Constraints on Cosmic-ray Acceleration Efficiency in Balmer Shocks of Two Young Type Ia Supernova Remnants in the Large Magellanic Cloud

Hovey, Luke; Hughes, John P.; McCully, Curtis; Pandya, Viraj; Eriksen, Kristoffer

doi:10.3847/1538-4357/aac94b

Constraints on Cosmic-ray Acceleration Efficiency in Balmer Shocks of Two Young Type Ia Supernova Remnants in the Large Magellanic Cloud

Journal Article · Wed Aug 01 00:00:00 EDT 2018 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/aac94b· OSTI ID:1469544

Hovey, Luke ^[1]; ^[2]; ^[3]; ^[4]; Eriksen, Kristoffer ^[1]

Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Rutgers Univ., Piscataway, NJ (United States). Dept. of Physics and Astronomy; Flatiron Inst., New York, NY (United States). Center for Computational Astrophysics
Las Cumbres Observatory, Goleta, CA (United States); Univ. of California, Santa Barbara, CA (United States). Dept. of Physics,
Univ. of California, Santa Cruz, CA (United States). UCO/Lick Observatory, Dept. of Astronomy and Astrophysics

We present results from an optical study of two young Balmer-dominated remnants of SNIa in the Large Magellanic Cloud, 0509-67.5 and 0519-69.0, in an attempt to search for signatures of efficient cosmic-ray (CR) acceleration. Here, we combine proper motion measurements with corresponding optical spectroscopic measurements of the Hα line at multiple rim positions from VLT/FORS2 and SALT/RSS and compare our results to published Balmer shock models. Analyses of the optical spectra result in broad Hα widths in the range of 1800–4000 km s^-1 for 12 separate Balmer-dominated filaments that show no evidence for forbidden line emission; the corresponding shock speeds from proper motion measurements from HST span a range of 1700–8500 km s^-1. Our measured values of shock speeds and broad Hα widths in 0509-67.5 and 0519-69.0 are fit well with a Balmer shock model that does not include effects of efficient CR acceleration. We determine an upper limit of 7%/χ (95% confidence) on the CR acceleration efficiency for our ensemble of data points, where χ is the ionization fraction of the pre-shock gas. The upper limits on the individual remnants are 6%/χ (0509-67.5) and 11%/χ (0519-69.0). Finally, these upper limits are below the integrated CR acceleration efficiency in the Tycho supernova remnant, where the shocks predominantly show little Hα emission, indicating that Balmer-dominated shocks are not efficient CR accelerators.

View Accepted Manuscript (DOE)

Research Organization:: Los Alamos National Laboratory (LANL)

Sponsoring Organization:: National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); USDOE

Grant/Contract Number:: AC52-06NA25396

OSTI ID:: 1469544

Report Number(s):: LA-UR-17-28677

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 2 Vol. 862; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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