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  Cosmic Crashes Forging Gold

Cosmic Crashes Forging Gold

The cosmic site where the heaviest chemical elements such as lead or gold are formed is likely to be identified: Ejected matter from neutron stars merging in a violent collision provides ideal conditions. In detailed numerical simulations, scientists of the Max Planck Institute for Astrophysics (MPA) and affiliated to the Excellence Cluster Universe and of the Free University of Brussels (ULB) have verified that the relevant reactions of atomic nuclei do take place in this environment, producing the heaviest elements in the correct abundances.

Fig. 1: Where did gold form? For a long time, the cosmic production site of this rare metal and of other very heavy chemical elements has been unknown. New theoretical models now confirm that it could be forged in the merger events of two neutron stars.
Image: Natural gold nuggets from California and Australia; Natural History Museum, London

 

Fig. 2: Various stages of the merger of two neutron stars; the sequence of images covers a period of about one hundredths of a second. Once the stars collide material is squeezed out between the stars and gets stripped off from tidal tails. In the material ejected a multitude of nuclear reactions take place producing heavy elements.

 

Fig. 3: The stable neutron-rich elements synthesized in the merger event are produced by a complicated sequence of reactions, starting form neutron captures and beta-decays onto light "seed" nuclei, and so producing heavier and heavier neutron-rich nuclei. When reaching the heaviest neutron- rich nuclei, fission reactions recycle the material towards lighter ones. These nuclear processes takes place forabout a second - as long as neutrons are available. Finally when all neutrons are captured, the nuclei decay back to stable nuclei. The principle reaction chains are shown here, where the colour coding indicates the abundance of the elements. The whole evolution is shown in this movie: linkPfeil.gifdivx (2.7 MB) or linkPfeil.gifmp4 (1MB).

Most heavy chemical elements are formed in nuclear fusion reactions in stars. Also in the centre of our Sun, hydrogen is ”burned“ to create helium, thereby releasing energy. Heavier elements are then produced from helium if the star is more massive than our Sun. This process, however, only works up to iron; further fusion reactions do not yield any net energy gain. Therefore heavier elements cannot be produced in this fashion. Instead, they can be assembled when neutrons are captured onto ”seed“-nuclei, which then decay radioactively.

This involves two main processes: the slow neutron capture (s-process), which takes place at low neutron densities inside stars during their late evolution stages, and the rapid neutron capture (r-process), which needs very high neutron densities. Physicists know that the r-process is responsible for producing a large fraction of the elements much heavier than iron (those with nuclear mass numbers A>80), including platinum, gold, thorium, and uranium (Fig. 1). However, the question of which astrophysical objects can accommodate for this r-process remains to be answered.

”The source of about half of the heaviest elements in the Universe has been a mystery for a long time,“ says Hans-Thomas Janka, senior scientist at the Max Planck Institute for Astrophysics (MPA) and within the Excellence Cluster Universe. ”The most popular idea has been, and may still be, that they originate from supernova explosions that end the lives of massive stars. But newer models do not support this idea.“

Violent mergers of neutron stars in binary systems (see note 1) offer an alternative scenario, when the two stars collide after millions of years of spiralling towards each other. For the first time, scientists at the MPA and the ULB have now simulated all stages of the processes occurring in such mergers by detailed computer models (Fig. 2). This includes both the evolution of the neutron star matter during the relativistic cosmic crashes and the formation of chemical elements in the tiny fraction of the whole matter that gets ejected during such events, involving the nuclear reactions of more than 5000 atomic nuclei (chemical elements and their isotopes (see note 2)).

”In just a few split seconds after the merger of the two neutron stars, tidal and pressure forces eject extremely hot matter equivalent to several Jupiter masses,“ explains Andreas Bauswein, who carried out the simulations at the MPA. Once this so-called plasma has cooled to less than 10 billion degrees, a multitude of nuclear reactions take place, including radioactive decays, and enable the production of heavy elements. ”The heavy elements are `recycled' several times in various reaction chains involving the fission of super-heavy nuclei, which makes the final abundance distribution become largely insensitive to the initial conditions provided by the merger model,“ adds Stephane Goriely, ULB researcher and nuclear astrophysics expert of the team (see also Fig. 3). This agrees well with previous speculations that the reaction properties of the atomic nuclei involved should be the decisive determining factor because this is the most natural explanation for the essentially identical abundance distributions of the heaviest r-process elements observed in many old stars and in our solar system.

The simulations showed that the abundance distribution of the heaviest elements (with mass numbers A>140) agrees very well with the one observed in our solar system. If one combines the results of the simulations and the estimated number of neutron star collisions in the Milky Way in the past, the figures indicate that such events could in fact be the main sources of the heaviest chemical elements in the Universe.

The team plans now to conduct new studies to further improve the theoretical predictions by refined computer simulations that can follow the physical processes in even more detail. On the other hand, observational astronomers look out for detecting the transient celestial sources that should be associated with the ejection of radioactive matter in neutron star mergers. Because of the heating by radioactive decays, the ejecta will shine up with almost the brightness of a supernova explosion — albeit only for a few days. A discovery would mean the first observational hint of freshly produced r-process elements in the source of their origin. The hunt is on!

Notes:

  1. Neutron stars are extremely compact remnants of stars, forming when a massive star reaches the end of its lifetime. The stellar core collapses while the outer layers are ejected in a supernova explosion. The neutron star at the centre has about one and a half times the mass of our Sun, but a diameter of only 20—30 kilometres. Sometimes in a binary star system two neutron stars form by two supernova explosions and then orbit each other. Due to energy loss, the two stars will eventually merge. These events, however, should be rare. Astronomers estimate that the merging of two neutron stars should occur about once every 100 000 years in a galaxy like the Milky Way.
  2. Isotopes are atoms with the same number of protons in their nucleus but different numbers of neutrons.

Original publication:

Stephane Goriely, Andreas Bauswein and Hans-Thomas Janka, "r-process nucleosynthesis in dynamically ejected matter of neutron star mergers", 2011 ApJ 738 L32 linkPfeilExtern.gifhttp://iopscience.iop.org/2041-8205/738/2/L32


Contact:

Dr. Hans-Thomas Janka
Max Planck Institute for Astrophysics, Garching
Tel.: +49 89 30000-2228
email: hjankampa-garching.mpg.de

Dr. Andreas Bauswein
Max Planck Institute for Astrophysics, Garching
Tel.: +49 89 30000-2236
email: abausweinmpa-garching.mpg.de

Dr. Hannelore Hämmerle
Press Officer
Max Planck Institute for Astrophysics, Garching
Tel. +49 89 30000-3980
E-mail: hhaemmerlempa-garching.mpg.de


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last modified: 2011-9-20