氢在恒星的爆炸中燃烧。在这些环境中,温度范围为107～109K或更高,密度范围为102K～106g/cm3。在这些地方,核反应可以很快的发生,以致放射性核素诸如14O、15O、17F、18F等,在有机会衰变之前就俘获了质子。有关在这些环境中放射性核素的质子诱发反应,对于确定核素的合成以及能量的产生扮演着重要的角色。 特别是,当爆炸后,预测新星包层这些放射性核素的总量存在着很大的偏差,因为现在的18F（p,α）15O和18F（p,γ）19Ne反应在恒星中的反应率存在着很大的不确定性（达到约 Hydrogen burns in the star’s explosion. In these environments, temperatures range from 107 to 109 K or higher with densities ranging from 102 K to 106 g / cm3. In these places, the nuclear reaction can occur quickly, so that radionuclides such as 14O, 15O, 17F, 18F and so on, capture the protons before they have a chance to decay. Proton-induced responses to radionuclides in these environments play an important role in determining radionuclide synthesis and energy production. In particular, there is a large bias in predicting the total amount of these radionuclides in the nascent envelope when exploding, since the current response rate of the 19F (p, γ) 19Ne 18F (p, α) 15O and 18F There is a lot of uncertainty (up to about