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text=Original entry date: 26/08/2010 (Daniel Huber)%0a%0aNew entry date: 14/09/2012 (Herbert Pablo, redefined the project)%0a%0aStatus: Ongoing. Daniel Huber transferred the lead of this project to Herbert Pablo. When Herbert moved jobs, it was transferred back. Now being carried out by a honours student.%0a%0aLead group: Ames%0a%0aCollaborating groups: Göttingen, Birmingham, Leuven, Meudon, NASA, Sydney%0a%0aContact person: Daniel Huber%0a%0aCoordinating subchair: Saskia Hekker%0a%0aKepler data: Q0-Q11. For some objects, depending on how promising they are it would be nice to have longer coverage, but it's difficult say at this juncture.%0a%0aContent: %0a%0a*Within the Kepler red giants data there exists a small subset in which one or multiple Fourier transform peaks are of anomalously large amplitude (several times larger than surrounding peaks). These peaks may be unrelated to the pulsation spectrum and instead be the signature of a close companion. When the data is phased over the suspected binary period, some of these stars appear to show ellipsoidal variations and, at least in one case, eclipses. This is both troubling and interesting as reasonable values for the mass of the companion tend to put it within the envelope of the red giant. Many red giants which show these peaks are at high galactic latitudes where contamination is small suggesting that this phenomenon is indeed real. Since these systems could indeed be in the common envelope stage, the Rosetta stone of close binary evolution, it is imperative that we catalog these systems and determine their true identity.%0a*Catalog all known high amplitude red giants for comparison with the overall Kepler Red Giant data set.%0a*Treating these high amplitude peaks as evidence for binarity results in ellipsoidal variables in many cases, and an eclipse in at least one case. We will apply this analysis to all red giants with high amplitude peaks, checking carefully for contamination, and explore the binary properties of these systems.%0a*For confirmed binaries, investigate their viability as common envelope systems. For confirmed common envelope systems investigate changes in binary period.%0a%0aPrerequisites: %0a*None%0a%0aRemarks:%0a*None%0a%0aMilestones:%0a*First draft second half of 2015.%0a
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diff:1426236610:1418680333:=5c5%0a%3c Status: Ongoing. Daniel Huber transferred the lead of this project to Herbert Pablo. When Herbert moved jobs, it was transferred back. Now being carried out by a honours student.%0a---%0a> Status: Ongoing. Daniel Huber transferred the lead of this project to Herbert Pablo. When Herbert moved jobs, it was transferred back.%0a
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diff:1418680333:1399304007:=9,10c9,10%0a%3c Collaborating groups: Göttingen, Birmingham, Leuven, Meudon, NASA, Sydney%0a%3c %0a---%0a> Collaborating groups: Amsterdam, Birmingham, Leuven, Meudon, NASA, Sydney%0a> %0a31c31%0a%3c *First draft second half of 2015.%0a---%0a> *First draft by summer 2013.%0a
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diff:1399304007:1399304007:=1,31d0%0a%3c Original entry date: 26/08/2010 (Daniel Huber)%0a%3c %0a%3c New entry date: 14/09/2012 (Herbert Pablo, redefined the project)%0a%3c %0a%3c Status: Ongoing. Daniel Huber transferred the lead of this project to Herbert Pablo. When Herbert moved jobs, it was transferred back.%0a%3c %0a%3c Lead group: Ames%0a%3c %0a%3c Collaborating groups: Amsterdam, Birmingham, Leuven, Meudon, NASA, Sydney%0a%3c %0a%3c Contact person: Daniel Huber%0a%3c %0a%3c Coordinating subchair: Saskia Hekker%0a%3c %0a%3c Kepler data: Q0-Q11. For some objects, depending on how promising they are it would be nice to have longer coverage, but it's difficult say at this juncture.%0a%3c %0a%3c Content: %0a%3c %0a%3c *Within the Kepler red giants data there exists a small subset in which one or multiple Fourier transform peaks are of anomalously large amplitude (several times larger than surrounding peaks). These peaks may be unrelated to the pulsation spectrum and instead be the signature of a close companion. When the data is phased over the suspected binary period, some of these stars appear to show ellipsoidal variations and, at least in one case, eclipses. This is both troubling and interesting as reasonable values for the mass of the companion tend to put it within the envelope of the red giant. Many red giants which show these peaks are at high galactic latitudes where contamination is small suggesting that this phenomenon is indeed real. Since these systems could indeed be in the common envelope stage, the Rosetta stone of close binary evolution, it is imperative that we catalog these systems and determine their true identity.%0a%3c *Catalog all known high amplitude red giants for comparison with the overall Kepler Red Giant data set.%0a%3c *Treating these high amplitude peaks as evidence for binarity results in ellipsoidal variables in many cases, and an eclipse in at least one case. We will apply this analysis to all red giants with high amplitude peaks, checking carefully for contamination, and explore the binary properties of these systems.%0a%3c *For confirmed binaries, investigate their viability as common envelope systems. For confirmed common envelope systems investigate changes in binary period.%0a%3c %0a%3c Prerequisites: %0a%3c *None%0a%3c %0a%3c Remarks:%0a%3c *None%0a%3c %0a%3c Milestones:%0a%3c *First draft by summer 2013.%0a
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