The photometric rotational period of BH2* is unlikely to have arisen without tidal forcing. Here we show the rotational evolution of MESA stellar models initialized at various fractions of the zero-age main-sequence breakup rotational frequency, indicated by the color map. Magnetic braking (calculated here using the prescription of J. L. van Saders & M. H. Pinsonneault 2013) causes stellar rotation to slow over evolutionary timescales, shown here using ﹩{\nu }_{{\rm{\max }}}﹩ as an age proxy. No other sources of angular momentum loss (such as mass loss) are accounted for in this simulation. Even under this extremely permissive scenario, our putative photometric rotation period (horizontal line) at the present day (vertical line) is faster than permitted by if BH2*’s rotation were to be attributed entirely to its primordial angular momentum.