PNV J00444033+4113068: Early superhumps with 0.7 mag amplitude and non-red color
PNV J00444033+4113068: Early superhumps with 0.7 mag amplitude and non-red color
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PNV J00444033 4113068：早期超级驼峰，振幅为 0.7 等，非红色
DOI：
10.1093/pasj/psac068
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发表时间：
2022
影响因子：
2.3
通讯作者：
Nogami Daisaku
中科院分区：
文献类型：
--
作者：
Tampo Yusuke;Isogai Keisuke;Kojiguchi Naoto;Uemura Makoto;Kato Taichi;Tordai Tamas;Vanmunster Tonny;Itoh Hiroshi;Dubovsky Pavol A;Medulka Tomas;Sano Yasuo;Hambsch Franz-Josef;Taguchi Kenta;Maehara Hiroyuki;Ito Junpei;Nogami Daisaku
在WZ Sge型矮新星（DN）爆发的最初几天，2：1共振在吸积盘中诱导出螺旋臂结构，这在光学光变曲线中被观察到为早期的超级峰。我们报告了我们的光学观测的食WZ Sge型DN PNV J00444033+4113068在其2021年的超级爆发使用3.8米晴明望远镜和通过可变星星网络合作。食分析表明，其轨道周期为0.055425534（1）d。我们的观测证实了早期的超级驼峰，振幅为0.7等，是已知的WZ Sge型DNe中振幅最大的。更有趣的是，它的早期超峰在次极小值附近变得最红，而其他WZ Sge型DNe在早期超峰极大值附近显示出最红的颜色。爆发峰附近的光谱显示出Heii 4686和Hα两条双峰发射线，峰间距≥700 km s−1，支持一个非常高倾角的系统。通过对早期超峰的映射，利用具有垂直伸展双臂结构的吸积盘成功地再现了早期超峰的独特轮廓和颜色。因此，PNV J00444033+4113068中早期超峰的大振幅和独特的颜色行为可以用2：1共振模型沿着与其他WZ Sge型DNe一起解释。
In the first days of WZ Sge-type dwarf nova (DN) outbursts, the 2 : 1 resonance induces a spiral arm structure in the accretion disk, which is observed as early superhumps in optical light curves. We reports on our optical observations of an eclipsing WZ Sge-type DN PNV J00444033+4113068 during its 2021 superoutburst using the 3.8 m Seimei telescope and through the Variable Star Network collaboration. The eclipse analysis showed that its orbital period was 0.055425534(1) d. Our observations confirmed early superhumps with an amplitude of 0.7 mag, the largest amplitude among known WZ Sge-type DNe. More interestingly, its early superhumps became the reddest around their secondary minimum, whereas other WZ Sge-type DNe show the reddest color around the early superhump maximum. The spectrum around the peak of the outburst showed two double-peaked emission lines of Heii4686 Å and Hα with a peak separation of ≥700 km s−1, supporting a very high-inclination system. With the early superhump mapping, the unique profile and color of the early superhump are successfully reproduced by an accretion disk with a vertically extended double arm structure. Therefore, a large amplitude and a unique color behavior of the early superhumps in PNV J00444033+4113068 can be explained by the 2 : 1 resonance model along with other WZ Sge-type DNe.