We performed the photometric observations of possible luminous blue variable (LBV) in UGC 2773 in a year after the eruption. Its brightness is measured to be ~ 17 mag in optical bands on Aug. 21. The light curves exhibit the very slow evolution and the fluctuations of around three tenth magnitude with the time scale of a few days.
■ [Extragalactic nova] M33 2010-07a : rebrightening again !
We update the light curve of M33 2010-07a. The light curve exhibit the rebrightening again. The light curves show the fast decline rate just after the maximum date. Thus, this nova may undergo the very rapid evolution of expanding atmosphere and have already progressed in the transitional phase. Alternatively, the dust formations in the nova ejecta might result in rapid decrease of the luminosity and the rebrightening.
■ [dwarf nova] Spectroscopy of WZ Sge type dwarf nova V592 Her : update
We update the spectra of V592 Her. The spectra suddenly become red. The absorption lines and at 8200A become slightly deep comparing to that obtained on Aug, 1.
We performed the spectroscopy of the extremely slow nova V1280 Sco. The spectrum shows the strong emission line of H-alpha. The emission line still forms the P Cyg profile with the asymmetric profile. The absorption lines reached at 2300km/s. HeI also shows the P Cyg profile with the absorptions, which reached at the 1400km/s. These characteristics indicate that the nova atmosphere still forms optically-thin winds above the optically-thick photosphere. On the other hand, the spectra exhibit the forbidden line, which indicate that a part of the expanding shell become the very optically-thin.
■ [dwarf nova] Spectroscopy of WZ Sge type dwarf nova V592 Her
We performed the spectroscopic observation of WZ Sge type dwarf nova V592 Her. The spectrum shows the absorptions of Balmer series. These absorptions seem to be broadened to bluer wavelength region. The absorption lines indicate that the disk become optically thick due to its radiations from the high temperature.
■ [Extragalactic nova] M33 2010-07a : slow decline after the rebrightening
We performed the photometric observation of M33 2010-07a. This nova underwent the rebrightening just after the rapid decline. This phenomena is also seen in that of V2491 Cyg (Arai et al.). The timescale of its decline of M33 2010a-07a may be also similar to that of V2491 Cyg.