The Recently Discovered Dwarf Nova System ASAS J002511+1217.2: A New WZ Sagittae Star
The Recently Discovered Dwarf Nova System ASAS J002511+1217.2: A New WZ Sagittae Star
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最近发现的矮新星系统 ASAS J002511 1217.2：一颗新的 WZ 射手星
DOI：
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发表时间：
2005
期刊：
影响因子：
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通讯作者：
P. Pääkkönen
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作者：
M. Templeton;R. Leaman;P. Szkody;A. Henden;L. Cook;D. Starkey;A. Oksanen;M. Koppelman;D. Boyd;P. Nelson;T. Vanmunster;R. Pickard;N. Quinn;R. Huziak;M. Aho;R. James;A. Golovin;E. Pavlenko;R. Durkee;T. Crawford;G. Walker;P. Pääkkönen
激变变星ASAS J 002511 +1217.2于2004年9月在爆发中被全天空自动巡天（ASAS）发现，并在接下来的两个月里被AAVSO观测员密切监测。光度学和光谱学都表明这是一个非常短周期的系统。在ASAS探测后5 ~ 18天的超爆发中，出现了周期为0.05687 ± 0.00001（1 σ）天（81.9分钟）的清晰的超峰。我们观察到超峰轮廓的变化，类似于在其他短周期系统中观察到的“晚期超峰”的转变;超峰周期似乎在恢复到原始值之前略微增加一段时间，由此产生的超峰相位偏移了大约半个周期。在主爆发结束和单次回波爆发之间的4天平静期内，我们探测到了周期为0.05666 ± 0.00003（1 σ）天（81.6分钟）的变化。在回波及其快速下降期间，具有原始超级峰周期的弱变化再次出现。在探测后近30天进行的时间分辨光谱学，以及在下降过程中产生的轨道周期测量值为82 ± 5分钟。发射线光谱中存在窄和宽分量，表明存在多个发射区域。观测证据的权重表明，ASAS J 002511 +1217.2是WZ Sge型矮新星，我们讨论了这个系统如何适合WZ分类方案。
The cataclysmic variable ASAS J002511+1217.2 was discovered in outburst by the All‐Sky Automated Survey (ASAS) in 2004 September, and intensively monitored by AAVSO observers through the following 2 months. Both photometry and spectroscopy indicate that this is a very short period system. Clearly defined superhumps with a period of 0.05687 ± 0.00001 (1 σ) days (81.9 minutes) are present during the superoutburst, 5 to 18 days following the ASAS detection. We observe a change in superhump profile similar to the transition to “late superhumps” observed in other short‐period systems; the superhump period appears to increase slightly for a time before returning to the original value, with the resulting superhump phase offset by approximately half a period. We detect variations with a period of 0.05666 ± 0.00003 (1 σ) days (81.6 minutes) during the 4 day quiescent phase between the end of the main outburst and the single echo outburst. Weak variations having the original superhump period reappear during the echo and its rapid decline. Time‐resolved spectroscopy conducted nearly 30 days after detection and well into the decline yields an orbital period measurement of 82 ± 5 minutes. Both narrow and broad components are present in the emission‐line spectra, indicating the presence of multiple emission regions. The weight of the observational evidence suggests that ASAS J002511+1217.2 is a WZ Sge–type dwarf nova, and we discuss how this system fits into the WZ classification scheme.