A PeVatron Candidate: Modeling the Boomerang Nebula in X-ray Band

Liang, Xuan-Han; Li, Chaoming; Wu, Qi-Zuo; Pan, Jia-Shu; Liu, Ruo-Yu

doi:10.3390/universe8100547

Cited by 12 publications

(12 citation statements)

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“…Our estimates for the PWN B-field, based on the PWN's X-ray spatial properties and SED fitting, are not only significantly below what was suggested by Kothes et al (2006) but also below B = 140 μG, which was suggested by Liang et al (2022) based on modeling of the diffusion of relativistic electrons in the PWN. Our disagreement with the Bfield derived from the analysis done by Liang et al (2022) is expected given our different assumptions and models. While Liang et al (2022) incorporated UHE tail emission not necessarily related to the PWN itself within their SED modeling, this paper focuses solely on emission within the general bounds of the PWN region.…”

Section: Constraining Pwn Magnetic Fieldcontrasting

confidence: 54%

“…While Liang et al (2022) incorporated UHE tail emission not necessarily related to the PWN itself within their SED modeling, this paper focuses solely on emission within the general bounds of the PWN region. Furthermore, unlike the dynamical model used in this paper, the PWN model used in Liang et al (2022) does not include any interaction with the SNR, and the temporal evolution consists only of changes resulting from diffusion and radiative losses.…”

Section: Constraining Pwn Magnetic Fieldmentioning

confidence: 99%

“…Under this assumption, Kothes et al (2006) suggested that the PWN Bfield is 2.6 mG and that the PWN was crushed by the SNR reverse shock 3900 yr ago. A more recent study based on a model of the diffusion of the relativistic electrons injected into the PWN and X-ray radial profile suggested that the PWN Bfield is 140 μG (Liang et al 2022).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands

Pope,

Mori,

Abdelmaguid

et al. 2023

ApJ

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G106.3+2.7, commonly considered to be a composite supernova remnant (SNR), is characterized by a boomerang-shaped pulsar wind nebula (PWN) and two distinct (“head” and “tail”) regions in the radio band. A discovery of very-high-energy gamma-ray emission (E γ > 100 GeV) followed by the recent detection of ultrahigh-energy gamma-ray emission (E γ > 100 TeV) from the tail region suggests that G106.3+2.7 is a PeVatron candidate. We present a comprehensive multiwavelength study of the Boomerang PWN (100″ around PSR J2229+6114) using archival radio and Chandra data obtained two decades ago, a new NuSTAR X-ray observation from 2020, and upper limits on gamma-ray fluxes obtained by Fermi-LAT and VERITAS observatories. The NuSTAR observation allowed us to detect a 51.67 ms spin period from the pulsar PSR J2229+6114 and the PWN emission characterized by a power-law model with Γ = 1.52 ± 0.06 up to 20 keV. Contrary to the previous radio study by Kothes et al., we prefer a much lower PWN B-field (B ∼ 3 μG) and larger distance (d ∼ 8 kpc) based on (1) the nonvarying X-ray flux over the last two decades, (2) the energy-dependent X-ray size of the PWN resulting from synchrotron burn-off, and (3) the multiwavelength spectral energy distribution (SED) data. Our SED model suggests that the PWN is currently re-expanding after being compressed by the SNR reverse shock ∼1000 yr ago. In this case, the head region should be formed by GeV–TeV electrons injected earlier by the pulsar propagating into the low-density environment.

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Section: Constraining Pwn Magnetic Fieldcontrasting

confidence: 54%

Section: Constraining Pwn Magnetic Fieldmentioning

confidence: 99%

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A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands

Pope,

Mori,

Abdelmaguid

et al. 2023

ApJ

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“…As caveats of the model, it was found that the PWN interpretation of LHAASO J2226+6057 leads to a very high radius of PWN, as well as a very small value of magnetic field. Naturally, these results are in contrast with the observational results (Ge et al 2021;Liang et al 2022), thus indicating that the PWN may not be the contributing source to power the UHE gamma-ray source detected. This indicates interaction between SNRs and associated MCs may be the primary reason behind particle acceleration to PeV energies in Galactic sources.…”

Section: Introductioncontrasting

confidence: 79%

Supernova connection of unidentified ultra high energy gamma-ray source LHAASO J2108+5157

Sarkar¹

2023

Preprint

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We present a simple phenomenological model of hadronic interaction between protons accelerated in an old supernova remnant (SNR) and cold protons situated within the associated molecular clouds (MCs). The accelerated protons from the old SNR escaped the SNR shock front, and got injected into the MCs at an earlier time, producing ultra high energy gamma-rays and neutrinos through inelastic proton-proton interaction. We also take into account the acceleration and subsequent escape of electrons from the SNR shock front. The escaped electrons produce gamma-rays through various radiative cooling mechanisms, after getting injected into the MCs. We use the model discussed in this letter to explain the multiwavelength (MWL) spectral energy distribution (SED) of unidentified Galactic ultra high energy gamma-ray source LHAASO J2108+5157. We also discuss the feasibility of applying this model in other cases as well. Future observations can test the viability of the model discussed in this letter, which will in turn confirm that the SNRs can, in fact, accelerate particles up to PeV energies.

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“…The break could be caused by the energydependent escape of CRs from SNRs so that a large fraction of low-energy CRs have not reached the molecular clouds (e.g., Ohira et al 2011;Celli et al 2019;Bao & Chen 2021). In addition, PWN or pulsars could serve as the sources of these high-energy CR protons (Cheng et al 1990;Blasi 2000;Amato et al 2003;The LHAASO Collaboration et al 2021;Liang et al 2022).…”

Section: Hadronic Scenariomentioning

confidence: 99%

Revisiting the Chandra Observation on the Region of PSR J1J1809–193: Indication of the Existence of an X-Ray Halo and Implication for the Origin of HESS J1809–193

Liu

2023

ApJ

Self Cite

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HESS J1809–193 is an extended TeV γ-ray source and the origin of its γ-ray emission remains ambiguous. The pulsar wind nebula (PWN) of PSR J1J1809–193 lying inside the extended γ-ray emission is a possible candidate. Powered by the central pulsar, ultrarelativistic electrons in the PWN can produce radio to X-ray emission through synchrotron and γ-ray emission by inverse Compton (IC) scattering. To check whether this PWN is the counterpart of HESS J1809–193, we analyzed the Chandra X-ray radial intensity profile and spectral index profile of this PWN. We then adopted a one-zone isotropic diffusion model to fit the keV and TeV data. We found diffuse nonthermal X-ray emission extending beyond the PWN, which is likely an X-ray halo radiated by escaping electron/positron pairs from the PWN. A relatively strong magnetic field of ∼20 μG is required to explain the spatial evolution of the X-ray spectrum (i.e., the significant softening of the spectrum with increasing distance from the pulsar), which, however, would suppress the IC radiation of pairs. Our result implies that a hadronic component may be needed to explain HESS J1809–193.

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A PeVatron Candidate: Modeling the Boomerang Nebula in X-ray Band

Cited by 12 publications

References 50 publications

A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands

A Multiwavelength Investigation of PSR J2229+6114 and its Pulsar Wind Nebula in the Radio, X-Ray, and Gamma-Ray Bands

Supernova connection of unidentified ultra high energy gamma-ray source LHAASO J2108+5157

Revisiting the Chandra Observation on the Region of PSR J1J1809–193: Indication of the Existence of an X-Ray Halo and Implication for the Origin of HESS J1809–193

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