论文标题
Nova V1674 Herculis的定期信号（2021）
The Periodic Signals of Nova V1674 Herculis (2021)
论文作者
论文摘要
我们介绍了非常快的Nova V1674 Herculis（Nova她的2021年）的爆发期间的时间序列光度法。 2021光曲线在0.152921（3）D和501.486（5）s处显示了周期性信号，我们分别将其解释为基础二进制中的轨道和白矮人自旋 - 旋转周期。我们还检测到这两个时钟之间的 /差异 /频率的边带信号。在爆发的前15天内，自旋周期似乎增加了0.014（1）％。这种增加可能是由于旋转的磁性白矮人突然损失高角度摩托车气体（“ Nova爆炸”）。两个周期性的信号在爆发的早期都出现了非常出色的，我们将其归因于Nova进化的极端速度（并且从内部二进制辐射变得透明）。在最快的初始增加到约71毫秒之后，自旋period开始稳定下降〜160毫秒/年 - 比中间极点中通常比通常看到的速度快约100倍。这可能是由于高质量转移率的高积压扭矩，当低质量供体恒星被NOVA爆发强烈辐照时，这可能很常见。
We present time-series photometry during eruption of the extremely fast nova V1674 Herculis (Nova Her 2021). The 2021 light curve showed periodic signals at 0.152921(3) d and 501.486(5) s, which we interpret as respectively the orbital and white dwarf spin-periods in the underlying binary. We also detected a sideband signal at the /difference/ frequency between these two clocks. During the first 15 days of outburst, the spin-period appears to have increased by 0.014(1)%. This increase probably arose from the sudden loss of high-angular-momentum gas ("the nova explosion") from the rotating, magnetic white dwarf. Both periodic signals appeared remarkably early in the outburst, which we attribute to the extreme speed with which the nova evolved (and became transparent to radiation from the inner binary). After that very fast initial increase of ~71 ms, the spin-period commenced a steady decrease of ~160 ms/year -- about 100x faster than usually seen in intermediate polars. This is probably due to high accretion torques from very high mass-transfer rates, which might be common when low-mass donor stars are strongly irradiated by a nova outburst.
