Early humps in WZ Sge stars
Early humps in WZ Sge stars
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WZ Sge 星的早期驼峰
DOI：
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
F. Meyer
中科院分区：
文献类型：
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作者：
Y. Osaki;F. Meyer
与双星轨道周期锁定的爆发中的光度驼峰仅在 WZ Sge 星爆发的早期阶段被观察到。有人认为，这种“早期驼峰”现象是质量比极低的双星系统吸积盘中潮汐2:1共振的表现。 “早期驼峰”可以通过 2:1 共振产生的潮汐耗散的双臂螺旋模式来理解，该模式首先由 Lin 和 Papaloizou ([CITE]) 讨论。在矮新星爆发期间潮汐从盘中去除角动量是一个重要特征，在盘不稳定模型的背景下进行了讨论。不同质量比系统中潮汐截断半径、3:1和2:1共振半径的排序自然导致矮新星系统根据质量比分为三组。 WZ Sge 恒星是那些质量比最低的系统，因此具有“早期驼峰”的特征。
Photometric humps in outburst that are locked with the binary orbital period have been observed exclusively in the early phase of outbursts of WZ Sge stars. It is suggested that this “early hump” phenomenon is the manifestation of the tidal 2:1 resonance in accretion disks of binary systems with extremely low mass ratios. The “early humps” can be understood by the two-armed spiral pattern of tidal dissipation generated by the 2:1 resonance, first discussed by Lin & Papaloizou ([CITE]). The tidal removal of angular momentum from the disk during outbursts of dwarf novae, an important feature, is discussed in the context of the disk instability model. The ordering of tidal truncation radius, the 3:1 and 2:1 resonance radius in systems of different mass ratio naturally leads to a classification of dwarf nova systems in three groups according to their mass ratio. The WZ Sge stars are those systems which have the lowest mass ratios and are therefore characterized by “early humps”.