论文标题
Nova爆发的物理学：一种自稳定的风量损失的古典Nova爆发的理论模型
Physics of nova outbursts: A theoretical model of classical nova outbursts with self-consistent wind mass loss
论文作者
论文摘要
我们提出了一个基于辐射压力梯度（即所谓的光学厚风）加速的自洽的风量损失的经典新星爆发周期的模型。进化模型由Henyey代码计算为1.0 $ M_ \ ODOT $ WHITE DWARF（WD），其质量积聚率为$ 5 \ times 10^{ - 9} 〜m_ \ odot $ yr $ yr $^{ - 1} $。当发生光学厚的风时，富含氢的包膜的最外部连接到稳定移动的信封。我们确认在热核失控处没有内部冲击波。风质量损失率达到$ 1.4 \ times 10^{ - 4} 〜m_ \ odot $ yr $^{ - 1} $，在最大光谱膨胀的时期，在该时期的光谱温度下降至$ \ log t _ {\ rm ph} $（k）$（k）= 3.90。几乎所有的积聚质量都在风中丢失。在氢燃烧中产生的核能以光子发射的形式丢失（64％），重力能量（将风质提升到重力，35％）和风的动能（0.23％）。在热核失控发作后的第二天（$ \ sim $ \ sim $ 25 d之前，在光学最大值之前$ \ sim $ 25 d）的第二天，经典的Nova应该非常明亮。在NOVA爆发的衰减阶段，信封结构非常接近稳态溶液的结构。
We present a model for one cycle of a classical nova outburst based on a self-consistent wind mass loss accelerated by the gradient of radiation pressure, i.e., the so-called optically thick winds. Evolution models are calculated by a Henyey code for a 1.0 $M_\odot$ white dwarf (WD) with a mass accretion rate of $5 \times 10^{-9}~M_\odot$ yr$^{-1}$. The outermost part of hydrogen-rich envelope is connected to a steadily moving envelope when optically thick winds occur. We confirm that no internal shock waves occur at the thermonuclear runaway. The wind mass loss rate reaches a peak of $1.4 \times 10^{-4}~M_\odot$ yr$^{-1}$ at the epoch of the maximum photospheric expansion, where the photospheric temperature decreases to $\log T_{\rm ph}$ (K)=3.90. Almost all of the accreted mass is lost in the wind. The nuclear energy generated in hydrogen burning is lost in a form of photon emission (64 %), gravitational energy (lifting-up the wind matter against the gravity, 35 %), and kinetic energy of the wind (0.23 %). A classical nova should be very bright in a far-UV (100 - 300 Å) band, during a day just after the onset of thermonuclear runaway ($\sim$25 d before the optical maximum). In the decay phase of the nova outburst, the envelope structure is very close to that of a steady state solution.
