The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas

Plotnikov, Illya; Sironi, Lorenzo

doi:10.1093/mnras/stz640

Title: The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas

Journal Article · Wed Mar 06 00:00:00 EST 2019 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stz640· OSTI ID:1577638

^[1]; Sironi, Lorenzo ^[2]

Princeton Univ., NJ (United States)
Columbia Univ., New York, NY (United States)

The emission process of Fast Radio Bursts (FRBs) remains unknown. We look into whether the synchrotron maser emission from relativistic shocks in a magnetar wind can explain the observed FRB properties. We perform particle-in-cell (PIC) simulations of perpendicular shocks in cold pair plasmas, checking our results for consistency among three PIC codes. We confirm that a linearly polarized X-mode wave is self-consistently generated by the shock and propagates back upstream as a precursor wave. We find that at magnetizations σ ≳ 1 (i.e. ratio of Poynting flux to particle energy flux of the pre-shock flow) the shock converts a fraction $$f_\xi ^{\prime } \approx 7 \times 10^{-4}/\sigma ^2$$ of the total incoming energy into the precursor wave, as measured in the shock frame. The wave spectrum is narrow-band (fractional width ≲1-3), with apparent but not dominant line-like features as many resonances concurrently contribute. The peak frequency in the pre-shock (observer) frame is $$\omega ^{\prime \prime }_{\rm peak} \approx 3 \gamma _{\rm s | u} \omega _{\rm p}$$, where γs|u is the shock Lorentz factor in the upstream frame and ωp the plasma frequency. At σ ≳ 1, where our estimated $$\omega ^{\prime \prime }_{\rm peak}$$ differs from previous works, the shock structure presents two solitons separated by a cavity, and the peak frequency corresponds to an eigenmode of the cavity. Our results provide physically grounded inputs for FRB emission models within the magnetar scenario.

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Research Organization:: Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)

Sponsoring Organization:: USDOE Office of Science (SC)

Grant/Contract Number:: PHY- 1804048; PHY-1523261

OSTI ID:: 1577638

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 485, Issue 3; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 69 works

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Erratum: The synchrotron maser emission from relativistic shocks in Fast Radio Bursts: 1D PIC simulations of cold pair plasmas Plotnikov, Illya; Sironi, Lorenzo Monthly Notices of the Royal Astronomical Society, Vol. 490, Issue 1 https://doi.org/10.1093/mnras/stz2653	journal	September 2019
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Precursor Wave Amplification by Ion–Electron Coupling through Wakefield in Relativistic Shocks Iwamoto, Masanori; Amano, Takanobu; Hoshino, Masahiro The Astrophysical Journal, Vol. 883, Issue 2 https://doi.org/10.3847/2041-8213/ab4265	journal	September 2019

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