The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

Burgess, Daniel A.; Mori, Kaya; Gelfand, Joseph D.; Hailey, Charles J.; Tokayer, Yarone M.; Woo, Jooyun; An, Hongjun; Malone, K.; Reynolds, Stephen P.; Safi‐Harb, Samar; Temim, Tea

doi:10.3847/1538-4357/ac650a

Cited by 17 publications

(15 citation statements)

References 51 publications

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“…A similarly low magnetic field (a few µG) was found in previous studies as the one needed to describe this source (Joshi et al 2022;Yu et al 2022). Moreover, a low magnetic field was found for other LHAASO detected PeVatron cadidates as well (De Sarkar & Gupta 2022;Joshi et al 2022;Crestan et al 2021;Li et al 2021;Burgess et al 2022), which is an a priori obvious outcome of requesting a leptonicallygenerated high energy emission. Further complications of the model, as we discussed, do not significantly alleviate this.…”

Section: Concluding Remarks: Large Radius/low Magnetic Field Issuesupporting

confidence: 76%

LHAASO J2226+6057 as a pulsar wind nebula

Sarkar

Zhang

Martín

et al. 2022

A&A

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Context. The Large High Altitude Air Shower Observatory has reported the detection of cosmic-ray sources in Milky Way that can accelerate particles up to PeV (= 10 15 eV) energies. These sources, so called "PeVatrons", are mostly unidentified. Several classes of sources, such as supernova remnants, pulsar wind nebula, or young stellar clusters can potentially be the counterparts of these PeVatrons.Aims. The aim of this work is to study a pulsar wind nebula interpretation of one of these PeVatrons, LHAASO J2226+6057, which has a relatively well covered multi-frequency spectrum. Methods. We have performed a leptonic, time-dependent modeling of the pulsar wind nebula (PWN) associated with PSR J2229+6114 considering a time-energy-dependent diffusion-loss equation. Injection, energy losses, as well as escape of particles were considered to balance the time-dependent lepton population. We have also included the dynamics of the PWN and the associated supernova remnant (SNR) and their interaction via the reverse shock to study the reverberation phase of the system. Results. We have considered different values of braking index (n) and true age (t age ) for the fitting of the multi-wavelength (MWL) spectral energy distribution (SED) of LHAASO J2226+6057. The best-fit PWN model parameters and their 1σ confidence intervals were evaluated. We have also demonstrated the impact of reverberation on the MWL SED with increasing time. Additionally, we have discussed the resultant large radius and low magnetic field associated with the PWN in question, as caveats for the possible physical connection of the pulsar as the origin of this high energy source.

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Section: Concluding Remarks: Large Radius/low Magnetic Field Issuesupporting

confidence: 76%

LHAASO J2226+6057 as a pulsar wind nebula

Sarkar

Zhang

Martín

et al. 2022

A&A

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“…Our work is based on the model described by Gelfand et al (2009) and was previously implemented to study other PWNe systems such as the Eel (Burgess et al 2022), Kes 75 (Gelfand et al 2014;Gotthelf et al 2021;Straal et al 2023), G21.5-0.9 (Hattori et al 2020), G54.1+0.3 (Gelfand et al 2015, and HESS J1640-465 (Gotthelf et al 2014;Mares et al 2021).…”

Section: Pwn Modelingmentioning

confidence: 99%

Broadband X-Ray Spectroscopy of the Pulsar Wind Nebula in HESS J1640-465

Abdelmaguid

Gelfand

Gotthelf

et al. 2023

ApJ

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We present updated measurements of the X-ray properties of the pulsar wind nebula associated with the TeV γ-ray source HESS J1640-465 derived from Chandra and Nuclear Spectroscopic Telescope Array data. We report a high N H value along the line of sight, consistent with previous work, which led us to incorporate the effects of dust scattering in our spectral analysis. Due to uncertainties in the dust scattering, we report a range of values for the PWN properties (photon index and unabsorbed flux). In addition, we fit the broadband spectrum of this source and found evidence for spectral softening and decreasing unasborbed flux as we go to higher photon energies. We then used a one-zone time-dependent evolutionary model to reproduce the dynamical and multiwavelength spectral properties of our source. Our model suggests a short spin-down timescale, a relatively higher than average magnetized pulsar wind, a strong pulsar wind nebula magnetic field and maximum electron energy up to PeV, suggesting HESS J1640-465 could be a PeVatron candidate.

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“…On the contrary, synchrotron emissions of PWNe do not suffer from the aforementioned effects, and thus they provide a complementary tool for investigating particle acceleration and transport in PWNe (e.g., Reynolds 2016). The highest-energy particles (in TeV-PeV energies) emit synchrotron photons in the X-ray to MeV band, and hence X-ray data are crucial to understanding UHECRs in PWNe (e.g., Mori et al 2022;Burgess et al 2022).…”

Section: Introductionmentioning

confidence: 99%

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

Park

Kim

Woo

et al. 2023

ApJ

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We present a detailed analysis of broadband X-ray observations of the pulsar PSR J1420−6048 and its wind nebula (PWN) in the Kookaburra region with Chandra, XMM-Newton, and NuSTAR. Using the archival XMM-Newton and new NuSTAR data, we detected 68 ms pulsations of the pulsar and characterized its X-ray pulse profile, which exhibits a sharp spike and a broad bump separated by ∼0.5 in phase. A high-resolution Chandra image revealed a complex morphology of the PWN: a torus-jet structure, a few knots around the torus, one long (∼7′) and two short tails extending in the northwest direction, and a bright diffuse emission region to the south. Spatially integrated Chandra and NuSTAR spectra of the PWN out to 2.′5 are well-described by a power-law model with a photon index Γ ≈ 2. A spatially resolved spectroscopic study, as well as NuSTAR radial profiles of the 3–7 keV and 7–20 keV brightness, showed a hint of spectral softening with increasing distance from the pulsar. A multiwavelength spectral energy distribution (SED) of the source was then obtained by supplementing our X-ray measurements with published radio, Fermi-LAT, and H.E.S.S. data. The SED and radial variations of the X-ray spectrum were fit with a leptonic multizone emission model. Our detailed study of the PWN may be suggestive of (1) particle transport dominated by advection, (2) a low magnetic-field strength (B ∼ 5 μG), and (3) electron acceleration to ∼PeV energies.

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The Eel Pulsar Wind Nebula: A PeVatron-candidate Origin for HAWC J1826−128 and HESS J1826−130

Cited by 17 publications

References 51 publications

LHAASO J2226+6057 as a pulsar wind nebula

LHAASO J2226+6057 as a pulsar wind nebula

Broadband X-Ray Spectroscopy of the Pulsar Wind Nebula in HESS J1640-465

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

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