A “Nova” refer to close binary systems, where outbursts occur on the white dwarf surface due to thermonuclear runaway. Numerical simulations of nova explosions have shown that the accreted envelopes attain peak temperature of about \(4 \times 10^{8}\) K. The temperature remains at the peak value for about several hundred seconds; this allows nuclear reactions to take place in the ejecta. Theoretical studies predict significant overproduction of few elements, e.g., 17O, 15N, and 13C, with respect to solar abundances. Spectroscopic observations have also confirmed about high metal abundances in novae ejecta. This paper briefly discusses about elemental abundances in novae ejecta predicted by the nucleosynthesis process as well as that found from observations.

“新星”是指紧密的二元系统，其中白矮星表面由于热核失控而发生爆发。新星爆炸的数值模拟表明，积聚的包壳达到约\（4×10 ^ {8} \）  K的峰值温度。温度保持在峰值约几百秒；温度保持在峰值附近。这使得核反应在弹射体中发生。理论研究预测，相对于太阳丰度，很少有元素过量生产，例如17O，15N和13C。光谱观察还证实了新星喷射中的高金属丰度。本文简要讨论了通过核合成过程预测的新星射出中的元素丰度以及从观测中发现的元素丰度。