Is it possible to test the sonofusion with the deuterium-tritium reaction?

The research on sonofusion tries to obtain nuclear fusion in deuterated liquids. In a typical experiment of sonofusion, a beam of neutrons generates tiny bubbles in the liquid. An ultrasound field expands and contracts these bubbles. The nuclear fusion could occur when the collapse of bubbles is sufficiently fast to generate an intense shock wave. The last experiment of Rusi Taleyarkhan and his team has demonstrated the emission of neutrons in deuterated acetone.

With deuterated products, the possible reactions are:
D + D > He3 + n
D + D > T + H

These reactions are not easy whereas the reaction between deuterium and tritium is the easier reaction of nuclear fusion:
D + T > He4 + n

If we could test the sonofusion with a mix of deuterium and tritium, the signs of fusion could be more evident. But the use of tritium is very expensive because it doesn’t exist in nature. It must be generated by a nuclear reaction:
Li6 + n > He4 + T

So the test of sonofusion with the DT reaction obliges the use of a very small amount of tritium.

A mean to limit the amount of tritium in a sonofusion experiment could be the use of tritiated tensioactive molecules.

These molecules, dissolved in heavy water, could be like for example CH3-(CH2)n-phenyl-SO3 Na (alkyl-phenyl-sulfonate) where one or several hydrogen atoms are replaced by tritium atoms.

When this sort of solution is exposed in sonofusion experiment, the neutron beam generates bubbles. These bubbles grow during the depressive phase of the sonic wave.

What could be the comportment of tensioactive molecules? I propose two hypothesis:
- the tensioactive molecule that encounters the surface of the bubble remains glued on this surface by its apolar part,
- when the compressive phase of sonic wave occurs, the bubble surface drags the tensioactive molecules.

By this way, a mix of deuterated water molecules and tritiated tensioactive molecules could be concentrated on the top of the shock wave in final collapse of bubble.

If this scheme works, it could be possible to study the sonofusion of deuterium and tritium in heavy water.

The synthesis of tritiated molecules is a standard technique, particularly for the biological research. Used as a radioactive marker, the tritium permits the study of chemical or biological reactions.

A very small amount of tritium seems to me sufficient to start D-T reactions. Some calculations and hypothesis suggest that sonofusion with tritium could be tested with a solution of heavy water containing less than 100 micromoles of tritium per liter.

These last years, the search for extrasolar planets has been successful. To date, the astronomers have detected more than 400 extrasolar planets. Among these 300 planets, only ten have been discovered by their own light.

There is perhaps a phenomenon which could facilitate this search for extrasolar planets.

The astronomer Michael Mumma and his team have discovered in 1981 (*) a natural laser emission produced by the Martian upper atmosphere. This very fine emission ray centered on 10,33 µm is due to carbon dioxide, majority component of the Martian atmosphere. This natural laser emission has been not only confirmed by other teams but another natural laser has been discovered in the Venusian upper atmosphere.

In consequence of these discoveries, one can suppose that this phenomenon of stimulated emission generated by a planetary atmosphere is frequent.

This phenomenon of stimulated emission could be used for the search for extrasolar planets. The direct detection of an extrasolar planet conflicts, with current technology, with a considerable obstacle: the difference of brightness between planet and its star companion. If the studied planet has an atmosphere and if this one presents a stimulated emission, the brightness of planet in the emission ray could be amplified considerably. To benefit from this emission, it would be necessary to detect very thin rays. With this condition, the ratio of brightness between star and planet could become more favorable for a direct detection.

A first step in the use of this phenomenon could be the checking of its presence on the extrasolar planets already discovered.

Several ray masers would deserve a detailed attention: the ray at 23.7 GHz emitted by molecule NH3 and the rays at 22 GHz and 1.66 GHz emitted by molecule H2O and radical OH. As the stars emit little in this part of electromagnetic spectrum, one can hope for a ratio of brightness more favorable for the planet detection. The ray maser of ammonia could be a good marker for gas giant planets. The masers of water and radical hydroxyl would be good indices for planets similar to Earth.

(*): “Discovery of Natural Gain Amplification in the 10-Micrometer Carbon Dioxide Laser Bands one Mars: A Natural Laser”; MICHAEL J MUMMA, DAVID BUHL, GORDON CHIN, DRAKE DEMING, FRED ESPENAK, THEODOR KOSTIUK, and DAVID ZIPOY; Science, 3 April 1981, Vol. 212, No 4490, pp. 45  – 49.