论文标题
2018年Nova的持续邮政爆发亮度，进化的伴侣和较长的轨道时期
The sustained post-outburst brightness of Nova Per 2018, the evolved companion, and the long orbital period
论文作者
论文摘要
2018年Nova（= V392）从比静态亮2mag亮2mag时停止了下降，自2019年以来一直在这种高原上稳定。喷射已经完全稀释到星际空间中。在高原阶段，我们获得了V392的BVrigrizy光度法和光谱，并将其与Nova爆发前收集的等效数据进行了比较。我们发现伴侣恒星是G9 IV/III，轨道时期为3.4118天，根据经典NOV的最长已知时期，V392是V392。 V392人的位置在理论等小线上的位置在经典的Novae和Novae在共生二进制室内爆发的位置，从而弥合了差距。红色的变红得出为E（B-V）= 0.72，并且等距的拟合返回系统的3.6 Gyr Age，1.35 MSUN，5.3 RSUN和15 LSUN和15 LSUN。射出的巨大NE过度过度以及从Nova最大的迅速下降，这两个指向巨大的白矮人（M（WD）> = 1.1-1.2 msun）。该系统被视为接近杆的条件，并且当前的高原相是由WD仍在表面燃烧的CS辐射引起的。
Nova Per 2018 (= V392 Per) halted the decline from maximum when it was 2mag brighter than quiescence and since 2019 has been stable at such a plateau. The ejecta have already fully diluted into the interstellar space. We obtained BVRIgrizY photometry and optical spectroscopy of V392 Per during the plateau phase and compared it with equivalent data gathered prior to the nova outburst. We find the companion star to be a G9 IV/III and the orbital period to be 3.4118 days, making V392 Per the longest known period for a classical nova. The location of V392 Per on the theoretical isochrones is intermediate between that of classical novae and novae erupting within symbiotic binaries, in a sense bridging the gap. The reddening is derived to be E(B-V)=0.72 and the fitting to isochrones returns a 3.6 Gyr age for the system and 1.35 Msun, 5.3 Rsun, and 15 Lsun for the companion. The huge Ne overabundance in the ejecta and the very fast decline from nova maximum both point to a massive white dwarf (M(WD) >= 1.1-1.2 Msun). The system is viewed close to pole-on conditions and the current plateau phase is caused by irradiation of the CS by the WD still burning at the surface.
