Same as Fig. 10 but for models with M_H = 10⁻⁶ M_⊙. When possible, ⁴⁰Ca abundances obtained by Bauer & Bildsten (2019) have been added to the corresponding panel (labeled as BB19). For T_eff = 11 500 K, gray symbols (inside a box) represent the abundances obtained by Bauer & Bildsten (2018) for ¹⁶O, ²⁴Mg, ²⁸Si, ⁴⁰Ca, and ⁵⁶Fe using the observed photospheric abundance of pollutants in G29–38. All these isolated points correspond to an accretion rate of 10¹⁰ g s⁻¹ but have been shifted a bit from that particular value for the sake of clarity.