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Axisymmetric Radiative Transfer Models of Kilonovae

Oleg KorobkinCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]Ryan WollaegerCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]Chris L. FryerCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USAAimee HungerfordCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]Stephan RosswogDepartment of Astronomy, Stockholm University, AlbaNova, Stockholm SE-106 91, SwedenChristopher J. FontesCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]M. R. MumpowerCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]E. A. ChaseCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60201, USAWesley EvenDepartment of Physical Science, Southern Utah University, Cedar City, UT 84720, USAJonah MillerCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]G. W. MischCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]Jonas LippunerCenter for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM 87545, USA; [email protected]

2021en

ABI

Annotatsiya

Abstract The detailed observations of GW170817 proved for the first time directly that neutron star mergers are a major production site of heavy elements. The observations could be fit by a number of simulations that qualitatively agree, but can quantitatively differ (e.g., in total r-process mass) by an order of magnitude. We categorize kilonova ejecta into several typical morphologies motivated by numerical simulations, and apply a radiative transfer Monte Carlo code to study how the geometric distribution of the ejecta shapes the emitted radiation. We find major impacts on both spectra and light curves. The peak bolometric luminosity can vary by two orders of magnitude and the timing of its peak by a factor of five. These findings provide the crucial implication that the ejecta masses inferred from observations around the peak brightness are uncertain by at least an order of magnitude. Mixed two-component models with lanthanide-rich ejecta are particularly sensitive to geometric distribution. A subset of mixed models shows very strong viewing angle dependence due to lanthanide “curtaining,” which persists even if the relative mass of lanthanide-rich component is small. The angular dependence is weak in the rest of our models, but different geometric combinations of the two components lead to a highly diverse set of light curves. We identify geometry-dependent P Cygni features in late spectra that directly map out strong lines in the simulated opacity of neodymium, which can help to constrain the ejecta geometry and to directly probe the r-process abundances.

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DOI: 10.3847/1538-4357/abe1b5

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