TY  - JOUR
A1  - Dudi, Reetika
A1  - Adhikari, Ananya
A1  - Brügmann, Bernd
A1  - Dietrich, Tim
A1  - Hayashi, Kota
A1  - Kawaguchi, Kyohei
A1  - Kiuchi, Kenta
A1  - Kyutoku, Koutarou
A1  - Shibata, Masaru
A1  - Tichy, Wolfgang
T1  - Investigating GW190425 with numerical-relativity simulations
JF  - Physical review : D, Particles, fields, gravitation, and cosmology
N2  - The third observing run of the LIGO-Virgo Collaboration has resulted in many gravitational wave detections, including the binary neutron star merger GW190425. However, none of these events have been accompanied with an electromagnetic transient found during extensive follow-up searches. In this article, we perform new numerical-relativity simulations of binary neutron star and black hole-neutron star systems that have a chirp mass consistent with GW190425. Assuming that the GW190425's sky location was covered with sufficient accuracy during the electromagnetic follow-up searches, we investigate whether the nondetection of the kilonova is compatible with the source parameters estimated through the gravitational -wave analysis and how one can use this information to place constraints on the properties of the system. Our simulations suggest that GW190425 is incompatible with an unequal mass binary neutron star merger with a mass ratio q < 0.8 when considering stiff or moderately stiff equations of state if the binary was face on and covered by the observation. Our analysis shows that a detailed observational result for kilonovae will be useful to constrain the mass ratio of binary neutron stars in future events.
Y1  - 2022
U6  - https://doi.org/10.1103/PhysRevD.106.084039
SN  - 2470-0010
SN  - 2470-0029
VL  - 106
IS  - 8
PB  - American Physical Society
CY  - College Park
ER  - 
TY  - JOUR
A1  - Dudi, Reetika
A1  - Dietrich, Tim
A1  - Rashti, Alireza
A1  - Brügmann, Bernd
A1  - Steinhoff, Jan
A1  - Tichy, Wolfgang
T1  - High-accuracy simulations of highly spinning binary neutron star systems
JF  - Physical review : D, Particles, fields, gravitation, and cosmology
N2  - With an increasing number of expected gravitational-wave detections of binary neutron star mergers, it is essential that gravitational-wave models employed for the analysis of observational data are able to describe generic compact binary systems. This includes systems in which the individual neutron stars are millisecond pulsars for which spin effects become essential. In this work, we perform numerical-relativity simulations of binary neutron stars with aligned and antialigned spins within a range of dimensionless spins of chi similar to [-0.28, 0.58]. The simulations are performed with multiple resolutions, show a clear convergence order and, consequently, can be used to test existing waveform approximants. We find that for very high spins gravitational-wave models that have been employed for the interpretation of GW170817 and GW190425 arc not capable of describing our numerical-relativity dataset. We verify through a full parameter estimation study in which clear biases in the estimate of the tidal deformability and effective spin are present. We hope that in preparation of the next gravitational-wave observing run of the Advanced LIGO and Advanced Virgo detectors our new set of numerical-relativity data can be used to support future developments of new gravitational-wave models.
Y1  - 2022
U6  - https://doi.org/10.1103/PhysRevD.105.064050
SN  - 2470-0010
SN  - 2470-0029
VL  - 105
IS  - 6
PB  - American Physical Society
CY  - College Park
ER  -