The basics of the thermonuclear runaway theory of novae are confirmed by observations. The white dwarf sustains surface nuclear burning for some time after runaway, and until recently, it was commonly believed that radiation from this nuclear burning solely determines the nova's bolometric luminosity.

The processes by which novae eject material from the binary system remain poorly understood. Mass loss from novae is complex (sometimes fluctuating in rate, velocity, and morphology) and often prolonged in time over weeks, months, or years.

The complexity of the mass ejection leads to gamma-ray-producing shocks internal to the nova ejecta. When gamma rays are detected (around optical maximum), the shocks are deeply embedded and the surrounding gas is very dense.

Observations of correlated optical and gamma-ray light curves confirm that the shocks are radiative and contribute significantly to the bolometric luminosity of novae. Novae are therefore the closest and most common interaction-powered transients.

观测证实了新星热核失控理论的基础。白矮星在失控后会在一段时间内维持表面核燃烧，直到最近，人们普遍认为这种核燃烧的辐射仅决定了新星的热光度。

新星从双星系统中喷射物质的过程仍然知之甚少。新星的质量损失是复杂的（有时会在速率、速度和形态上发生波动），并且时间通常会持续数周、数月或数年。

质量抛射的复杂性导致了新星抛射物内部产生伽马射线的冲击。当探测到伽马射线时（在光学最大值附近），冲击会深深嵌入并且周围的气体非常密集。

对相关光学和伽马射线光曲线的观察证实，这些冲击是辐射性的，对新星的热光度有显着影响。因此，新星是最接近和最常见的交互驱动瞬变。