C12(a,g) rate study

The results on this page are from a senior thesis project by Matthew Michael Boyes
in collaboration with Alexander Heger & Stan E. Woosley.

Senior Thesis Thesis_Boyes.pdf 4.9 MB

Printable Version Thesis_Boyes_print.ps 56 MB

Posters

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Information

The movies are composed from a series of Kippenhahn Diagrams, i.e., stellar structure as a function of time, which vary one parameter of the star. All sequences use the same color coding:

/// convection
XXX semiconvection

net nuclear energy generation (burning plus neutrino losses) in erg g-1 s-1
0 >10-1 >10 0 >10 1 >10 2 >10 3 >10 4 >10 5 >10 6 >10 7 >10 8 >10 9 >1010 >1011 >1012 >1013 >1014

net nuclear energy loss (burning plus neutrino losses) in erg g-1 s-1
0 <-10-1 <-10 0 <-10 1 <-10 2 <-10 3 <-10 4 <-10 5 <-10 6 <-10 7 <-10 8 <-10 9 <-1010 <-1011 <-1012 <-1013 <-1014

A sample image explaning the different burning stages.

How to play the movies.

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Movies

The movies magnify the evolution of the helium core starting at end of central helium burning till core collapse.

Movies by Alexander Heger
mass
(solar masses)
fine grid reduced grid
(animated gif) (mpeg-1) (mpeg-1)
15 2.2 MByte 2.6 MByte 737 kByte
20 2.2 MByte 2.6 MByte 750 kByte
25 2.2 MByte 2.7 MByte 744 kByte

 

The movie shows the evolution of the helium core till from end of central helium burning till core collapse. Convection is shown as green hatching, semiconvection as red cross hatching. Specific energy generation (blue) and energy losses (pink; mostly by plasma neutrinos), are shown as color shading and each "level" of higher color intensity represents an order of magnitude higher value, in erg per gram and second, starting at 1/10 erg per gram and second.

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Plots

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Acknowledgements: This work has been supported by the NSF (AST-9731569, INT-9726315), NASA (NAG5-8128), the DOE (B347885, W-7405-ENG-48), and the Alexander von Humboldt Foundation (FLF-1065004).
Matt Boyes
Monday, 01-Oct-2001 13:34:59 PDT