Run of the GSP_Phot T_eff, pulsation period (Pf), and peak-to-peak amplitude in the G band [Amp(G)] of RR Lyrae stars for which both the GSP_Phot and the SOS Cep&RRL G absorption [A(G)] values are available as a function of the difference between the two absorption estimates, using for GSP_Phot only the MARCS library results in the astrophysical_parameters_supp table of the DR3 archive. The absorption differences are clearly unrelated to the pulsation period or the G peak-to-peak amplitude. The top panel clearly shows that large absorption differences are caused by an incorrect temperature in GSP_Phot MARCS. The absorption estimates agree for 6 300 ≲ T_eff ≲ 6 800 K, which is the typical mean temperature range of RRab stars (see also Column 11 in Table A.3). The variability (0.2-1.0 mag peak-to-peak amplitude in the G band) of the RR Lyrae stars is absorbed as increased flux uncertainties in the time-averaged BP/RP spectra. Through the unusually large BP/RP flux uncertainties, the χ² is flattened, and thus space for degeneracies is opened. In particular, a temperature-extinction degeneracy takes place that would explain the difference between the SOS Cep&RRL and the GSP_Phot absorption estimates for RR Lyrae stars.