Astronomy:CNO cycle

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Short description: Catalysed fusion reactions by which stars convert hydrogen to helium
Logarithm of the relative energy output (ε) of proton–proton (p-p), CNO, and 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.

The CNO cycle (for carbon–nitrogen–oxygen; 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.[1]

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 carbon, nitrogen, and oxygen isotopes 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, all these cycles have the same net result:

4 11H   +   2 e−
  →   42He   +   2 e+   +   2 e−   +   2 νe   +   3 γ   +   24.7 MeV
  →   42He   +   2 νe   +   7 γ   +   26.7 MeV

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.[2] One nucleus goes on to become carbon, nitrogen, and oxygen isotopes through a number of transformations in an endless loop.

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 4×106 K[3] (4 megakelvin), making it the dominant energy source in smaller stars. A self-maintaining CNO chain starts at approximately 15×106 K, but its energy output rises much more rapidly with increasing temperatures[1] so that it becomes the dominant source of energy at approximately 17×106 K.[4]

The Sun has a core temperature of around 15.7×106 K, and only 1.7% of 4He nuclei produced in the Sun are born in the CNO cycle.

The CNO-I process was independently proposed by Carl von Weizsäcker[5][6] and Hans Bethe[7][8] in the late 1930s.

The first reports of the experimental detection of the neutrinos produced by the CNO cycle in the Sun were published in 2020. 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.[2][9][10]

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[5][6] and Hans Bethe. Bethe's 1939 papers on the CN-cycle[7][8] drew on three earlier papers written in collaboration with Robert Bacher and Milton Stanley Livingston[11][12][13] and which came to be known informally as "Bethe's Bible". It was considered the standard work on nuclear physics for many years and was a significant factor in his being awarded the 1967 Nobel Prize in Physics.[14] Bethe's original calculations suggested the CN-cycle was the Sun's primary source of energy.[7][8] This conclusion arose from a belief that is now known to be mistaken, that the abundance of nitrogen in the sun is approximately 10%; it is actually less than half a percent.[15] The CN-cycle, named as it contains no stable isotope of oxygen, involves the following cycle of transformations:[15]

126C   →  137N   →  136C   →   147N   →   158O   →   157N   →   126C

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:[15]

126C  +  11H  →  137N  +  Gamma      +  1.95 MeV
137N      →  136C  +  Positron  +  Electron Neutrino  +  1.20 MeV (half-life of 9.965 minutes[16])
136C  +  11H  →  147N  +  γ      +  7.54 MeV
147N  +  11H  →  158O  +  γ      +  7.35 MeV
158O      →  157N  +  e+  +  νe  +  1.73 MeV (half-life of 2.034 minutes[16])
157N  +  11H  →  126C  +  42He      +  4.96 MeV

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 2.04 MeV, 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.[17]

The limiting (slowest) reaction in the CNO-I cycle is the proton capture on 147N. In 2006 it was experimentally measured down to stellar energies, revising the calculated age of globular clusters by around 1 billion years.[18]

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 electron and the neutrino is not great enough to cause a significant recoil of the much heavier daughter nucleus[lower-alpha 1] 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 1.20 MeV, and the neutrino emitted during the decay of oxygen-15 can have an energy from zero up to 1.73 MeV. On average, about 1.7 MeV of the total energy output is taken away by neutrinos for each loop of the cycle, leaving about 25 MeV available for producing luminosity.[19]

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 157N shown above does not produce carbon-12 and an alpha particle, but instead produces oxygen-16 and a photon and continues

157N→168O→179F→178O→147N→158O→157N

In detail:

157N  +  11H  →  168O  +  γ      +  12.13 MeV
168O  +  11H  →  179F  +  γ      +  0.60 MeV
179F      →  178O  +  e+  +  νe  +  2.76 MeV (half-life of 64.49 seconds)
178O  +  11H  →  147N  +  42He      +  1.19 MeV
147N  +  11H  →  158O  +  γ      +  7.35 MeV
158O      →  157N  +  e+  +  νe  +  2.75 MeV (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 gamma instead of nitrogen-14 and alpha, and continues

178O → 189F → 188O → 157N → 168O → 179F → 178O

In detail:

178O  +   11H  →   189F  +   γ       +   5.61 MeV
189F       →   188O   +   e+   +   νe   +   1.656 MeV (half-life of 109.771 minutes)
188O   +   11H   →   157N   +   42He       +   3.98 MeV
157N   +   11H  →   168O   +   γ       +   12.13 MeV
168O   +   11H   →   179F   +   γ       +   0.60 MeV
179F       →   178O   +   e+   +   νe   +   2.76 MeV (half-life of 64.49 seconds)

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 gamma instead of nitrogen-15 and alpha, and continues: 188O→199F→168O→179F→178O→189F→188O

In detail:

188O  +  11H  →  199F  +  γ      +  7.994 MeV
199F  +  11H  →  168O  +  42He      +  8.114 MeV
168O  +  11H  →  179F  +  γ      +  0.60 MeV
179F      →  178O  +  e+  +  νe  +  2.76 MeV (half-life of 64.49 seconds)
178O  +  11H  →  189F  +  γ      +  5.61 MeV
189F      →  188O  +  e+  +  νe  +  1.656 MeV (half-life of 109.771 minutes)

In some instances 189F can combine with a helium nucleus to start a sodium-neon cycle.[20]

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.[clarification needed]

HCNO-I

The difference between the CNO-I cycle and the HCNO-I cycle is that 137N captures a proton instead of decaying, leading to the total sequence

126C→137N→148O→147N→158O→157N→126C

In detail:

126C  +  11H  →  137N  +  Gamma      +  1.95 MeV
137N  +  11H  →  148O  +  Gamma      +  4.63 MeV
148O      →  147N  +  Positron  +  Electron Neutrino  +  5.14 MeV (half-life of 70.641 seconds)
147N  +  11H  →  158O  +  γ      +  7.35 MeV
158O      →  157N  +  e+  +  νe  +  2.75 MeV (half-life of 122.24 seconds)
157N  +  11H  →  126C  +  42He      +  4.96 MeV

HCNO-II

The notable difference between the CNO-II cycle and the HCNO-II cycle is that 179F captures a proton instead of decaying, and neon is produced in a subsequent reaction on 189F, leading to the total sequence

157N→168O→179F→1810Ne→189F→158O→157N

In detail:

157N  +  11H  →  168O  +  γ      +  12.13 MeV
168O  +  11H  →  179F  +  γ      +  0.60 MeV
179F  +  11H  →  1810Ne  +  γ      +  3.92 MeV
1810Ne      →  189F  +  e+  +  νe  +  4.44 MeV (half-life of 1.672 seconds)
189F  +  11H  →  158O  +  42He      +  2.88 MeV
158O      →  157N  +  e+  +  νe  +  2.75 MeV (half-life of 122.24 seconds)

HCNO-III

An alternative to the HCNO-II cycle is that 189F captures a proton moving towards higher mass and using the same helium production mechanism as the CNO-IV cycle as

189F→1910Ne→199F→168O→179F→1810Ne→189F

In detail:

189F  +  11H  →  1910Ne  +  γ      +  6.41 MeV
1910Ne      →  199F  +  e+  +  νe  +  3.32 MeV (half-life of 17.22 seconds)
199F  +  11H  →  168O  +  42He      +  8.11 MeV
168O  +  11H  →  179F  +  γ      +  0.60 MeV
179F  +  11H  →  1810Ne  +  γ      +  3.92 MeV
1810Ne      →  189F  +  e+  +  νe  +  4.44 MeV (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.[citation needed]

See also

Footnotes

  1. ↑ Note: It is not important how invariant masses of e and ν are small, because they are already small enough to become relativistic. What is important is that the daughter nucleus is heavy compared to p/c .

References

  1. ↑ 1.0 1.1 Salaris, Maurizio; Cassisi, Santi (2005). Evolution of Stars and Stellar Populations. John Wiley and Sons. pp. 119–121. ISBN 0-470-09220-3. https://archive.org/details/evolutionofstars0000sala. 
  2. ↑ 2.0 2.1 Agostini, M.; Altenmüller, K.; et al. (The BOREXINO collaboration) (25 June 2020). "First Direct Experimental Evidenceof CNO neutrinos" (PDF). arXiv:2006.15115 [hep-ex].
  3. ↑ Reid, I. Neill; Hawley, Suzanne L. (2005). "The structure, formation, and evolution of low-mass stars and brown dwarfs – Energy generation". New Light on Dark Stars: Red dwarfs, low-mass stars, brown dwarfs. Springer-Praxis Books in Astrophysics and Astronomy (2nd ed.). Springer Science & Business Media. pp. 108–111. ISBN 3-540-25124-3. https://books.google.com/books?id=o7pe7Fp4JaAC&pg=PA108. 
  4. ↑ Schuler, S.C.; King, J.R.; The, L.-S. (2009). "Stellar Nucleosynthesis in the Hyades open cluster". The Astrophysical Journal 701 (1): 837–849. doi:10.1088/0004-637X/701/1/837. Bibcode: 2009ApJ...701..837S. 
  5. ↑ 5.0 5.1 "Über Elementumwandlungen in Innern der Sterne I". Physikalische Zeitschrift 38: 176–191. 1937. 
  6. ↑ 6.0 6.1 "Über Elementumwandlungen in Innern der Sterne II". Physikalische Zeitschrift 39: 633–646. 1938. 
  7. ↑ 7.0 7.1 7.2 "Energy Production in Stars". Physical Review 55 (1): 541–7. 1939. doi:10.1103/PhysRev.55.103. PMID 17835673. Bibcode: 1939PhRv...55..103B. 
  8. ↑ 8.0 8.1 8.2 "Energy production in stars". Physical Review 55 (5): 434–456. 1939. doi:10.1103/PhysRev.55.434. PMID 17835673. Bibcode: 1939PhRv...55..434B. 
  9. ↑ Agostini, M.; Altenmüller, K.; Appel, S.; Atroshchenko, V.; Bagdasarian, Z.; Basilico, D.; Bellini, G.; Benziger, J. et al. (25 November 2020). "Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun" (in en). Nature 587 (7835): 577–582. doi:10.1038/s41586-020-2934-0. ISSN 1476-4687. PMID 33239797. https://www.nature.com/articles/s41586-020-2934-0. "This result therefore paves the way towards a direct measurement of the solar metallicity using CNO neutrinos. Our findings quantify the relative contribution of CNO fusion in the Sun to be of the order of 1 per cent;". 
  10. ↑ "Neutrinos yield first experimental evidence of catalyzed fusion dominant in many stars" (in en). https://phys.org/news/2020-11-neutrinos-yield-experimental-evidence-catalyzed.html. "Pocar points out, "Confirmation of CNO burning in our sun, where it operates at only one percent, reinforces our confidence that we understand how stars work."" 
  11. ↑ "Nuclear Physics, A: Stationary states of nuclei". Reviews of Modern Physics 8 (2): 82–229. 1936. doi:10.1103/RevModPhys.8.82. Bibcode: 1936RvMP....8...82B. https://authors.library.caltech.edu/51288/1/RevModPhys.8.82.pdf. 
  12. ↑ "Nuclear Physics, B: Nuclear dynamics, theoretical". Reviews of Modern Physics 9 (2): 69–244. 1937. doi:10.1103/RevModPhys.9.69. Bibcode: 1937RvMP....9...69B. 
  13. ↑ "Nuclear Physics, C: Nuclear Dynamics, Experimental". Reviews of Modern Physics 9 (2): 245–390. 1937. doi:10.1103/RevModPhys.9.245. Bibcode: 1937RvMP....9..245L. 
  14. ↑ Bardi, Jason Socrates (January 23, 2008). "Landmarks: What makes the stars shine?". Physical Review Focus 21 (3). doi:10.1103/physrevfocus.21.3. https://physics.aps.org/story/v21/st3. Retrieved November 26, 2018. 
  15. ↑ 15.0 15.1 15.2 Krane, Kenneth S. (1988). Introductory Nuclear Physics. John Wiley & Sons. p. 537. ISBN 0-471-80553-X. https://archive.org/details/introductorynucl00kran. 
  16. ↑ 16.0 16.1 Ray, Alak (2010). "Massive stars as thermonuclear reactors and their explosions following core collapse". in Goswami, Aruna; Reddy, B. Eswar. Principles and Perspectives in Cosmochemistry. Springer Science & Business Media. p. 233. ISBN 9783642103681. https://books.google.com/books?id=gCr9WVH0utwC&pg=PA233. 
  17. ↑ Wapstra, Aaldert; Audi, Georges (18 November 2003). "The 2003 Atomic Mass Evaluation". Atomic Mass Data Center. http://amdc.in2p3.fr/web/masseval.html. 
  18. ↑ Lemut, A.; Bemmerer, D.; Confortola, F.; Bonetti, R.; Broggini, C.; Corvisiero, P. et al. (2006). "First measurement of the 14N(p,γ)15O cross section down to 70 keV". Physics Letters B 634 (5–6): 483–487. doi:10.1016/j.physletb.2006.02.021. Bibcode: 2006PhLB..634..483L. 
  19. ↑ Scheffler, Helmut; Elsässer, Hans (1990). Die Physik der Sterne und der Sonne. Bibliographisches Institut (Mannheim, Wien, Zürich). ISBN 3-411-14172-7. 
  20. ↑ https://core.ac.uk/download/pdf/31144835.pdf

Further reading




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