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Abstract
Magnetic reconnection, a critical process in astrophysical luminosity outbursts like solar flares, may also underpin such events in high-mass young stellar objects (HMYSOs). Despite theoretical predictions, observational evidence linking luminosity outbursts to magnetic reconnection in HMYSOs is still lacking. Our study examines the bursting HMYSO G36.11+0.55, where we find a significant correlation between the variability of 6.668 GHz CH3OH maser and the magnetic field strength inferred from 6.035 GHz ex-OH masers. This aligns with models of accretion-driven magnetic flux accumulation and reconnection-driven ejection, proposed for low-mass protostellar flares in theoretical studies. The CH3OH maser light curve closely resembles those observed or expected in other luminosity outbursts linked to magnetic reconnection. Furthermore, CH3OH maser flare regions coincide with jets from the source, also supporting the model of reconnection-driven magnetic flux ejection. These observational results underscore the essential role of magnetic fields in HMYSO outburst dynamics and material accretion near HMYSOs.
Magnetic reconnection is a key process in astrophysical luminosity outbursts, such as solar flares, and may also drive similar events in high-mass young stellar objects (HMYSOs). The authors study HMYSO G36.11+0.55, revealing a correlation between CH3OH maser variability and magnetic field strength, supporting models of reconnection-driven ejection and highlighting the role of magnetic fields in HMYSO dynamics.