论文标题
IW和Star ASAS J071404+7004.3的分析
Analysis of the IW And star ASAS J071404+7004.3
论文作者
论文摘要
我们在2020年的明亮灾难性变量ASAS J071404+7004.3进行了时间分辨的光度法运动。Inight等人。 （2022，ARXIV/2109.14514）最近发表了时间分辨的光谱，X射线观测和长期和短期光学变化。尽管他们的结果在许多地方都是正确的，但他们将ASAS J071404+7004.3归类为VY SCL型Novalike对象。通过比较该对象的ASA-SN数据和IW和型对象HO PUP，我们表明它们的类型分类不正确。 ASAS J071404+7004.3显示出静止的爆发，然后是浅倾角，这是IW和Star的定义特征。该对象主要显示具有低振幅矮化Nova型振荡的状态，其中一些可以识别为“心跳”型状态，为各种IW和型现象。 Inight等人描述的低状态。 （2022）并不是VY SCL恒星的真正低状态，而是一个矮人型状态，爆发幅度增加。基于地面的（我们的运动）和苔丝观察结果都检测到了轨道变化，其周期[0.136589（5）d通过地面运动和TESS数据的0.1366476（3）d。与Inight等人的Radial-velocity研究获得的时期非常吻合。 （2022）。 2019 - 2020年的ASAS J071404+7004.3的停滞并不比其矮化Nova型状态更明亮。当矮nova型变化的幅度较大时，这一物体的最明亮时刻发生在大量时，这挑战了当质量转移率很高时发生静止的解释。
We made a time-resolved photometric campaign of the bright cataclysmic variable ASAS J071404+7004.3 in 2020. Inight et al. (2022, arXiv/2109.14514) recently published time-resolved optical spectroscopy, X-ray observations and long- and short-term optical variations. Although their results were correct in many parts, they classified ASAS J071404+7004.3 as a VY Scl-type novalike object. By comparing the ASAS-SN data of this object and the IW And-type object HO Pup, we showed that their type classification was incorrect. ASAS J071404+7004.3 showed outbursts from a standstill followed by shallow dips, which is the defining characteristic of an IW And star. This object predominantly showed states with low-amplitude dwarf nova-type oscillations, some of which could be identified as the "heartbeat"-type state as a variety of the IW And-type phenomenon. The low state described by Inight et al. (2022) was not a true low state of a VY Scl star, but a dwarf nova-type state with increased outburst amplitudes. Both ground-based (our campaign) and TESS observations detected orbital variations whose periods [0.136589(5) d by the ground-based campaign and 0.1366476(3) d by the TESS data] are in very good agreement with the one obtained by radial-velocity studies by Inight et al. (2022). The standstill in 2019-2020 in ASAS J071404+7004.3 was not brighter than its dwarf nova-type states. The brightest moment of this object occurred when the amplitudes of dwarf nova-type variations were large, which challenges the widely accepted interpretation that standstills in Z Cam stars occur when the mass-transfer rates are high.
