I have been investigating this isotope of helium for a while, which is extremely abundant on the moon (and in general in the entire solar system except on planets with atmosphere). It is believed that it could be used as a fusion fuel $(\text{²H} +\text{³He}\to \text{⁴He} + \text{n}, \text{³He} +\text{³He}\to \text{⁴He} + 2\text{n})$ and since it is not radioactive and nothing would be the perfect energy source, but there is very little on earth because the atmosphere "does not let it pass".

It is known that the moon is full of it, but my question is, how do we detect it?

There are many articles that this element could be a source of infinite energy etc. but I have not found published explanations on how presence and concentration could or has be detected.

While China is already planning to do some tests with this element on the moon, there are (as yet) no published concentration maps.


NASA [1] indicates that helium-3 can be assessed indirectly by measuring the presence of titanium dioxide and soil characteristics ("maturity"), the correlation having been derived from the study of Apollo lunar rock samples. The helium-3 is "detected" through remote analysis for these favorable mineral and soil characteristics. Using data on the titanium level and soil characteristics from the Clementine spacecraft combined with with it's own microwave measurements of the thickness of the regolith, Chang-e 1 produced a map of likely helium-3 concentrations in the regolith [2, 3]. Although the near and far sides contain roughly equal amounts of helium-3 overall, higher concentrations (or at least, more favorable titanium levels and soil characteristics) are found in regions of the near side corresponding roughly to the major lunar seas. Chang-e 1's map, taken from [3], is given below.

enter image description here


  1. Lunar Helium-3 and Fusion Power, NASA Publication 10018 (1988), p. 26.

  2. W.-Z. Fa and Y.-Q. Jin, "Global inventory of Helium-3 in lunar regoliths estimated by a multi-channel microwave radiometer on the Chang-E 1 lunar satellite", Chinese Svience Bulletin 55, pages4005–4009(2010). (Link)

  3. "Chang-e 1 Maps Moon's Helium-3 Inventory", http://lunarnetworks.blogspot.com/2010/12/change-1-maps-moons-helium-3-inventory.html?m=1

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    $\begingroup$ Not sure about those units. Ppb or ppm usually is not based on area or volume. $\endgroup$ Mar 30 '20 at 11:16
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    $\begingroup$ @OscarLanzi ya agreed, it's a blogpost so probably hasn't seen any peer review. Areal density (for example picograms/m^2) would make sense for a deposited material that will only be found near the surface, but ppb can't have a /m^2 after it. $\endgroup$
    – uhoh
    Mar 30 '20 at 11:25
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    $\begingroup$ @Cornelisinspace thanks for that, but I have a hunch it's a typo or something else. $\endgroup$
    – uhoh
    Mar 30 '20 at 11:26
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    $\begingroup$ @uhoh en.wikipedia.org/wiki/… $\endgroup$
    – Cornelis
    Mar 30 '20 at 11:34
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    $\begingroup$ @Cornelisinspace yep, that looks nicer :-) $\endgroup$
    – uhoh
    Mar 30 '20 at 11:36

@OscarLanzi's reality-based answer

is thorough and excellent!

In short, the 3He flux from the Sun is known and how deep those particles will embed themselves in the regolith surface and the rate of regolith heating, cooling, and overturn by meteorites can all be modeled.

So the methods outlined do not actually detect 3He at all, they just assume that it must be there.

Here I'll address the "could" part of the question

How could the presence of 3He be detected on the lunar surface?

but I have not found published explanations on how presence and concentration could or has be detected.

If I wanted to find direct evidence of 3He on the Moon and try to make a quantitative measurement of it, I would look for ~21 MeV gamma rays produced by thermal neutron capture of 3He.

From Energy Levels of Light Nuclei; A=4 (1992) starting with reaction #14: 3He(n, γ)4He, Qm = 20.578 and

Table 4.14: Measured values for the thermal neutron capture cross section for the 3H(n, γ) 4He reaction

we can see that this reaction leading to a distinct high-energy gamma ray (or it's detailed-balance inverse) has astrophysical implications and for diagnostics of fusion reactors so has been studied extensively.

The thermal neutron radiative capture cross-section is about 60 micro-barns (yes) which is not big but it's not vanishingly small either.

Water has been successfully(?) prospected on the moon via energetic neutron scattering by protons (hydrogen) but I don't know the thermal neutron flux at the Moon's surface well enough to estimate the gamma ray rate expected in orbit.

Since the coverage is expected to be widespread, it won't be any stronger if you are 1 meter above the Moon than if you were in orbit 100 km above it, for the same reason that a wall doesn't get brighter when you walk towards it. (cf. etendue)

Now, a detector that can capture a 20.6 MeV gamma ray and determine its energy precisely will be a bit of a challenge. A big old NaI scintillator would work, but it would have to be pretty big to contain the full shower produced by such a high energy gamma ray. For this energy one might look into the lower resolution BGO (bismuth germinate) scintillator detectors, smaller because bismuth and germanium have a lot more electrons and higher nuclear charge for shower-stopping, but perhaps just as heavy.

If the gamma ray background is too high, then you'll need a gamma ray detector with much higher resolution, so that a weak peak might stand out more sharply. A germanium detector (a big single crystal germanium reverse-biased diode) would provide much higher resolution, but again it would have to be exceedingly large to contain all the energy of a 20.6 MeV gamma ray much of the time.

Fig. 2: The energy levels of 4He are plotted on a vertical scale giving the c.m. energy, in MeV, relative to its ground state.

Source: Energy Levels of Light Nuclei; A=4 (1992)

Fig. 2: The energy levels of 4He are plotted on a vertical scale giving the c.m. energy, in MeV, relative to its ground state. Horizontal lines representing the levels are labeled by the level energies and values of total angular momentum, parity, and isospin (Jπ, T ). Also shown are threshold energies and typical thin-target excitation functions for some of the reactions in the 4He system. See Fig. 1 for further details about notation and Table 4.3 for more information about the levels, including partial and total widths.


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