Solar axions cannot explain the XENON1T excess
  We argue that the interpretation in terms of solar axions of the recent
XENON1T excess is not tenable when confronted with astrophysical observations
of stellar evolution. We discuss the reasons why the emission of a flux of
solar axions sufficiently intense to explain the anomalous data would radically
alter the distribution of certain type of stars in the color-magnitude diagram
in first place, and would also clash with a certain number of other
astrophysical observables. Quantitatively, the significance of the discrepancy
ranges from $3.3\sigma$ for the rate of period change of pulsating White
Dwarfs, and exceedes $19\sigma$ for the $R$-parameter and for $M_{I,{\rm
TRGB}}$.
