A Model for Magnetic Reconnection as the Origin of TeV Outbursts from NGC 1275

Abstract

NGC 1275 showed two TeV $γ$-ray outbursts between November 2022 and January 2023, as detected by the Large High Altitude Air Shower Observatory (LHAASO). The source was also active in the X-ray and GeV bands during the TeV outburst period. Very-long-baseline radio observations reported a sudden acceleration and deflection of a jet knot in late 2022, before the main TeV activity. Motivated by this sequence, we examine whether magnetic reconnection triggered by the interaction between the jet and the ambient medium can explain the TeV flares. In this picture, reconnection produces many plasmoids, and a large ``monster'' plasmoid becomes the main flare region. We model the low-state emission with a multi-zone stochastic-dissipation component and add a compact reconnection-powered region for the flaring state. We then compare leptonic and hadronic interpretations. The leptonic model explains the enhanced X-ray emission as electron synchrotron radiation and the TeV emission mainly as inverse-Compton radiation. A pure proton--proton model can also produce TeV photons if dense target gas is present, but it requires a compact cloud with a density above the values directly inferred from free--free absorption and a large proton power. These requirements are demanding, but they do not by themselves exclude the hadronic interpretation, because the gas may be compressed by the jet or may contain denser cloud cores. Our results show that magnetic reconnection in the parsec-scale jet is a viable origin of the 2022--2023 TeV activity of NGC 1275, while better constraints on the gas density and jet power are needed to distinguish between leptonic and hadronic radiation channels.