An exploding cloud of chondrule-forming silicate vapour could have arisen from one of two processes: rapid de-compression following the shock of two rocky planets colliding, or rapid heating of a single rocky planet by thermonuclear reactions.
Within the conventional multimillion-year timescale, the scenario is a sea of rocky planetesimals slugging it out in repeated impacts until a few attained planet size and the debris of smaller fragments accreted to the survivors. Iron meteorites demonstrate that bodies of at least dwarf planet size existed already by 4565 Ma. The larger the planetesimals, the fewer there were and the less likely they were to collide. An impact scenario commends itself only by default, because the heat from radioactivity, though greater than now (because there was more radioactive matter and the half-lives of now extinct radioisotopes were very short), would not have been high enough to cause whole planets to disintegrate.
But suppose that rates of radioactivity were higher. If radioisotopes within a planet produced more heat than could have been conducted upward and radiated away, thermal expansion would have ruptured the outer part and upsurging magma flooded the surface. This may have been what happened. The oldest rocks of every extant terrestrial planet are igneous. Mercury, Venus and Mars were blanketed with magma to a depth of several kilometers. The only reason this did not happen on Earth is that the lithosphere was buffered from the melting interior by a subterranean ocean. Nonetheless, after the Deluge magmatism was large-scale.
Mercury is now the smallest terrestrial planet, but its disproportionately massive core – three quarters of its total mass – indicates that at some early stage it shed part of its mantle. Mercury gives us a clue as to why some planets exploded and others did not. It underwent incomplete disruption because it was intermediate in size: bigger than Earth but smaller than the planets that disintegrated completely. At that point Mercury was only partially differentiated. Most of the iron that would later have melted and sank to the centre was still in its proto-mantle and lost when most of the mantle was lost. The iron-rich remnant of a body then continued to differentiate towards its present proportions.
At this point we need to delve more fundamentally into the origin of isotopes. Some were so short-lived that they could have come into being only shortly before the chondrules and CAIs in which they were trapped. One of these was the radioisotope calcium-41. We know of its existence because meteorites contain measurable amounts of its stable decay product, potassium-41. The half-life of a radioactive element (radioisotope) is the time taken for half of it to decay into another element, in this case 99,400 years in present-day terms. After 10 half-lives all but 0.1% will have decayed, and if the quantity is small to begin with, the remaining amount will be immeasurable. (For comparison, uranium-238, with a current half-life of 4.47 billion years, is barely radioactive.) The former presence of 41Ca in the oldest meteorites means that the isotope cannot have come into being much before a million years earlier. Given that the universe is close to 14 billion years old in radiometric time, a creation origin for the 41Ca can be ruled out. Longer-lived isotopes also must have had a natural origin, since whether a radioisotope was short-lived or long-lived was just a matter of degree.
The usual explanation for the presence of radioisotopes in the solar system is that they were synthesised in supernovas. Long-lived isotopes were injected into the nebula long before it collapsed, while the most ephemeral came from a nearby supernova that happened to occur just as the solar system was forming. In either case, the injected isotopes should have been homogeneous, a scenario the data do not support (Krestianinov et al. 2023). Alternatively, since the synthesis of unstable isotopes immediately before year zero is unlikely to have been coincidence, they may have been forged within the planets themselves. Some elements, such as uranium, are radioactive in all their forms, so uranium-238, by far the most stable form, may have existed from the beginning. Although very dense, uranium has a chemical affinity for silicates. Planets initially had a homogeneous distribution, but as they melted, uranium became concentrated in the upper mantle and in the granites of the middle and upper crust.
The energy of stars, including the Sun, comes chiefly from thermonuclear fusion. In their cores, temperatures are high enough to overcome the electrostatic forces that keep atoms apart, and the pressure high enough to fuse the atoms into new elements. In the process, excess binding energy is converted into heat energy. The Sun being a relatively small star, the temperature at its core – around 15 million degrees – is sufficient only to fuse hydrogen. More massive stars can go further and fuse the initial product, helium, into carbon, nitrogen and oxygen. The temperature required here is around 100 million degrees.
Rates of radioactivity are related to the speed of light. The higher the speed, the faster isotopes decay, because a faster speed of light results in lower atomic mass and lower binding energy. The disintegration of atoms by decay and their synthesis by fusion are both controlled by that binding energy. If the speed of light had once been faster, the threshold for nuclear fusion would have been lower, and the temperatures enabling the Sun now to synthesise only helium would also have facilitated the fusion of carbon, nitrogen and oxygen. The present Sun derives about 1% of its energy from the C-N-O cycle. Theoretically its mass is too small for such reactions. However, if carbon already existed in its core as a result of nucleosynthesis when c was higher, the element would have acted as a catalyst.
Elements heavier than fluorine, a volatile, are less abundant in the Sun than in other Sun-like stars (Rampalli et al. 2024). Rather, the ratios are broadly chondritic, as a consequence of swallowing up the debris of exploded planets. Three elements in the atmosphere far exceed chondritic ratios (Lodders 2020): nitrogen (49 times more abundant), carbon (9.7 times) and oxygen (2.2 times) – the very elements that are the product of nuclear fusion in more massive stars, where they occur in approximately the same proportions. Thus there is evidence that significant C-N-O nucleosynthesis did occur in the past and that, since the Sun is too small to have ever reached 100 million degrees, thresholds for thermonuclear fusion were once much lower. Conceivably, heavier elements were synthesised in processes requiring still higher energy levels, but their greater density put them beyond the power of convective currents to dredge them up. However, the Sun’s atmosphere gives no hint of nucleosynthesis beyond oxygen.
With electrostatic forces so much weaker, nucleosynthesis would also have taken place in the planets. The type of reaction would have depended on whether the planet was terrestrial or gaseous. Terrestrial planets presumably already had the full range of stable elements, so a radioactive isotope would have been generated simply by changing the number of neutrons. Aluminium, for instance, is the seventh most abundant element in planets, and turning the natural isotope 27Al into 26Al just required knocking out one neutron; likewise 40Ca, the eighth most abundant, into radioactive 41Ca just required capturing one neutron. As with stars, the thresholds for nuclear reactions would have been proportional to density and mass. It was therefore the most massive rocky planets that exploded.
Chondrules and matrix are complementary in composition. The chondrules of carbonaceous chondrites have low Si/Mg and Fe/Mg ratios, the matrix high ratios, showing that the components had a common source (Palme et al. 2015). The most natural interpretation is that chondrules represent intermediate-depth material that became depleted in silicon as a result of silicon-rich minerals rising towards the surface and became depleted in iron as a result of iron-rich minerals sinking towards the core. Since an impact origin cannot account for variation of this nature, the cause must have been nucleosynthesis (Budde et al. 2016), specifically within a planetary body.
Radionuclides began to be synthesised in the cores of rocky planets almost from the start. The heat they generated accelerated the process faster than the falling speed of light slowed it down, until the consequent rise in pressure caused the mantle to burst. Temperatures rose most rapidly where Al and Ca, including their radioactive forms, were most abundant. At the moment of explosion, the melt vaporised, then cooled into droplets. Pulverised material from the outermost layer coalesced with the droplets while vapour filled the interstices in the newly forming bodies. Shock-heated rock fragments (‘metamorphic clasts’) also entered the mix. The depressurized metal core broke up into bodies of dwarf-planet size.
The explosions were of course violent, but the gravity of the exploding body put a brake on the dispersing debris. Some of the fragments remained in the vicinity, some crashed into other planets, some went into orbit around them. The retention of volatile sodium in the chondrules but not in the higher-temperature CAIs shows that they formed in an environment dense enough to prevent evaporation – denser, moreover, than the supposed nebula (Alexander et al. 2008). Radiogenic heating continued for a time within the new bodies.
Jupiter and Saturn started out as pure hydrogen, like the Sun. They were massive enough to fuse helium but not heavier elements. Jupiter’s temperature at the core is now around 20,000° C, and its composition approximately 75% hydrogen and 24% helium by mass. Saturn, being less massive, and cooler at its core, around 12,000° C, fused a smaller proportion Why the minor elements C, N, S, P, Ar, Kr and Xe are three times the solar abundance (Cavalié et al. 2023) is not well understood; possibly these came from volatile-rich asteroids and comets.
Uranus and Neptune are 15–18% less massive than Saturn and contain a smaller proportion of helium. Estimates of their rock content depend heavily on modelling assumptions. Whether the rock is diffuse or concentrated is also unknown.
One mystery is why Jupiter, Saturn and Neptune should radiate twice as much energy as they receive from the Sun. One suggestion is that the excess heat comes from fusion of deuterium (Fukuhara 2020), though this does not account for Neptune’s high heat flux. A further possibility is that the excess is residual heat from helium fusion no longer occurring. Uranus, being relatively cool, is the odd man out. If a large body crashing into it caused its 98º tilt, some of its deep interior may have been exhumed so that the heat radiated away.
That chondrules originated from mantle silicates that underwent catastrophic heating is no longer controversial, whatever the cause. Chondrites do not represent the primordial material from which asteroids accreted and then differentiated, for differentiated bodies existed already before the formation of chondrules (Sokol et al. 2007). According to many researchers, ‘Chondrules and refractory inclusions are impact-melt objects’ (Sears 2005). ‘Chondrules and metal grains in the CB chondrites formed from a vapour-melt plume produced by a giant impact between planetary embryos’ (Krot et al. 2005). ‘Entire planetesimals were melted internally by the decay of 26Al, and collisions led to the splashing of their liquid contents. Cascades of molten droplets would thereby have been lofted into the nebula where they would have cooled to become chondrules.’ (Sanders & Taylor 2005) In other words, explosions are visualised. CAIs, too, may derive from planetary explosions (Sanders 2009).
