Multi-epoch X-ray observations of SLSN-I 2018bsz support ejecta-CSM interaction as the dominant X-ray powering mechanism rather than a central magnetar.
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Late-time radio observations of SN 2012au show re-brightening best explained by emission from a newborn pulsar wind nebula rather than continued shock interaction with circumstellar material.
A new radiative-diffusion framework couples magnetar spin-down, shock propagation, and radiative transport to produce double-peaked, merged, or single-peaked light curves in engine-powered transients, demonstrated on LSQ14bdq.
A second coherent radio burst spanning 704-4032 MHz with spectral index -2.18, 54% linear and 22% circular polarization, and an orthogonal polarization angle jump was detected from 2XMM J104608.7-594306, showing rare radio activity in sources thought to be radio-quiet.
A magnetar model unifies emission phases of supernova-associated fast X-ray transients EP240414a, EP250108a, and GRB 171205A via jet, cocoon, wind, and PWN components.