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HD 62658 (B9p V) is a little-studied chemically peculiar star. Light curvesobtained by the Kilodegree Extremely Little Telescope (KELT) and TransitingExoplanet Survey Satellite (TESS) show clear eclipses with a period of about4.75 d, as well as out-of-eclipse brightness modulation with the same 4.75 dperiod, consistent with synchronized rotational modulation of surface chemicalspots. High-resolution ESPaDOnS circular spectropolarimetry shows a clearZeeman signature in the line profile of the primary; there is no indication ofa magnetic field in the secondary. PHOEBE modelling of the light curve andradial velocities indicates that the two components have almost identicalmasses of about 3 M$_\odot$. The primary's longitudinal magnetic field $\langleB_z \rangle$ varies between about $+100$ and $-250$ G, suggesting a surfacemagnetic dipole strength $B_{\rm d} = 850$~G. Bayesian analysis of the Stokes$V$ profiles indicates $B_{\rm d} = 650$~G for the primary and $B_{\rm d} <110$ G for the secondary. The primary's line profiles are highly variable,consistent with the hypothesis that the out-of-eclipse brightness modulation isa consequence of rotational modulation of that star's chemical spots. We alsodetect a residual signal in the light curve after removal of the orbital androtational modulations, which might be pulsational in origin; this could beconsistent with the weak line profile variability of the secondary. This systemrepresents an excellent opportunity to examine the consequences of magneticfields for stellar structure via comparison of two stars that are essentiallyidentical with the exception that one is magnetic. The existence of such asystem furthermore suggests that purely environmental explanations for theorigin of fossil magnetic fields are incomplete.

MOBSTER -- III. HD 62658: a magnetic Bp star in an eclipsing binary with a non-magnetic 'identical twin'