Recent observations have shown that [P/Fe] in the Galactic stars decreases with increasing [Fe/H] for [Fe/H] ≳ − 1 whereas it is almost subsolar for [Fe/H] ≲ −2. These [P/Fe] trends with [Fe/H] have not been well reproduced by previous theoretical models incorporating phosphorus (P) enrichment only by core collapse supernoave. We here show, for the first time, that the trends can be naturally explained by our new models incorporating P enrichment by oxygen–neon (ONe) novae, which occur at the surface of massive white dwarfs whose masses are larger than 1.25M _⊙ with a metallicity-dependence rate. We also show that the observations can be better reproduced by the models by assuming that (i) the total mass of gaseous ejecta per ONe nova (M _ej) is as high as 4 × 10⁻⁵ M _⊙ and (ii) the number of such novae per unit mass (N _ONe) is as large as 0.01 at [Fe/H] ≈ −3. The assumed M _ej is consistent with observations, and the high N _ONe is expected from recent theoretical models for ONe nova fractions. We predict that (i) [P/Fe] increases with increasing [Fe/H] for −2 ≲ [Fe/H] ≲ −1 and (ii) [P/Fe] and [Cl/Fe] trends with [Fe/H] are very similar to each other due to very large yields of P and Cl from ONe novae. It is thus worthwhile for future observations to assess the validity of the proposed P enrichment by ONe novae by confirming or ruling out these two predictions.

中文翻译：

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银河系中新星的磷富集

最近的观测表明，当 [Fe/H] ≳ − 1 时，银河系恒星中的 [P/Fe] 随着 [Fe/H] 的增加而降低，而当 [Fe/H] ≲ -2 时，[P/Fe] 几乎接近太阳下。这些 [P/Fe] 与 [Fe/H] 的趋势尚未通过先前仅通过核心塌陷超新星富集磷 (P) 的理论模型来很好地重现。我们在这里首次表明，这些趋势可以通过我们的新模型自然地解释，该模型结合了氧氖（ONe）新星富磷，这些新星发生在质量大于 1.25 的大质量白矮星表面中号 _⊙具有金属丰度依赖性。我们还表明，通过假设（i）每个 ONe 新星的气体喷射物的总质量（中号 _ej ) 高达 4 × 10 ⁻⁵ 中号 _⊙和 (ii) 每单位质量的此类新星数量（氮 _ONe ) 在 [Fe/H] ≈ -3 时大至 0.01。假设的中号 _ej与观察结果一致，且高氮 _ONe是根据最近的 ONe 新星分数理论模型预计的。我们预测 (i) [P/Fe] 随着 [Fe/H] 的增加而增加，且 -2 ≲ [Fe/H] ≲ -1 且 (ii) [P/Fe] 和 [Cl/Fe] 随 [Fe] 变化趋势/H] 彼此非常相似，因为 ONe 新星产生的 P 和 Cl 非常大。因此，未来的观测有必要通过确认或排除这两个预测来评估所提出的 ONe 新星富集 P 的有效性。