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Published June 14, 2023 | Version 0.0.1
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NMMA Kilonova Lightcurve Grids

Authors/Creators

  • 1. Nikhef, Science Park 105, 1098 XG Amsterdam, The Netherlands
  • 2. Institut fur Physik und Astronomie, Universitat Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, 14476, Potsdam, Germany
  • 3. School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
  • 4. The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden
  • 5. Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
  • 6. Department of Physics, American University of Sharjah, PO Box 26666, Sharjah, UAE
  • 7. 9 Laboratoire de Physique et de Chimie de l'Environnement, Universite Joseph KI-ZERBO, Ouagadougou, Burkinka Faso
  • 8. Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
  • 9. Artemis, Universite C´ ote d'Azur, Observatoire C ˆ ote d'Azur, CNRS, CS 34229, F-06304 Nice Cedex 4, France
  • 10. Department of Physics, Massachusetts Institute of Technology, 77 Massachusetts Ave, Cambridge, MA 02139, USA
  • 11. Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Muhlenberg 1, Potsdam 14476, Germany
  • 12. Department of Physics, Deshbandhu College, University of Delhi, New Delhi, India
  • 13. Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, F-69622, Villeurbanne, France

Description

The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the NMMA (Nuclear-physics and Multi-Messenger Astrophysics) framework. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. It also enables us to classify electromagnetic observations, e.g., to distinguish between supernovae and kilonovae. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions. The extension of the NMMA code presented here is the first attempt of analysing the gravitational-wave signal, the kilonovae, and the GRB afterglow simultaneously, which reduces the uncertainty of our constraints. Incorporating all available information, we estimate the radius of a 1.4 solar mass neutron star to be R=11.98+0.35−0.40 km.

Notes

These models have been generated using NMMA, which paper is accessible here on the arxiv: https://arxiv.org/abs/2205.08513

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