Although the low declination the 2019 explosion of this recurrent nova was observed intensively with low resolution spectrograph on Celestron C11″ telescope. Below are examples of our spectra and all low resolution spectra collected in ARAS database. The result was presented at the Telč conference by Francois Teyssier.[Read more…] about Recurrent nova V3890 Sgr
Long term monitoring of intermediate polars is performed as a part of the InterLongitude Astronomy campaign. High quality and long time series observations allow us to investigate fine effects on complex light curves. In
the case of MU Cam we have investigated the periodic modulation of the spin phases with the orbital phase. This dependency was already described by Kim et al. (2005). As an explanation they proposed inhomogeneous accretion flow from the secondary. However based on our new data we can propose simple explanation as the influence of orbital sidebands in the periodic signal produced by intermediate polar. This explanation is supported by the fact that the changes in spin maxima phase are observed mainly when the sideband frequency is dominant in the periodogram. This result was presented on conferences in Bezovec and Telč.
The by-product of long term monitoring of intermediate polars is the discovery of low states similar to the low states in classical polars. Up to now we know that such phenomenon was observed in V1323 Her, FO Aqr, DO Dra.[Read more…] about Low states of intermediate polars
By-product of the Project dwarf are the observation of flares on red dwarf in binary systems. The project dwarf is aimed at detection of circumbinary extrasolar planets using the timing of the minima of low-mass eclipsing binaries. There are many red dwarf stars among the observed objects. Thus time to time some flare was detected. Object GJ3236 turned to be the most active one. Another one was AD Leo, subject of 2019 campaign[Read more…] about Flares on red dwarfs
Light curves of several semiregular and symbiotic variables from my program. Visual estimates together with data from ASAS-SN survey and CCD observations from AAVSO database. Some time visual data are useful (WY And), sometime the advantage of one visual observer is visible (CH Cyg), sometime visual data fill the gap in the survey data (TZ Cep), sometime visual observation are completely wrong (CK Vir).[Read more…] about Visual observations
Nova Cas 1995 probably finished its long supersoft X-ray source phase. This SSS phase was accompanied with periodic (0.6932672d) brightness variation interpreted as orbital wave. The amplitude of these variations increased until 2005. It reached 2.0 mag in the B band. Then it was decreasing slowly. The abrupt change came in 2015. Goranskij et al. reported amplitude only 0.3 mag (2015ATel.7985….1G). I observed V723 Cas regularly since 2010 with 1 meter VNT telescope. Unfortunately in 2015 Goranskij was the first to observe the target.[Read more…] about V723 Cas