%0a> red giant sample.%0a
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diff:1399320982:1399320954:=18,19c18,20%0a%3c *Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash. If this fading occurs on a Kelvin-Helmholtz timescale as expected, a star in this phase of evolution will decrease in%0a%3c brightness by more than 10^-5 mag per year. We aim to detect such stars%0a---%0a> *Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash.  If this fading occurs on a Kelvin-Helmholtz%0a> timescale as expected, a star in this phase of evolution will decrease in%0a> brightness by more than 10^-5 mag per year.  We aim to detect such stars%0a
host:1399320982=188.177.191.251
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diff:1399320954:1399320954:=1,31d0%0a%3c Detecting the core He flash through a rapid brightness variation%0a%3c %0a%3c Entry date: 21/01/2013%0a%3c %0a%3c Status: Ongoing%0a%3c %0a%3c Lead group: Pittsburgh (Carnegie)%0a%3c %0a%3c Collaborating groups: Columbus (Ohio St)%0a%3c %0a%3c Contact person: Josh Simon%0a%3c %0a%3c Coordinating subchair: Dennis Stello%0a%3c %0a%3c Kepler data: public time series of public red giants%0a%3c %0a%3c Content: %0a%3c *Bildsten et al. (2012) and previous studies indicate that red giants fade extremely rapidly from the tip of the red giant branch after they undergo a core helium flash.  If this fading occurs on a Kelvin-Helmholtz%0a%3c timescale as expected, a star in this phase of evolution will decrease in%0a%3c brightness by more than 10^-5 mag per year.  We aim to detect such stars%0a%3c by searching for a steady long-term decline in brightness among the Kepler%0a%3c red giant sample.%0a%3c %0a%3c Prerequisites: %0a%3c *Population classifications from project [59]%0a%3c %0a%3c Remarks:%0a%3c *The difference between [55] and this project, is that the former will use DeltaP as a diagnostic, and this one will use the Kepler magnitude.%0a%3c %0a%3c Journal:%0a%3c *ApJ%0a\ No newline at end of file%0a
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