Timeline for How are heavier elements such as carbon and silicon distributed within the Sun?
Current License: CC BY-SA 3.0
7 events
| when toggle format | what | by | license | comment | |
|---|---|---|---|---|---|
| Aug 3, 2016 at 6:57 | comment | added | ProfRob | @dualredlaugh The CNO is energetically unimportant (1%), but is responsible for turning almost all the C into N in the core. The N to O (and back to C) bit is much slower. | |
| Aug 3, 2016 at 3:07 | comment | added | HDE 226868♦ | @dualredlaugh The CNO cycle is relatively uncommon in the Sun; it starts becoming dominant at about 1.7$\times$10$^7$ K, a bit higher than the Sun's core temperature. So yes, the p-p chain is far more prevalent than the CNO cycle in Sun-like stars. | |
| Aug 3, 2016 at 3:05 | comment | added | dualredlaugh | I noticed that there is relatively little overlap between the carbon and nitrogen fraction curves. Might this imply that the CNO cycle is a less common mode of fusion in the Sun? | |
| Aug 3, 2016 at 2:51 | vote | accept | uhoh | ||
| Aug 3, 2016 at 2:45 | comment | added | uhoh | Wow, thanks for taking the time to put this together. Those plots are exactly what I hoped to see - there's so much happening there! Indeed this suggests further questions. Thank you! The footnotes are appreciated as well, I'm pretty sure John Bahcall's papers can be trusted in this context :-). | |
| Aug 3, 2016 at 0:38 | history | edited | HDE 226868♦ | CC BY-SA 3.0 |
Gave possible guess for helium-3 spike.
|
| Aug 3, 2016 at 0:23 | history | answered | HDE 226868♦ | CC BY-SA 3.0 |