Photometric observations were made for the SX Phoenicis star XX Cyg between September and October 2019 at the 1.88-m Kottamia reflector telescope in Egypt. A total 340 VBR CCD photometer of the BVR filters with the light curves derived from the new observations was used. in addition 9540 photometric magnitude in V color from different sources. The variable, comparison and check stars monitored in the same frames. Light curves indicate a total light range of 0.82 mag. We do not detect any secondary maximum in the descending portion of the light curves of XX Cyg, as noticed in some previous work. magnitude estimates are presented for the delta scuti star XX Cyg.

We present a high angular resolution observation of OH maser main lines at 1665 MHz and 1667 MHz in addition to the 1720 MHz satellite line toward the high-mass star forming region IRAS 06056+2131. The IRAS 06056+2131 observations were carried out using the UK radio interferometer array, Multi-Element Radio Linked Interferometer Network (MERLIN) through different nights along with different phase and amplitude calibrator sources. The full polarization mode at MERLIN enables us to investigate the magnetic strength around the source through studying both linear and circular polarization in the OH maser emission lines. The results of this study show a weak 1665 MHz emission toward the IRAS 06056+2131 source estimated to be ~ 4Jy as total intensity. On the other hand, we have not reported any emission lines from the 1667 MHz and 1720 MHz toward IRAS 06056+231. Accordingly, the star forming evolutionary status of the traced proto-stellar object has been discussed.

We obtained the X-ray spectrum in the early stage of the outburst. We simultaneous measurements of the Fe K emission line of the Super Soft Source (SSS) and Classical Novae observed with two satellites are Suzaku and NuStar. The spectrum is modeled with an absorbed thermal bremsstrahlung spectrum (freefree emission) and several Gaussians for the most components of the Fe K lines. SSSs are objects with temperatures of between 200,000 and 800,000 K and luminosities around 1038 ergs/s. More than 90% of their observed X-ray emission is below 0.5 keV. Currently, it is a subject of debate exactly what physical object is associated with these high X-ray luminosities and low temperatures. Super-Hard X-ray emission was detected up to～70 keV from the classical nova V2491 Cygni. Currently, there are two leading theories. In the first, SSSs consist of a neutron star or black hole surrounded by a bright and highly extended accretion disk or cloud, which reprocesses energetic photons produced by the accretion onto the compact object. In the other theory, SSSs are white dwarfs with classic hydrogen fusion occurring from material accreting onto their surfaces. The second theory would make SSSs the progenitor for Type Ia supernovae.

In this work, there are two separated open clusters were discovered in the field of the open cluster Gulliver 11, one of them has been named Gulliver 11C, which is in agreement with the results obtained by Cantat-Gaudin , while the other has been named Gulliver 11B, located behind Gulliver 11C as obtained through our wok. The vector point diagram method was used to specify the membership probability. Photometric and astrometric parameters of both the two clusters were studied, center, radius, distance, color excess, age, luminosity-mass functions, total mass and relaxation time of the clusters were determined. All of our results were obtained depends on parallax, proper motions, and the Renormalized Unit Wight Error (RUWE) . In this respect, the Gaia DR2 catalogue was used for data extraction to obtain these parameters. The results obtained were compared with those of the literature.

We present the results of the soft X-ray observations for blazar source namely, MRK 421. The observations of this source were carried out using the Suzaku satellite. Suzaku (Also known as Astro-E2) is Japan's fifth X-ray Astronomy mission, which covers the energy range 0.2 - 700 keV, where Suzaku consists of: the X-ray Imaging Spectrometer (XIS, Koyama et al. 2007) for the 0.2−10 keV low energy band; the Hard X-ray Detector (HXD, Takahashi, et al. 2007; Kokubun et al. 2007) Thanks to the soft X-ray broad bandpass coupled with the high sensitivity of Suzaku(0.8-10 keV), we measured the evolution of the spectrum over the 0.8–10 keV flux of 3 × 10 −10 erg s −1 cm −2. The BL Lac Object MRK 421, at a redshift of z=0.031, has been monitored. As a result of this monitoring toward the sources ( MRK 421 ), We noticed that the X-ray flux was variable through all targets. This variability has been discussed in this study. Additionally, different models have been applied to the sources in order to estimate alist of parametres such as photon index, normalization, source temperature, break energy in addition to the fitting uncertainty(chi-square).

We will study the solar photospheric abundance of Fe I and Fe II using high-resolution spectroscopic data obtained by Fourier transform spectrograph (FTS). Based on the Local Thermodynamical Equilibrium (LTE) and Non-Local Thermodynamical Equilibrium (NLTE) assumptions, we re-derive the solar Fe abundance using the model of the solar photosphere of Holweger & Muller.

We present the first scientific results of the program on short term period variable stars observed using the KFISP facility at the Kottamia Astronomical Observatory (KAO). These results include good quality light curves of pulsating star (XX Cyg), with eclipsing algol type star binaries (RV Tri). Photometric observations were made for the SX Phoenicis star XX Cyg between September and October 2019. The photometric precision reached by the available instrumental and equipment, and used in the several scientific subprograms, has satisfied the initial expectations. A total 340 VBR CCD photometeric with the light curves derived from the new observations was used. in addition 9540 photometric magnitudes in V color from different sources. Light curves indicate a total light range of 0.82 mag. We do not detect any secondary maximum in the descending portion of the light curves of XX Cyg, as noticed by Alerto and Michael (1986)