Speaker
Description
Recent LHAASO observations have revealed ultra-high-energy (UHE) gamma-ray emission extending into the PeV range from several pulsar wind nebulae (PWNe), establishing them as prime candidates for Galactic “PeVatrons.” We conducted a comparative study of three PWNe powered by pulsars with markedly different spin-down ages: PSR J0007+7303 (14 kyr), PSR J1849−0001 (43 kyr), and PSR J1740+1000 (114 kyr). Despite their diverse evolutionary stages and environments, all three nebulae emit photons beyond 100 TeV, posing important questions about particle acceleration and transport over pulsar lifetimes. We compare their X-ray properties measured with Chandra X-ray Observatory (CXO) and their UHE properties measured by LHAASO, also computing estimates for the magnetic field and maximum particle energy based on these measurements. We then perform multi-wavelength (MW) SED modeling for these systems and compare the results with our estimates, assessing the applicability and limitations of the single-zone framework to PWNe spanning a wide range of ages.
