@article{GiegSchianchiDietrichetal.2022,
  author    = {Gieg, Henrique and Schianchi, Federico and Dietrich, Tim and Ujevic, Maximiliano},
  title     = {Incorporating a Radiative Hydrodynamics Scheme in the Numerical-Relativity Code BAM},
  series = {Universe : open access journal},
  volume    = {8},
  journal   = {Universe : open access journal},
  number    = {7},
  publisher = {MDPI},
  address   = {Basel},
  issn      = {2218-1997},
  doi       = {10.3390/universe8070370},
  pages     = {25},
  year      = {2022},
  abstract  = {To study binary neutron star systems and to interpret observational data such as gravitational-wave and kilonova signals, one needs an accurate description of the processes that take place during the final stages of the coalescence, for example, through numerical-relativity simulations. In this work, we present an updated version of the numerical-relativity code BAM in order to incorporate nuclear-theory-based equations of state and a simple description of neutrino interactions through a neutrino leakage scheme. Different test simulations, for stars undergoing a neutrino-induced gravitational collapse and for binary neutron stars systems, validate our new implementation. For the binary neutron stars systems, we show that we can evolve stably and accurately distinct microphysical models employing the different equations of state: SFHo, DD2, and the hyperonic BHB Lambda phi. Overall, our test simulations have good agreement with those reported in the literature.},
  language  = {en}
}
@article{UjevicRashtiGiegetal.2022,
  author    = {Ujevic, Maximiliano and Rashti, Alireza and Gieg, Henrique Leonhard and Tichy, Wolfgang and Dietrich, Tim},
  title     = {High-accuracy high-mass-ratio simulations for binary neutron stars and their comparison to existing waveform models},
  series = {Physical review : D, Particles, fields, gravitation, and cosmology},
  volume    = {106},
  journal   = {Physical review : D, Particles, fields, gravitation, and cosmology},
  number    = {2},
  publisher = {American Physical Society},
  address   = {College Park},
  issn      = {2470-0010},
  doi       = {10.1103/PhysRevD.106.023029},
  pages     = {10},
  year      = {2022},
  abstract  = {The subsequent observing runs of the advanced gravitational-wave detector network will likely provide us with various gravitational-wave observations of binary neutron star systems. For an accurate interpretation of these detections, we need reliable gravitational-wave models. To test and to point out how existing models could be improved, we perform a set of high-resolution numerical relativity simulations for four different physical setups with mass ratios q = 1.25, 1.50, 1.75, 2.00, and total gravitational mass M = 2.7 M???. Each configuration is simulated with five different resolutions to allow a proper error assessment. Overall, we find approximately second-order converging results for the dominant (2,2) mode, but also the subdominant (2,1), (3,3), and (4,4) modes, while generally, the convergence order reduces slightly for an increasing mass ratio. Our simulations allow us to validate waveform models, where we find generally good agreement between state-of-the-art models and our data, and to prove that scaling relations for higher modes currently employed for binary black hole waveform modeling also apply for the tidal contribution. Finally, we also test if the current NRTidal model used to describe tidal effects is a valid description for high-mass-ratio systems. We hope that our simulation results can be used to further improve and test waveform models in preparation for the next observing runs.},
  language  = {en}
}