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Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars

Naturevolume 340pages126128 (1989) | Download Citation

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Abstract

NEUTRON-STAR collisions occur inevitably when binary neutron stars spiral into each other as a result of damping of gravitational radiation. Such collisions will produce a characteristic burst of gravitational radiation, which may be the most promising source of a detectable signal for proposed gravity-wave detectors1. Such signals are sufficiently unique and robust for them to have been proposed as a means of determining the Hubble constant2. However, the rate of these neutron-star collisions is highly uncertain3. Here we note that such events should also synthesize neutron-rich heavy elements, thought to be formed by rapid neutron capture (the r-process)4. Furthermore, these collisions should produce neutrino bursts5 and resultant bursts of γ-rays; the latter should comprise a subclass of observable γ-ray bursts. We argue that observed r-process abundances and γ-ray-burst rates predict rates for these collisions that are both significant and consistent with other estimates.

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Author information

Affiliations

  1. Department of Physics, Ben Gurion University, Beer Sheva, Israel

    • David Eichler
  2. Astronomy Program, University of Maryland, College Park, Maryland, 20742, USA

    • David Eichler
  3. Department of Physics, The Technion, Haifa, Israel

    • Mario Livio
  4. Racah Institute for Physics, Hebrew University, Jerusalem, Israel

    • Tsvi Piran
  5. Princeton University Observatory, Princeton, New Jersey, 08544, USA

    • Tsvi Piran
  6. Departments of Physics and Astrophysics, University of Chicago, 5640 Ellis Avenue, Chicago, Illinois, 60637, USA

    • David N. Schramm
  7. NASA/Fermilab Astrophysics Center, Batavia, Illinois, 60510, USA

    • David N. Schramm

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https://doi.org/10.1038/340126a0

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