A pulsar wind nebula origin of the ultra-high-energy source 1LHAASO J1929+1846
A pulsar wind nebula origin of the ultra-high-energy source 1LHAASO J1929+1846
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DOI：
10.1088/1674-4527/ace51d
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发表时间：
2023
影响因子：
1.8
通讯作者：
Jun Fang
中科院分区：
文献类型：
--
作者：
Qi Xia;Liancheng Zhou;Jun Fang
Abstract. 1LHAASO J1929+1846 is one of the ultra-high-energy (UHE, E > 0.1 PeV) sources in the first catalog of γ-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). It has been detected fluxes at 3 TeV for 2.48 ± 0.11 × 10-13 TeV-1 cm-2 s-1 with the Water Cherenkov Detector Array (WCDA) and at 50 TeV for 0.64 ± 0.06 × 10-16 TeV-1 cm-2 s-1 with the Kilometer Squared Array (KM2A), but the origin of its UHE emission remains unknown. The pulsar wind nebula (PWN) G54.1+0.3, which is powered by the pulsar PSR 1930+1852 with a period of 136 ms and it is detected within a 0.29° region around the centroid of 1LHAASO J1929+1846. We explore whether G54.1+0.3 is capable of producing the UHE radiation of 1LHAASO J1929+1846. Firstly, the data with Fermi Large Area Telescope (Fermi-LAT) for the PWN is analysed to obtain the GeV fluxes. Secondly, the multiband non-thermal fluxes for the nebula are investigated based on a one-zone time-dependent model. In the model, we assume the spin-down energy of the pulsar is persistently injected into particles (electrons and positrons) and magnetic field in the PWN, and these high-energy particles produce multiband non-thermal radiation from radio to γ-rays via synchrotron radiation and inverse Compton scattering. We reproduce the spectral energy distribution (SED) of PWN G54.1+0.3 with reasonable parameters. The result indicates that the UHE γ-ray source 1LHAASO J1929+1846 possibly originates from the PWN G54.1+0.3.
