Nucleosynthesis: other than big bang and supernova According to many texts, hydrogen, helium and traces of lithium-7 were created in a brief period after the big bang; helium is created through fusion (pp, CNO) in main sequence stars; elements like carbon, nitrogen and oxygen and neon are created in main sequence stars heavier than the Sun.
I've also learnt that sun-like stars enrich the interstellar medium with hydrogen and helium through mass loss after leaving the main sequence; that stars with a greater mass but too light to end as a supernova (roughly up to 8 $M_\odot$) also enrich the interstellar medium with C, N, O, Ne after dredge-up phases. A lot of the stellar ashes are buried in white dwarfs, so much of the heavier elements remain in the star for the most part, if I'm correct.
I've learnt that essentially all elements heavier than these are created in supernova events.
But according to the Astronomy Picture of the Day for 2015-01-25 a significant fraction of many elements (also) have another origin.

*

*Are Li, Be, B on Earth produced in significant amounts through spallation by cosmic rays of C, N, O high in the atmosphere of the earth? (Not in stars: no stable nuclei with A=5 or A=8 and lithium undergoes fusion.)


*Are the "green" elements in the diagram (e.g. F, K, Zn, La) produced in the red (super)giant phase of moderately heavy stars and liberated through dregde-up and mass loss (stellar wind)? Or by novae of white dwarfs?


*How is gold produced by collisions of neutron stars (text below the diagram)?


*Elements up to Pu are produced through r-process neutron capture in supernovae, but why not Am, CM etc.? Or are they produced but too unstable ($\alpha$, $\beta$ decay) to survive long enough?
 A: The answer to the first question is no, not in significant quantities. Li, Be and B are produced in spallation reactions in the cosmos, but here on Earth they were part of the gas cloud that formed the Sun (almost entirely).
The second answer is yes, during the Asymptotic Giant Branch (AGB) phase, along with many other heavy elements and Carbon. The mechanism by which intermediate stars create heavy elements beyond iron is (slow) neutron capture onto pre-existing iron-peak nuclei via the "s-process". These elements, along with others (e.g. C, F) produced in nucleosynthesis are brought to the surface by convection and expelled in slow winds, driven by radiation pressure. About half the elements beyond iron are produced mainly by this s-process and not in supernovae.
The third answer is "possibly" and by the r-process; rapid neutron capture by heavy elements in dense, neutron-rich environments. Gold, platinum, osmium and iridium - the elements around the "third r-process peak" - may especially be produced in this way. Some evidence for this has now emerged by analysing infrared spectra from a merging neutron star event identified through a gravitational wave detection.
The fourth answer is that all kinds of unstable isotopes are produced in supernovae and then decay.
More details and references can be found in my answer to What is the origin of elements heavier than iron?
