论文标题
在修改量表中审查Novae的光曲线。 I.经常性诺瓦
Review of light curves of novae in the modified scales. I. Recurrent novae
论文作者
论文摘要
我们在“时间的对数，爆发的振幅”的修改量表中回顾了10个已知复发Novae（RN）的光曲线。建立了一个统一规则以使时间尺度归一化。确认已知结果：在一系列复发爆发中，Nova的光曲线保留了其形状，是通过在这10个Novae中区分三组来实现的。 CI AQL（+ V2487 OPH）和T PYX（+ im nor）组由另一个成员包含。 V745 SCO组包括V394 CRA和V3890 SGR。三个RN：T CRB，RS OPH和U SCO具有其独特性。在将银河novae的光曲线与大小和小麦芽岩（LMC和SMC）的一些Novae的光曲线进行了比较之后，我们除了在这些星系中还有3个已知的复发性Novae之外，还选择了几个候选者。 Assuming that the physical characteristics of the novae in the group coincide, we estimated the absolute magnitudes of the galactic novae: CI Aql and V2847 Oph have absolute magnitudes M_V=-7.5 mag, IM Nor and T Pyx - M_V=-7.2 mag, V3890 Sgr - M_V=-7.9 mag, U Sco - M_I=-9.0 mag.比较复发性诺瓦的摘要光曲线与一些低振幅古典的光曲线的比较使我们在最后一个中，可以区分复发性的26名候选人列表。其中三个是从其他作者列表中知道的。一个有趣的例子是V1017 SGR，该SGR于1919年爆发为T PYX类型的Nova，并且还显示出较小的爆发被归类为矮小新星爆发的明亮爆发。
We reviewed the light curves of 10 known recurrent novae (RNs) in the modified scales of the "logarithmic of time, amplitude of outburst". A unified rule was established to normalize the time scale. Confirmation of the known result: in a series of recurrent outbursts, the light curve of nova retains its shape, was realized by distinguishing three groups amongst these 10 novae. The CI Aql (+V2487 Oph) and T Pyx (+ IM Nor) groups contain by one additional member. The V745 Sco group includes V394 CrA and V3890 Sgr. Three RNs: T CrB, RS Oph and U Sco, have its own uniqueness. After comparing the light curves of galactic novae with the light curves of some novae of the Large and Small Magellanic Clouds (LMC and SMC), we selected several candidates for recurrent novae in addition to 3 known recurrent novae in these galaxies. Assuming that the physical characteristics of the novae in the group coincide, we estimated the absolute magnitudes of the galactic novae: CI Aql and V2847 Oph have absolute magnitudes M_V=-7.5 mag, IM Nor and T Pyx - M_V=-7.2 mag, V3890 Sgr - M_V=-7.9 mag, U Sco - M_I=-9.0 mag. The comparison of the summarized light curves of recurrent novae with the light curves of some low-amplitude classical novae allowed us amongst the last to distinguish the list of 26 candidates in recurrent novae. Three of them are known from lists of other authors. An interesting example is the V1017 Sgr, which erupted in 1919 as a nova of the T Pyx type, and which also shows less bright outbursts classified as dwarf nova outbursts.
