A5041661264- Astrophysical Phenomena and Observations
- High-pressure geophysics and materials
- Pulsars and Gravitational Waves Research
- Mechanics and Biomechanics Studies
- Crystallography and Radiation Phenomena
- Nuclear Physics and Applications
- Particle Detector Development and Performance
- Laser-Plasma Interactions and Diagnostics
- Radiation Detection and Scintillator Technologies
- Advanced X-ray Imaging Techniques
- Astrophysics and Cosmic Phenomena
University of Alicante
2020-2024
4U 0114+65 is a high-mass X-ray binary system formed by the luminous supergiant B1Ia, known as V{*} V662 Cas, and one of slowest rotating neutron stars (NS) with spin period about 2.6 hours. This fact provides rare opportunity to study interesting details accretion within each individual pulse compact object. In this paper, we analyze 200 ks Chandra grating data, divided into 9 uninterrupted observations around orbit. The changes in circumstellar absorption column through orbit suggest an...
Cen X-3 is a compact high mass X-ray binary likely powered by Roche lobe overflow. We present phase-resolved spectral and timing analysis of two pointed XMM-Newton observations. The first one took place during normal state the source, when it has luminosity $L_{\rm X}\sim 10^{36}$ erg s$^{-1}$. This observation covered orbital phases $\phi= 0.00-0.37$, i.e. egress from eclipse. lightcurve highly structured, showing distinctive intervals. argue that different intervals correspond to emergence...
Cen X-3 is a compact, high-mass X-ray binary (HMXRB), likely powered by Roche lobe overflow. We present phase-resolved spectral and timing analysis of target opportunity Chandra observation made during low-flux to high-flux transition. The high-resolution spectra allow us delve into the events that occurred this episode. spectrum described single black body absorbed local column density order 10 23 − 24 cm −2 , which one two orders magnitude higher than found for previous analyses data taken...
We present the first {\it XMM-Newton} observation of classical supergiant high-mass X-ray binary XTE J1855$-$026 taken entirely during eclipse neutron star (NS), covering orbital phases $\phi= 0.00-0.11$. The analysis data allows us to a) compare with parameters obtained existing pre and b) explore back illuminated stellar wind B0I type donor. black body component, used describe soft excess eclipse, is not observed eclipse. It must be then produced near NS or along donor-NS line. $0.3-10$...