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CNO cycle

Nuclear fusion reaction

Summary

Nuclear fusion reaction

triple-α]] fusion processes at different temperatures (T). The dashed line shows the combined energy generation of the p–p and CNO processes within a star.

In astrophysics, the carbon–nitrogen–oxygen (CNO) cycle, sometimes called Bethe–Weizsäcker cycle, after Hans Albrecht Bethe and Carl Friedrich von Weizsäcker, is one of the two known sets of fusion reactions by which stars convert hydrogen to helium, the other being the proton–proton chain reaction (p–p cycle), which is more efficient at the Sun's core temperature. The CNO cycle is hypothesized to be dominant in stars that are more than 1.3 times as massive as the Sun.

Unlike the proton-proton reaction, which consumes all its constituents, the CNO cycle is a catalytic cycle. In the CNO cycle, four protons fuse, using isotopes of carbon, nitrogen, and oxygen as catalysts, each of which is consumed at one step of the CNO cycle, but re-generated in a later step. The end product is one alpha particle (a stable helium nucleus), two positrons, and two electron neutrinos.

There are various alternative paths and catalysts involved in the CNO cycles, but all these cycles have the same net result: :4 + 2 :: → + 2 + 2 + 2 + 3 +
:: → + 2 + 7 +

The positrons will almost instantly annihilate with electrons, releasing energy in the form of gamma rays. The neutrinos escape from the star carrying away some energy.{{cite journal |display-authors=2

Overview of the CNO-I Cycle

The proton–proton chain is more prominent in stars the mass of the Sun or less. This difference stems from temperature dependency differences between the two reactions; pp-chain reaction starts at temperatures around {{cite book | chapter-url=https://books.google.com/books?id=o7pe7Fp4JaAC&pg=PA108 }} (4 megakelvins), making it the dominant energy source in smaller stars. A self-maintaining CNO chain starts at approximately , but its energy output rises much more rapidly with increasing temperatures{{cite book | url-access=registration

The Sun has a core temperature of around , and only of nuclei produced in the Sun are born in the CNO cycle.

The CNO-I process was independently proposed by Carl von Weizsäcker |trans-title= On transformations of elements in the interiors of stars I |trans-title= On transformations of elements in the interiors of stars II |doi-access = free

The first reports of the experimental detection of the neutrinos produced by the CNO cycle in the Sun were published in 2020 by the BOREXINO collaboration. This was also the first experimental confirmation that the Sun had a CNO cycle, that the proposed magnitude of the cycle was accurate, and that von Weizsäcker and Bethe were correct.

Cold CNO cycles

Under typical conditions found in stars, catalytic hydrogen burning by the CNO cycles is limited by proton captures. Specifically, the timescale for beta decay of the radioactive nuclei produced is faster than the timescale for fusion. Because of the long timescales involved, the cold CNO cycles convert hydrogen to helium slowly, allowing them to power stars in quiescent equilibrium for many years.

CNO-I

The first proposed catalytic cycle for the conversion of hydrogen into helium was initially called the carbon–nitrogen cycle (CN-cycle), also referred to as the Bethe–Weizsäcker cycle in honor of the independent work of Carl Friedrich von Weizsäcker in 1937–38 and Hans Bethe. Bethe's 1939 papers on the CN-cycle{{cite journal |article-number = 3 |access-date = 26 November 2018 |url-access=limited : → → → → → →

This cycle is now understood as being the first part of a larger process, the CNO-cycle, and the main reactions in this part of the cycle (CNO-I) are: C-12 + H - N-13 + y _ _ + 1.95 MeV N-13 _ _ - C-13 + e+ + ve + 1.20 MeV C-13 + H - N-14 + y _ _ + 7.54 MeV N-14 + H - O-15 + y _ _ + 7.35 MeV O-15 _ _ - N-15 + e+ + ve + 2.75 MeV N-15 + H - C-12 + He _ _ + 4.96 MeV

:{| border="0" |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ || ||(half-life of 9.965 minutes{{cite book |editor1-first = Aruna |editor1-last = Goswami |editor2-first = B. Eswar |editor2-last = Reddy |chapter-url = https://books.google.com/books?id=gCr9WVH0utwC&pg=PA233 |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 122.24 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |} where the carbon-12 nucleus used in the first reaction is regenerated in the last reaction. After the two positrons emitted annihilate with two ambient electrons producing an additional , the total energy released in one cycle is 26.73 MeV; in some texts, authors are erroneously including the positron annihilation energy in with the beta-decay Q-value and then neglecting the equal amount of energy released by annihilation, leading to possible confusion. All values are calculated with reference to the Atomic Mass Evaluation 2003.{{cite web |access-date=25 October 2011 |archive-date=28 September 2011 |archive-url=https://web.archive.org/web/20110928003450/http://amdc.in2p3.fr/web/masseval.html

The limiting (slowest) reaction in the CNO-I cycle is the proton capture on . In 2006 it was experimentally measured down to stellar energies, revising the calculated age of globular clusters by around 1 billion years.

The neutrinos emitted in beta decay will have a spectrum of energy ranges, because although momentum is conserved, the momentum can be shared in any way between the positron and neutrino, with either emitted at rest and the other taking away the full energy, or anything in between, so long as all the energy from the Q-value is used. The total momentum received by the positron and the neutrino is not great enough to cause a significant recoil of the much heavier daughter nucleus and hence, its contribution to kinetic energy of the products, for the precision of values given here, can be neglected. Thus the neutrino emitted during the decay of nitrogen-13 can have an energy from zero up to , and the neutrino emitted during the decay of oxygen-15 can have an energy from zero up to . On average, about 1.7 MeV of the total energy output is taken away by neutrinos for each loop of the cycle, leaving about available for producing luminosity. | trans-title = The Physics of the Stars and the Sun

CNO-II

In a minor branch of the above reaction, occurring in the Sun's core 0.04% of the time, the final reaction involving shown above does not produce carbon-12 and an alpha particle, but instead produces oxygen-16 and a photon and continues :{{Separated entries ||||||||separator= → }}

In detail:

N-15 + H - O-16 + y _ _ + 12.13 MeV O-16 + H - F-17 + γ _ _ + 0.60 MeV F-17 _ _ - O-17 + e+ + νe + 2.76 MeV O-17 + H - N-14 + He _ _ + 1.19 MeV N-14 + H - O-15 + y _ _ + 7.35 MeV O-15 _ _ - N-15 + e+ + ve + 2.75 MeV

--:{| border="0" |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 64.49 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 122.24 seconds) |}

Like the carbon, nitrogen, and oxygen involved in the main branch, the fluorine produced in the minor branch is merely an intermediate product; at steady state, it does not accumulate in the star.

CNO-III

This subdominant branch is significant only for massive stars. The reactions are started when one of the reactions in CNO-II results in fluorine-18 and a photon instead of nitrogen-14 and an alpha particle, and continues : → → → → → →

In detail:

:{| border="0" |- style="height:2em;" | || + || || → || || + || || || || + || |- style="height:2em;" | || || || → || || + || || + || || + || || (half-life of ) |- style="height:2em;" | || + || || → || || + || || || || + || |- style="height:2em;" | || + || || → || || + || || || || + || |- style="height:2em;" | || + || || → || || + || || || || + || |- style="height:2em;" | || || || → || || + || || + || || + || || (half-life of ) |}

CNO-IV

A proton reacts with a nucleus causing release of an alpha particle.

Like the CNO-III, this branch is also only significant in massive stars. The reactions are started when one of the reactions in CNO-III results in fluorine-19 and a photon instead of nitrogen-15 and an alpha particle, and continues :{{Separated entries| |||||||separator= → }}

In detail:

:{| border="0" | || + || ||→ || || + || || || || + || |- | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 64.49 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 109.771 minutes) |- style="height:2em;" |}

In some instances can combine with a helium nucleus, forming , to start a neon-sodium cycle, in which:

||separator= → }}

The sodium-23 can also turn into magnesium-24 after proton bombardment, initiating a magnesium-aluminum cycle, in which:

|||||||separator= → }}

Hot CNO cycles

Under conditions of higher temperature and pressure, such as those found in novae and X-ray bursts, the rate of proton captures exceeds the rate of beta-decay, pushing the burning to the proton drip line. The essential idea is that a radioactive species will capture a proton before it can beta decay, opening new nuclear burning pathways that are otherwise inaccessible. Because of the higher temperatures involved, these catalytic cycles are typically referred to as the hot CNO cycles; because the timescales are limited by beta decays instead of proton captures, they are also called the beta-limited CNO cycles.

HCNO-I

The difference between the CNO-I cycle and the HCNO-I cycle is that captures a proton instead of decaying, leading to the total sequence :→→→→→→

In detail:

:{| border="0" |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 70.641 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 122.24 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |}

HCNO-II

The notable difference between the CNO-II cycle and the HCNO-II cycle is that captures a proton instead of decaying, and neon is produced in a subsequent reaction on , leading to the total sequence

:→→→→→→

In detail:

:{| border="0" |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 1.672 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 122.24 seconds) |}

HCNO-III

An alternative to the HCNO-II cycle is that captures a proton moving towards higher mass and using the same helium production mechanism as the CNO-IV cycle as :→→→→→→

In detail:

:{| border="0" |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 17.22 seconds) |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | ||+ || ||→ || ||+ || || || ||+ || |- style="height:2em;" | || || ||→ || ||+ || ||+ || ||+ ||||(half-life of 1.672 seconds) |}

Use in astronomy

While the total number of "catalytic" nuclei are conserved in the cycle, in stellar evolution the relative proportions of the nuclei are altered. When the cycle is run to equilibrium, the ratio of the carbon-12/carbon-13 nuclei is driven to 3.5, and nitrogen-14 becomes the most numerous nucleus, regardless of initial composition. During a star's evolution, convective mixing episodes moves material, within which the CNO cycle has operated, from the star's interior to the surface, altering the observed composition of the star. Red giant stars are observed to have lower carbon-12/carbon-13 and carbon-12/nitrogen-14 ratios than do main sequence stars, which is considered to be convincing evidence for the operation of the CNO cycle.

Footnotes

References

(25 November 2020). "Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun". Nature.
"Neutrinos yield first experimental evidence of catalyzed fusion dominant in many stars".
Depalo, Rosanna. "The neon-sodium cycle: Study of the 22Ne(p, γ)23Na reaction at astrophysical energies".
(2016-01-05). "Towards a study of 22 Ne(p γ ) 23 Na at LUNA". Journal of Physics: Conference Series.
(2013-02-01). "Impact of a Revised 25Mg(p,g)26Al Reaction Rate on the Operation of the Mg-Al Cycle". The Astrophysical Journal.
(December 1998). "The chemical evolution of the secondary stars in close binaries, arising from common-envelope evolution and nova outbursts". Monthly Notices of the Royal Astronomical Society.

Wikipedia Source

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nuclear-fusion-reactions carbon nitrogen oxygen fluorine neon nucleosynthesis hans-bethe

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