Fig. 6: P-rich stars versus nucleosynthesis predictions.
From: Phosphorus-rich stars with unusual abundances are challenging theoretical predictions
Median chemical abundance pattern of the P-rich stars (black squares) against the several model prediction patterns (colored lines), where [X/Fe]=log10(n(X)/n(Fe))-log10(n(X)/n(Fe))⊙. Error bars show the star-to-star abundance rms scatter. a The low-mass AGB subpanel shows the yields20 for a metallicity of Z = 0.004 (Fe/H] ~−0.7) and various initial masses [1.0–3.0]M⊙ in a rainbow fashion (steps of 0.5 M⊙), the redder being the lower masses. b In the core collapse supernova (SNII) subpanel, we show standard models (i.e. without any specific effect like rotation or O-C mergers) where the mass range is [13–40]M⊙ and metallicity such that Z = 0.001 ([Fe/H] ~−1.3)22. In the same subpanel, the pair-instability supernovae (PISN) yields62 are represented by dashed lines for masses of 180 and 200 M⊙. c The initial masses of the intermediate-mass AGB predictions20 (intM-AGB) range from 3.5 to 6 M⊙ with Z = 0.004 (or [Fe/H]~−0.7). d The SN Type Ia (SNIa) yields63 cover all values in central densities (1.37 × 109–2.12 × 109 g cm−3) and deflagration speeds (1.5%–5% of sound speed) provided by the authors. e Theoretical predictions for super-AGB stars64 (S-AGB) at two metallicities (Z = 0.001, 0.0001 or [Fe/H] ~−1.3, −2.3; continuous and dotted lines, respectively) and three initial masses (6.5, 7.5 and 8.0 M⊙) are displayed. f Finally, we display the only solar metallicity (Z = 0.014 or [Fe/H] ~0.0) novae yields available in the literature65 with CO core WDs (dashed lines) and ONe WDs (continuous lines) with the same mass range of [0.85–1.15]M⊙.
