Two 3He nuclei fuse into one 4He nucleus and release two protons. This closes the main branch of the pp chain in the Sun.
Once 3He has been made, it can meet another 3He nucleus or a 4He nucleus. The first path ends the pp-I chain and produces no further neutrinos; the second opens the pp-II and pp-III branches, which emit the 7Be and 8B solar neutrinos. The competition between the two therefore sets how many of these neutrinos the Sun emits. In the 1990s the reaction was also measured to test the idea that an unknown low-energy resonance could explain the solar neutrino deficit.
Facts
- How well known
- Measured down to the energies at which the reaction runs in the Sun. The remaining uncertainty comes from the correction for the atomic electrons of the target, which make the reaction easier in the laboratory than it is for bare nuclei, and from the energy spectrum of the emitted protons.
- Live evaluation
- No live evaluation yet · Evaluations
- Reaction rates
- Explore the rates →
- Q-value · energy released
- 12.860 MeV
- Gamow window
- 22 ± 6.3 keVcentre of the Sun, 15.7 MK (pp-I)
- Kind
- Fusion
On the timeline
How it was measured
- Direct measurement underground
- Direct measurement at the surface
- Laser and inertial-confinement plasmas
5 measurements, 1996–2017, 3 at LUNAShow the listHide the list
1996
LUNA 50 kVLaboratori Nazionali del Gran Sasso (INFN)
Direct measurement underground · down to about 21 keV
First data inside the solar Gamow peak, no evidence for a low-energy resonance; tentative S(0) = 5.1 ± 0.1 MeV b after the screening correction. [1]
1998
LUNA 50 kVLaboratori Nazionali del Gran Sasso (INFN)
Direct measurement underground · down to 20.76 keV
Full analysis of the first LUNA campaign; electron screening observed clearly for this reaction, larger than expected, and dominating the uncertainty of the bare S(0) = 5.40 MeV b. [2]
1999
LUNA 50 kVLaboratori Nazionali del Gran Sasso (INFN)
Direct measurement underground · down to 16.5 keV
New detector setup; data down to the lower edge of the solar Gamow peak, with no sign of the narrow resonance proposed to reduce the 7Be and 8B neutrino fluxes. [3]
2004
RCNP, OsakaResearch Center for Nuclear Physics, Osaka University
Direct measurement at the surface · 30–50 keV
Doubly charged 3He beam free from molecular interference; S-factor in the gap left by LUNA, with smaller statistical and systematic errors than earlier data. [4]
2017
OMEGA laserLaboratory for Laser Energetics, University of Rochester
Laser and inertial-confinement plasmas · low centre-of-mass energy, plasma
Proton spectra from 3He+3He fusion in high-energy-density plasmas; the measured shape is proposed as a benchmark for the analysis of low-resolution accelerator data. [5]
Measurements (EXFOR)
Every dataset EXFOR holds for this reaction, drawn by the energies it covers, against the energies a star uses.
21 datasets in 10 EXFOR entries, 1966–2004
centre of the Sun, T₉ = 0.0157 (15.7 MK)
- Lowest energy in EXFOR
- 17 keV
- Bonetti et al., 1999 · S · A0379.002
- Distance from the Gamow peak
- Inside the window
- E₀ = 22.1 keV, window 15.8–28.4 keV
- Rate from energies not in EXFOR
- 7.3%
- at T₉ = 0.0157, smooth estimate · 7.3% of it lies below the lowest energy in EXFOR
- Gamow window, hatched where no measurement reaches
- Outlined bars are shown but not counted (the rule is under “How these numbers are made”).
- A diamond is a dataset at a single energy. Bars running off the right edge continue to higher energies.
The datasets of the gap map, by quantity
| Quantity | Datasets | E_cm range (keV) |
|---|---|---|
| σcross section | 6 | 29.8 keV – 12 MeV |
| SS-factor | 8 | 16.5 keV – 2.96 MeV |
| dσ/dΩangular distribution | 7 | 99.8 keV – 4.55 MeV |
How these numbers are made
Lowest measured energy, everywhere in the data explorer: the lowest centre-of-mass energy at which a dataset in EXFOR measures the reaction itself (cross section, S-factor, angular distribution, yield or resonance strength), judged point by point. A point counts when it is a value, not an upper or lower limit, when it lies at least one standard deviation above zero, and when its energy is physical: at least 1 keV for charged particles, and not below the threshold of an endothermic reaction. Not counted: extrapolated, calculated, evaluated or derived values; superseded, deleted or preliminary data; ratios; a single S-factor value, which in EXFOR is a fit result; and indirect methods (Trojan horse, Coulomb dissociation, ANC, surrogate reactions), recognized from EXFOR's method and analysis codes, their text and the title. Frame and unit errors of EXFOR are corrected first, and values the literature shows to be upper limits are read as limits, from a list that gives the evidence for each. Datasets that reach the same energy within 0.5% are all credited, earliest first. Rate from energies not in EXFOR: the share of the rate integrand at that temperature outside the energy ranges the counted datasets cover (from their lowest measured point to their highest), with a constant S-factor (σ ∝ S(E₀)/E · e^−2πη, so the integrand is e^(−E/kT − 2πη)); for a neutron capture, σ ∝ 1/v. Resonances make the real integrand lumpy, so read it as a smooth baseline.
Details
The two-proton exit channel makes the reaction measurable by detecting the energetic protons in silicon telescopes, which LUNA did with the 50 kV accelerator and a windowless 3He gas target. The data reached below the centre of the solar Gamow peak and excluded a narrow resonance there. The low-energy data show a rise of the S-factor due to electron screening by the atomic electrons of the target, larger than expected; the screening correction is the main uncertainty on the bare-nucleus S(0).
Measurements with a doubly charged 3He beam at Osaka, free of molecular-beam contamination, filled the energy gap above the LUNA range. Plasma experiments at laser facilities measured the proton spectrum, whose shape matters when low-resolution detectors are used.
Peak energy E0 ± half the 1/e width, centre of mass, from the AME2020 masses.
Evaluations
Compilations that combine the data into a recommended rate.
Open questions
- The origin of the electron-screening enhancement, which is larger than expected.
- The shape of the three-body proton spectrum and its effect on detection efficiencies.
Related reactions
References
- 1.
C. Arpesella et al. (LUNA Collaboration)
Measurement of the 3He(3He,2p)4He cross section within the solar Gamow peak
Phys. Lett. B 389, 452 (1996)LUNA
- 2.
M. Junker et al. (LUNA Collaboration)
Cross section of 3He(3He,2p)4He measured at solar energies
Phys. Rev. C 57, 2700 (1998) · 10.1103/PhysRevC.57.2700 · arXiv:nucl-ex/9707003LUNA
- 3.
R. Bonetti et al. (LUNA Collaboration)
First measurement of the 3He(3He,2p)4He cross section down to the lower edge of the solar Gamow peak
Phys. Rev. Lett. 82, 5205 (1999) · 10.1103/PhysRevLett.82.5205 · arXiv:nucl-ex/9902004LUNA
- 4.
N. Kudomi, M. Komori, K. Takahisa, S. Yoshida, K. Kume, H. Ohsumi, T. Itahashi
Precise measurement of cross section of 3He(3He,2p)4He by using 3He doubly charged beam
Phys. Rev. C 69, 015802 (2004) · 10.1103/PhysRevC.69.015802 · arXiv:astro-ph/0306454
- 5.
A. B. Zylstra et al.
Phys. Rev. Lett. 119, 222701 (2017) · 10.1103/PhysRevLett.119.222701
- 6.
E. G. Adelberger et al.
Solar fusion cross sections II: the pp chain and CNO cycles
Rev. Mod. Phys. 83, 195 (2011) · 10.1103/RevModPhys.83.195
- 7.
B. Acharya et al.
Solar fusion III: New data and theory for hydrogen-burning stars
Rev. Mod. Phys. 97, 035002 (2025) · 10.1103/8lm7-gs18 · arXiv:2405.06470
How to cite this page
J. Skowronski, 3He(3He,2p)4He, in Reaction atlas, 2026-10-12, https://jskowron.eu/atlas/3He-3He2p-4He.
Cite the date you used; it is the last change to this page.
Something wrong or missing? Report an error (opens a new issue on GitHub) · Suggest a reaction (opens a new issue on GitHub)