Bulletin of the American Physical Society
APS April Meeting 2021
Volume 66, Number 5
Saturday–Tuesday, April 17–20, 2021; Virtual; Time Zone: Central Daylight Time, USA
Session S03: Atomic Physics and Kilonova EmissionInvited Live
|
Hide Abstracts |
Sponsoring Units: DAP DAMOP Chair: Chris Fontes, Los Alamos National Laboratory |
Monday, April 19, 2021 1:30PM - 2:06PM Live |
S03.00001: Advances in atomic theory of heavy elements for neutron star merges Invited Speaker: Marianna Safronova Lanthanides and actinides play an important role in understanding of neutron star merger events. Calculating opacities for these heavy elements is a challenging task. Reliable benchmarks for atomic transition properties are urgently needed. I will report on recent advances in first-principle atomic theory of lanthanides and actinides and development of online portal for high-precision atomic data for needs of atomic, astrophysics, and plasma physics communities. [Preview Abstract] |
Monday, April 19, 2021 2:06PM - 2:42PM Live |
S03.00002: Mass ejection in neutron star mergers: connecting merger simulations to nucleosynthesis and kilonova observations Invited Speaker: Francois Foucart Determining the properties of the mildly relativistic outflows produced during and after the merger of neutron star binaries is crucial to understand the role of neutron star mergers in the production of heavy elements, as well as to analyze multi-messenger observations of these systems. The mass and composition of these outflows determine how much matter is available for r-process nucleosynthesis, as well as the relative abundance of the various elements produced by the r-process. Additionally, the properties of these matter outflows are tightly linked to the observable characteristics of kilonovae, the optical/infrared signals powered by radioactive decays of the ashes of the r-process. A good understanding of merger outflows allows us to constrain the role of merger in nucleosynthesis, and improves our ability to gather information about the properties of the merging objects from kilonova observations. To model merger outflows, we currently rely on numerical simulations of neutron star mergers and of their post-merger remnants. In this talk, I will review what simulations have taught us so far about neutron star merger outflows, and discuss both their recent successes and the impact of their remaining limitations on our ability to reliably model neutron star merger outflows. [Preview Abstract] |
Monday, April 19, 2021 2:42PM - 3:18PM Live |
S03.00003: Modeling Kilonova Light-Curves Invited Speaker: Ryan Wollaeger Kilonovae are the transient electromagnetic emission powered by radioactive decay of elements synthesized following the merger of two neutron stars or a neutron star and black hole. A kilonova was observed definitively for the first time in August 2017, as a counterpart to gravitational waves detected by LIGO and Virgo, GW170817. Efforts to numerically synthesize the light curves and spectra for merger and ejecta models have since expanded into parameter studies of the impact of uncertainties in composition, morphology, nucleosynthesis and decay, and remnant sources. In this talk, we provide an overview of these efforts, and in particular discuss a broad grid of multidimensional kilonova models we have generated with the Monte Carlo radiative transfer code SuperNu. This grid covers a large space of mass and velocity identified in the literature, and has proven useful in constraining recent observations GW190814 and GRB 160624A. [Preview Abstract] |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700