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Cold dark matter is thought to fill our galactic neighborhood with a density $\rho$ of about 0.3 GeV/cm${}^3$ and with a velocity $v$ of roughly 200 to 300 km/s. (The velocity dispersion is much debated.) For a given dark matter mass $m$ and nucleon scattering cross section $\sigma$, this will lead to a constant collision rate of roughly

$r \sim \rho v \sigma / m$

for every nucleon in normal matter. The kinetic energy transferred to the nucleon (which is essentially at rest) will be roughly

$\Delta E \sim 2 v^2 \frac{M m^2}{(m+M)^2}$,

where $M \approx 1$ amu $\approx 1$ GeV/c${}^2$ is the mass of a nucleon. The limits for light ($m \ll M$) and heavy ($m \gg M$) dark matter are

$\Delta E_\mathrm{light} \sim 2 v^2 \frac{m^2}{M}$ and $\Delta E_\mathrm{heavy} \sim 2 v^2 M$.

This leads to an apparent intrinsic heat production in normal matter

$\tilde{P} \sim r \Delta E / M$,

which is measured in W/kg. The limits are

$\tilde{P}_\mathrm{light} \sim 2 \rho v^3 \sigma m / M^2$ and $\tilde{P}_\mathrm{heavy} \sim 2 \rho v^3 \sigma / m$.

What existing experiment or observation sets the upper limit on $\tilde{P}$?

(Note that $\tilde{P}$ is only sensibly defined on samples large enough to hold onto the recoiling nucleon. For tiny numbers of atoms--e.g. laser trap experiments--the chance of any of the atoms colliding with dark matter is very small, and those that do will simply leave the experiment.)

The best direct limit I could find looking around the literature comes from dilution refrigerators. The NAUTILUS collaboration (resonant-mass gravitational wave antenna) cooled a 2350 kg aluminum bar down to 0.1 K and estimated that the bar provided a load of no more than 10 $\mu$W to the refrigerator. Likewise, the (state-of-the-art?) Triton dilution refrigerators from Oxford Instruments can cool a volume of (240 mm)${}^3$ (which presumably could be filled with lead for a mass of about 150 kg) down to ~8mK. Extrapolating the cooling power curve just a bit, I estimated it handled about $10^{-7}$ W at that temperature.

In both cases, it looked like the direct limit on intrinsic heating is roughly $\tilde{P} < 10^{-9}$W/kg.

However, it looks like it's also possible to use the Earth's heat budget to set a better limit. Apparently, the Earth produces about 44 TW of power, of which about 20 TW is unexplained. Dividing this by the mass of the Earth, $6 \times 10^{24}$ kg, limits the intrinsic heating to $\tilde{P} < 3 \times 10^{-12}$W/kg.

Is this Earth-heat budget argument correct? Is there a better limit elsewhere?

To give an example, the CDMS collaboration searches for (heavy) dark matter in the range 1 to 10${}^3$ GeV/c${}^2$ with sensitivities to cross sections greater than 10${}^{-43}$ to 10${}^{-40}$ cm${}^2$ (depending on mass). A 100 GeV dark matter candidate with a cross-section of 10${}^{-43}$ cm${}^2$ would be expected to generate $\tilde{P} \sim 10^{-27}$ W/kg, which is much too small to be observed.

On the other hand, a 100 MeV dark matter particle with a cross-section of $10^{-27}$ cm${}^2$ (which, although not nearly as theoretically motivated as heavier WIMPs, is not excluded by direct detection experiments) would be expected to generate $\tilde{P} \sim 10^{-10}$ W/kg. This would have shown up in measurements of the Earth's heat production.

EDIT: So it looks like I completely neglected the effects of coherent scattering, which has the potential to change some of these numbers by 1 to 2 orders of magnitude. Once I learn more about this, I will update the question.

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Great Question! Starting a bounty on it! –  FrankH Oct 22 '12 at 20:21
Unfortunately still no answers. Perhaps this preprint on astroseismology might tangentially spark ideas. It just came out today, and is very preliminary, but the basic idea is DM may cool cores of stars via scattering, and such cooling may alter the internal structure enough to detectably change the pulsation spectrum. –  Chris White Dec 17 '12 at 0:10
I can't offer much --- but I did recently hear a talk about DM direct detection (regarding:, and this question was asked. The rough answer was that heating can't provide as good constraints on cross-sections as lower-limits from WMAP signatures, and upper-limits from line-surveys. –  DilithiumMatrix Dec 26 '12 at 21:48
Concerning the geological heating limit: potassium-40 decays are not included in the neutrino measurements (due to threshold effects) and contribute to the otherwise unexplained 20 TW. See and for descriptions of the LOS geo-neutrino measurements. –  dmckee Mar 14 '13 at 20:41
The Mack et al. article the question cites about Earth's heat budget say "Obviously, the possibility to make direct heat flow measurements under the surface is unique to Earth", however, two Apollo missions actually did drill into the Moon and determine heat flux. –  DavePhD Feb 28 '14 at 14:09

1 Answer 1

Dark matter is not the only possible source of heat in ordinary matter: cosmic rays and similar would also heat ordinary matter. Experiments searching for dark matter see a great deal of heat from cosmic rays and look very hard for but have not yet found dark matter, which is looked for primarily by the heat it deposits. This is to say: when dark matter hits a nucleus the nucleus recoils, depositing some energy in a detector, but causing very little ionization, relative to (most) cosmic rays. This energy deposition quickly (particularly in CDMS, but also in other experiments) becomes heat which (in turn) is detected directly because it heats a bolometer or indirectly because it (for example) nucleates bubbles. With careful experimental techniques that allow the energy deposited to be seen quickly and distinguished from other energy depositions. These experiments show that there is orders of magnitude more heating / deposition of energy from cosmic rays than from dark matter, and by extension this is true for all matter not well shielded from cosmic rays e.g. effectively all matter we can imagine "seeing". Actually, this is too weak a statement: even in well shielded locations (deep mines) there is much more heat deposition from cosmic rays than dark matter. So, (in effect) I think that the best recent published limit on dark matter detection will for the forseeable future be the best limit on heating from dark matter. I suppose, this assumes that we know pretty well what the relative cross section of dark matter with different kinds of matter is. I suppose that if, contrary to all expectations, dark matter interacts strongly with something not yet used in a detector and weakly with stuff that has, this could be wrong. But, that is "not expected".

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"... dark matter, which is looked for primarily by the heat it deposits" Hmm, that's not really my understanding, but maybe I'm not historically informed. Which experiments have searched for dark matter through heating, rather than through the identification of individual recoil a la CDMS, XENON, etc.? The only one I am aware of is the XQC sounding rocket experiment as analyzed by Steinhartd and collaborators, and that wasn't even designed to search for dark matter. –  Jess Riedel Jun 4 '14 at 17:18
I'm with @JessRiedel on this. Direct dark matter experiments detect energy depositions, but they detect in much more distinctive modes than "heat" suggests. –  dmckee Jun 6 '14 at 15:16
To clarify for those interested: recoil and heating detection are conceptually two distinct regimes. In recoil experiments like XENON that look for heavy DM, you must identify the individual recoil; if the energy deposited by the collision is allowed to thermalize with the rest of the xenon container (which must be large to make collisions reasonably frequent), the temperature increase would be undetectably small. –  Jess Riedel Jun 7 '14 at 15:40
On the other hand, for small DM masses the event rate is much higher (allowing small target volumes) but the recoil energy is below the typical thermal energy of the target. Thus, individual recoils cannot be identified, but a statistically significant increase in total energy from many collisions can be measured. See –  Jess Riedel Jun 7 '14 at 15:41

protected by Qmechanic Feb 27 '13 at 17:06

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