论文标题
基于MW的IMF的上限，H II地区的ADF和T $^2 $形式主义
The ADF and the t$^2$ formalism in H II regions based on the upper mass limit of the IMF for the MW
论文作者
论文摘要
我们深入研究了H II区域中的丰度差异问题，这次是从不同的角度研究：通过研究初始质量函数（IMF）对O，C的上限（M $ _ {\ rm UP} $）对O，C的影响，并由Milky Way的化学进化模型预测。我们使用用直接方法（DM）确定的丰度和温度无关的方法（TIM）。我们将目前的预测丰度与Orion，M17和M8的观察进行比较，以确定银河系IMF的M $ _ {\ rm UP} $值。从DM丰度中，模型可以预测M $ _ {\ rm up} $ = 25-45 m $ _ {\ odot} $，而从Tim，CEMS得出M $ _ {\ rm up} $ = 70-110 m $ _ $ _ _ {\ odot} $。预计具有恒星质量和恒星形成率的螺旋星系预计具有m $ _ {\ rm up} \ sim100 $ m $ _ {\ odot} $。这些结果支持从TIM得出的丰度优于从DM中得出的丰度。
We study in depth the abundance discrepancy problem in H II regions, this time from a different perspective than the usual one: by studying the effect of the upper mass limit (M$_{\rm up}$) of the initial mass function (IMF) on the O, C, and He predicted by chemical evolution models for the Milky Way. We use abundances determined with the direct method (DM) and with the temperature independent method (TIM). We compare the predicted abundances at the present time with observations of Orion, M17, and M8 to determine the M$_{\rm up}$ value of the galactic IMF. From the DM abundances, the models predict an M$_{\rm up}$ = 25-45 M$_{\odot}$, while from the TIM, CEMs derive an M$_{\rm up}$ = 70-110 M$_{\odot}$. Spiral galaxies with the stellar mass and star formation rate of the MW are predicted to have an M$_{\rm up} \sim100$ M$_{\odot}$. These results support that abundances derived from the TIM are better than those derived from the DM.
