NEUTRON-STAR IMPLOSIONS

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The lightest of the chemical elements—hydrogen, helium, and lithium—were created in the hot, early phase of the Universe, about a minute after the big bang. Heavier elements were forged later—in the nuclear fires of many generations of stars and during supernova explosions. But the origin of many rare chemical species, particularly the heaviest elements, remains uncertain. In particular, recent observations of a nearby galaxy enriched with heavy elements challenge traditional nucleosynthesis models. George Fuller of the University of California, San Diego, and colleagues now propose a novel scenario for the origin of the heaviest elements, including gold, platinum, and uranium. Their hypothesis involves tiny black holes inducing neutron-star implosions and, if viable, would in one fell swoop offer solutions to other astrophysical riddles beyond heavy element synthesis.

Elements heavier than iron can be assembled only from lighter “seed” nuclei that capture free neutrons or protons. Neutron capture occurs through either a “slow” s process or a “rapid” r process. In both cases, the neutron-rich nucleus undergoes beta decay, converting neutrons to protons and advancing to higher atomic numbers. The s process can proceed at the modest neutron densities available in the outer shells of evolving stars. By contrast, the r process requires 10 billion times greater neutron densities (above 10exp1cmexp3) in order that neutron captures occur much faster than beta decay. The r process is responsible for gold, platinum, most of the lanthanides, and all of the natural actinides. The heaviest r-process nuclei—up to and beyond an atomic mass number of 240—occur through the “strong” r process, in which an iron seed captures 100 or more neutrons.

The strong r process requires a high neutron density and some combination of a large excess of neutrons over protons, very high temperatures, and rapid expansion. Such extremes are expected in supernovae—but only in rare cases—and in mergers between two neutron stars or between a neutron star and a black hole. These compact binary mergers are estimated to be 1000 times less frequent than supernovae, but they can expel considerably larger amounts of neutron-rich matter—a low-rate/high-yield scenario that’s consistent with the rarity of plutonium-244 in the early Solar System and in deep-sea reservoirs on Earth.

A wrinkle in this picture is a nearby low-luminosity dwarf galaxy known as Reticulum II, whose stars are highly enriched with strong-r-process nuclei. Reticulum II is the only dwarf galaxy (out of ten) with a significant “excess” of heavy nuclei, which suggests the nuclei were produced by an infrequent event, but perhaps one not so rare as a compact-object merger. Fuller and co-workers therefore envision an alternative scenario in which r-process nuclei are generated in the ejected matter of a very rapidly spinning neutron star, or “millisecond pulsar,” as it implodes to form a black hole.

The researchers imagine that the trigger for this catastrophic collapse is a primordial black hole (PBH). Hypothetical relics from the early Universe, PBHs can have the mass of an asteroid packed into an atom-sized space and collectively they are one of several candidates for dark matter. PBHs would roam dwarf galaxies and the center of our Milky Way with a relatively high abundance, so they would collide with neutron stars at a higher rate than that of compact-object mergers. When a PBH is captured by a neutron star, it sinks towards the center and swallows the star from the inside. Then, as the growing black hole sucks in neutron-star matter, viscous shearing and magnetic fields carry angular momentum to the star’s outer layers along its equator. Fuller et al. argue that these mechanisms rip off dense nuclear matter in which the strong r process can develop (Fig.).

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