Search Publications
Supernova remnants in the Magellanic Clouds
Bozzetto, L. M.; Filipovic, M. D.
We present initial results of an ongoing study of the supernova remnants (SNRs) and candidates in the Magellanic Clouds. Some 108 objects in both Clouds are considered to be either an SNR or a reliable candidate. This represents the most complete sample of known SNRs in any galaxy. therefore, this study allows us to study SNR population properties…
Magnetism in Massive Stars
Henrichs, H. F.
Stars with mass more than 8 solar masses end their lives as neutron stars, which we mostly observe as highly magnetized objects. Where does this magnetic field come from? Such a field could be formed during the collapse, or is a (modified) remnant of a fossil field since the birth of the star, or otherwise generated by a dynamo during its lifetime…
Structural Analysis of A2034 Clusters of Galaxies
Hudaverdi, M.; Ercan, E. N.; Bozkurt, M.
We present the analysis of X-ray and optical observations of Abell 2034. It is located at the moderate redshift of z=0.113. X-ray data are taken from the XMM-Newton archive. The best-fit single temperature of 7.6 keV model well defines the diffuse hot plasma. The cluster is observed by ground based optical Turkish National Observatory RTT-150 tele…
X-Ray Analysis of Galactic SNR G27.4+0.0
Hudaverdi, M.; Ercan, E. N.; Sezer, A. +2 more
In this work, we present X-ray analysis result of SNR G27.4+0.0 observed by XMM-Newton satellite. Three EPIC detectors are studied comparatively. The spatial and spectral analysis are performed, 0.3-10 keV (all band). In order to define possible distribution of interested abundances soft, medium and hard X-ray images are constructed. NEI (Non-equi…
Probing the Cosmic Filaments by Means of X-Ray Observations
Hudaverdi, M.; Ercan, E. N.; Bozkurt, M.
Recent observations and numerical simulations show that galaxies are not distributed in the Universe randomly. They are placed like the pearls of a necklace. The matter is spread into the space in the form of cosmic filaments and voids. The intersection regions of these cosmic filaments are what we observe as "clusters of galaxies". In this work w…
Dynamics of Faint Clusters of Galaxies
Erkurt, A.; Tektunali, H. G.; Hudaverdi, M. +1 more
Recent studies with high-resolution cameras have extensively showed that clusters of galaxies are not as relaxed as we assumed. With its advent technology XMM-Newton allows us to obtain the temperature and metal abundance map in detail. In this study, we present our results related to six (A194, A1056, A1674, A1882, A2634, A2638) nearby (z < 0.…
X-Ray Formation Mechanisms in Massive Binary Systems
Antokhin, I. I.
Massive, hot, luminous stars of types O, early B and WR have strong supersonic radiatively driven winds. Both single and binary early-type stars are known X-ray emitters. According to current understanding of X-ray formation mechanisms in the winds of single and binary early-type massive stars, binaries should be harder and more luminous X-ray sou…
Binary Clusters Observed with XMM-Newton X-Ray Observatory
Hudaverdi, M.; Beygu, B.; Ercan, N.
Clusters of galaxies are thought to form by accretion of galaxies along the cosmic filaments, and merging of clusters formed earlier. Observations and hydrodynamic simulations show the strong effects of mergers on physical conditions of the Intra Cluster Medium (ICM). In this work, we investigate five relatively nearby Abell clusters; A3705 (z= 0.…
Turkish National Observatory (TUG) View of Clusters of Galaxies
Hudaverdi, M.; Ercan, E. N.; Bozkurt, M. +2 more
We present the results of the optical observations of clusters of galaxies trough photometric observations with RTT150 telescope. We have selected a sample of 10 nearby (z < 1.2) Abell clusters from the northern sky. Properties of the extended X-ray intra-cluster medium (ICM) are studied using Chandra and XMM-Newton archival data. Considering p…
The complex structure of the Mg II regions of 40 BeV stars
Danezis, E.; Lyratzi, E.; Theodossiou, E. +4 more
In this paper we present a study of the UV Mg II resonance lines in 40 BeV stars' spectra. We used the model proposed by Danezis et al. (2002, 2003). This model is based on the idea of independent density layers in the regions where the spectral lines that present SACs (DACs) are created. We calculated the apparent rotation (Vrot) and e…