# Are we really star-stuff from the interior of collapsing stars?

Carl Sagan has said several times that we are "star-stuff".

One instance can be found in Good Reads' Carl Sagan > Quotes > Quotable Quote:

The nitrogen in our DNA, the calcium in our teeth, the iron in our blood, the carbon in our apple pies were made in the interiors of collapsing stars. We are made of starstuff.

Question: Was most of my nitrogen really made in the interior of a star during its collapse? Was my calcium and iron made there as well, and not (for example) in an expanding shell after a supernova?

• Well you are looking for a somehow very fine distinction. I would call it stars stuff anyway. Normally the synthesis up to iron is explained has due to fusion in inner core of stable or going to collapse stars. Heavier elements are thought to form upon supernova explosion due to the very high energy of the ejecta (plus other mechanism such as capture which should less related to supernova). It seems reasonable that light elements could form as you said, as for the supernova inputs energy to the remaining external shells which still contain H He etc. Just to discuss because I am not sure... Jan 12, 2019 at 10:52
• @Alchimista you expect me to take the word of an alchimista on nucleosynthesis? ;-)
– uhoh
Jan 12, 2019 at 10:55
• Many elements are made by the s-process and distributed by AGB stars that aren't collapsing, and which will never go supernova. See astronomy.stackexchange.com/questions/8894/… for details. And let's not forget the triple alpha process and the CNO cycle. Jan 12, 2019 at 11:26
• @uhoh :)) yes forget everything goes to gold Jan 12, 2019 at 11:55
• Yes, most everyday stuff is from normal fusion in smaller stars ejected as planetary nebula or heavier stuff made in supernovas. The two exceptions are heavy elements like gold, that emerge from neutron star mergers (still starstuff) and beryllium and boron, that are mostly spallation. And some primordial hydrogen, helium and lithium, of course. Jan 12, 2019 at 11:56

Some of it will be from the interior of collapsing stars, some will be from supernovas, some from normal everyday fusion, and some from other processes.

The answers from @HDE226868 and @RobJeffries on this question on where heavier elements come from gives good background, including this nugget:

The split between r-process and s-process production of heavier than iron (peak) elements is about 50:50. ie They weren't mainly made in supernovae, which is a frequent, incorrect claim.

but of most importance is Rob's final point:

The relative contributions of various sites to the r-process remains an unsettled matter. You could also read my answers on this topic in Physics Stack Exchange.

On following Rob's links I think this provides you with an excellent overall answer (and relative percentages)

A more up-to-date visualisation of what goes on (produced by Jennifer Johnson) and which attempts to identify the sites (as a percentage) for each chemical element is shown below. It should be stressed that the details are still subject to a lot of model-dependent uncertainty.

Looking at C and N - the majority seems to be from dying low mass stars, and Ca and Fe are from exploding stars, which indicates that Carl is not far off the mark.

• That image is great! Jan 12, 2019 at 13:10
• Wikipedia has a similar chart based on Johnson's data, but you can hover over an element to see the estimated percentages (as actual numbers) for each kind of nucleosynthesis. Jan 14, 2019 at 22:05

Sagan's quote is half-correct. While some of these elements are created during or immediately prior to a supernova of some sort, others are either partially or entirely fused during normal stellar nucleosynthesis. Nitrogen falls into the latter category, whereas calcium and iron have one foot in each. On the whole, though, calling these elements "starstuff" is pretty accurate.

# Nitrogen

My answer serves largely to complement Rory's, and to address the issue of nitrogen production in particular, partly since there is some disagreement as to how much high-mass stars produce. It is thought that the majority of nitrogen is produced in the carbon-nitrogen-oxygen (CNO) cycle, which includes the subprocess originally known as the CN cycle. The CNO cycle is only dominant in stars more massive than the Sun, partly because the energy generation rate is much more sensitive to temperature than the proton-proton chain (scaling as $$\epsilon\sim T^{20}$$, compared to $$\epsilon\sim T^4$$), largely because the Coulomb barrier is much higher for the CNO cycle.

Intermediate-mass AGB stars, with masses in the vicinity of $$5M_{\odot}$$, enrich the interstellar medium with nitrogen through strong stellar winds (1, 2), and are thought to be the most important contributors to nitrogen synthesis. AGB stars are post-main sequence stars that have ascended the red giant branch and are now large and luminous, undergoing shell burning of helium and hydrogen. Their high mass-loss rates are responsible for the enrichment, and most of this mass loss happens before the planetary nebula phase; therefore, I'd be reluctant to characterize the sources of nitrogen as even dying stars. They're simply old, evolved intermediate-mass stars - still not massive enough to undergo supernovae, but also not true low-mass stars.

In short, the answer to the nitrogen question is no, most nitrogen in the universe was not made from supernova nucleosynthesis, but was indeed made by lower-mass stars, in particular intermediate-mass AGB stars. The contributions of supernovae are, as indicated above, not agreed upon.

# Calcium

Calcium can indeed be produced via nucleosynthesis in massive stars, usually via silicon- and oxygen- based pathways that synthesize $$^{40}\text{Ca}$$, a common calcium isotope. Recently, discoveries of calcium-rich supernovae have indicated that those could be substantial contributors to calcium abundances. The characteristics of the progenitors are not yet known; they could be low-mass white dwarfs accreting matter from a companion, compact objects colliding, or higher-mass stars undergoing traditional core collapse supernovae. We don't have enough data to determine what the contribution of these supernovae is to calcium production, although it's being worked on.

# Iron

Much of the iron produced by stars is in the form of the isotope $$^{56}\text{Fe}$$, which is one of the end results of silicon burning in the extreme late stages (essentially the last day or so) of a high-mass star's life, as well as in supernovae. $$^{56}\text{Ni}$$ is initially synthesized but decays to $$^{56}\text{Co}$$ and eventually $$^{56}\text{Fe}$$.

• Thanks for the elaborations. Roughly speaking, is the $~T^20$ vs $~T^4$ mostly due to the higher coulomb barrier?
– uhoh
Jan 12, 2019 at 16:09
• @uhoh Yes; in the end, the CNO cycle is rate-limited by the high Coulomb barrier, and therefore has a higher temperature dependence. Jan 12, 2019 at 16:19
• Fluorine!
– uhoh
Nov 4, 2021 at 19:13