000007933 001__ 7933
000007933 005__ 20260211165809.0
000007933 0247_ $$2DOI$$a10.3390/galaxies13020019
000007933 037__ $$aSCART-2026-0096
000007933 100__ $$aVink, Jorick
000007933 245__ $$aThe Blue Supergiant Problem and the Main-Sequence Width
000007933 260__ $$c2025
000007933 520__ $$aUsing Gaia DR3 we derive new distances and luminosities for a sample of Galactic B supergiants which were thought to be post main-sequence (MS) objects from their HR diagram location beyond the terminal-age MS (TAMS). When applying the newer Gaia distances in addition to enhanced amounts of core-boundary mixing, aka convective overshooting, we show that these Galactic B supergiants are likely enclosed within the MS band, indicating an evolutionary stage of steady core hydrogen burning. We discuss the importance of considering enhanced overshooting and how vectors in the mass-luminosity plane (ML-plane) can be used to disentangle the effects of wind mass loss from interior mixing. We finish with the key message that any proposed solution to the BSG problem should consider not only an explanation for the sheer number of B supergiants inside the Hertzsprung gap, but should at the same time also account for the steep drop in rotation rates identified at spectral type B1—corresponding to an effective temperature of ∼21 kK, and for which two distinct families of solutions have been proposed.
000007933 594__ $$aNO
000007933 6531_ $$amassive stars
000007933 6531_ $$astellar evolution
000007933 6531_ $$ablue supergiants
000007933 6531_ $$ared supergiants
000007933 6531_ $$ablue supergiant problem
000007933 6531_ $$astellar winds
000007933 6531_ $$aconvection
000007933 700__ $$aOudmaijer, René
000007933 773__ $$c19$$n2$$pGalaxies$$v13$$y2025
000007933 8560_ $$frene.oudmaijer@ksb-orb.be
000007933 85642 $$ahttps://www.mdpi.com/2075-4434/13/2/19
000007933 905__ $$apublished in
000007933 980__ $$aREFERD