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Title: Californium-254 and Kilonova Light Curves

Journal Article · · The Astrophysical Journal. Letters (Online)
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]; ORCiD logo [3]; ORCiD logo [5]; ORCiD logo [5]; ORCiD logo [6]; ORCiD logo [5]; ORCiD logo [2]; ORCiD logo [2]; ORCiD logo [7]; ORCiD logo [5]; ORCiD logo [8]; ORCiD logo [5]; ORCiD logo [9]
  1. Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Chemistry
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
  3. Univ. of Notre Dame, IN (United States)
  4. Univ. of Notre Dame, IN (United States); Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States). Center for the Evolution of the Elements (JINA-CEE)
  5. Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States). Center for the Evolution of the Elements (JINA-CEE)
  6. Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States). Center for the Evolution of the Elements (JINA-CEE); Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Chemistry
  7. Univ. of Notre Dame, IN (United States). Dept. of Civil Engineering and Geological Sciences; Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States). Center for the Evolution of the Elements (JINA-CEE)
  8. Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Joint Inst. for Nuclear Astrophysics (JINA), East Lansing, MI (United States). Center for the Evolution of the Elements (JINA-CEE); Southern Utah Univ., Cedar City, UT (United States)
  9. Columbia Univ., New York, NY (United States). Columbia Astrophysics Lab.

Neutron star mergers o er unique conditions for the creation of the heavy elements and additionally provide a testbed for our understanding of this synthesis known as the r-process. We have performed dynamical nucleosynthesis calculations and identi ed a single isotope, 254Cf, which has a particularly high impact on the brightness of electromagnetic transients associated with mergers on the order of 15 to 250 days. This is due to the anomalously long half-life of this isotope and the e ciency of ssion thermalization compared to other nuclear channels. We estimate the ssion fragment yield of this nucleus and outline the astrophysical conditions under which 254Cf has the greatest impact to the light curve. Future observations in the middle-IR which are bright during this regime could indicate the production of actinide nucleosynthesis.

Research Organization:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Organization:
USDOE
Grant/Contract Number:
89233218CNA000001
OSTI ID:
1484657
Report Number(s):
LA-UR--18-25559
Journal Information:
The Astrophysical Journal. Letters (Online), Journal Name: The Astrophysical Journal. Letters (Online) Journal Issue: 2 Vol. 863; ISSN 2041-8213
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English

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Physical Conditions for the r -process. I. Radioactive Energy Sources of Kilonovae journal November 2018
β -delayed Fission in r -process Nucleosynthesis journal December 2018
Actinide Production in the Neutron-rich Ejecta of a Neutron Star Merger journal December 2018
Neutron Star Mergers Might Not Be the Only Source of r -process Elements in the Milky Way journal April 2019
Probing the Production of Actinides under Different r-process Conditions journal July 2019
Finding the Remnants of the Milky Way's Last Neutron Star Mergers journal July 2019
Actinide-rich and Actinide-poor r -process-enhanced Metal-poor Stars Do Not Require Separate r -process Progenitors journal August 2019
Physical conditions for the r-process I. radioactive energy sources of kilonovae text January 2018
Actinide-rich and Actinide-poor $r$-Process Enhanced Metal-Poor Stars do not Require Separate $r$-Process Progenitors text January 2019