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Pulsar wind nebula (PWN) Boomerang and the associated supernova remnant (SNR)G106.3+2.7 are among candidates for the ultra-high-energy (UHE) gamma-raycounterparts published by LHAASO. Although the centroid of the extended source,LHAASO J2226+6057, deviates from the pulsar's position by about $0.3^\circ$,the source partially covers the PWN. Therefore, we cannot totally exclude thepossibility that a part of the UHE emission comes from the PWN. Previousstudies mainly focus on whether the SNR is a PeVatron, while neglecting theenergetic PWN. Here, we explore the possibility of the Boomerang Nebula being aPeVatron candidate by studying its X-ray radiation. By modelling the diffusionof relativistic electrons injected in the PWN, we fit the radial profiles ofthe X-ray surface brightness and the photon index. The solution with a magneticfield $B=140\mu$G can well reproduce the observed profiles and implies a severesuppression of IC scattering of electrons. Therefore, a proton component needbe introduced to account for the UHE emission, in light of recent LHAASO'smeasurement on Crab Nebula, if future observations reveal part of the UHEemission originating from the PWN. In this sense, Boomerang Nebula would be ahadronic PeVatron.

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