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Littérature scientifique sur le sujet « X-rays: star »

Auteur : Grafiati

Publié le 9 mars 2023

Mis à jour le 31 juillet 2025

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Articles de revues sur le sujet "X-rays: star"

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Vilhu, O., T. R. Kallman, K. I. I. Koljonen, and D. C. Hannikainen. "Wind suppression by X-rays in Cygnus X-3." Astronomy & Astrophysics 649 (May 2021): A176. http://dx.doi.org/10.1051/0004-6361/202140620.

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Context. The radiatively driven wind of the primary star in wind-fed X-ray binaries can be suppressed by the X-ray irradiation of the compact secondary star. This causes feedback between the wind and the X-ray luminosity of the compact star. Aims. We aim to estimate how the wind velocity on the face-on side of the donor star depends on the spectral state of the high-mass X-ray binary Cygnus X-3. Methods. We modeled the supersonic part of the wind by computing the line force (force multiplier) with the Castor, Abbott & Klein formalism and XSTAR physics and by solving the mass conservation a

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Brorby, M., and P. Kaaret. "X-rays from Green Pea analogues." Monthly Notices of the Royal Astronomical Society 470, no. 1 (2017): 606–11. http://dx.doi.org/10.1093/mnras/stx1286.

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Abstract X-ray observations of two metal-deficient luminous compact galaxies (LCG; SHOC 486 and SDSS J084220.94+115000.2) with properties similar to the so-called Green Pea galaxies were obtained using the Chandra X-ray Observatory. Green Pea galaxies are relatively small, compact (a few kpc across) galaxies that get their green colour from strong [O iii] λ5007 Å emission, an indicator of intense, recent star formation. These two galaxies were predicted to have the highest observed count rates, using the X-ray luminosity–star formation rate (LX–SFR) relation for X-ray binaries, from a statisti

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Nagase, Fumiaki. "Photoionized Plasmas in X-Ray Binary Pulsars: ASCA Observations." Symposium - International Astronomical Union 188 (1998): 101–4. http://dx.doi.org/10.1017/s0074180900114524.

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Massive X-ray binary pulsars have often evolved early-type companion stars which emanate strong stellar winds. X-rays emitted from the accreting neutron star irradiate and ionize the surrounding stellar wind, thus forming a photoionized sphere surrounding the neutron star. The photoionization structure of matter surrounding the neutron star was calculated by Hatchett and McCray (1977) and McCray et al. (1984), for Cen X-3 and Vela X-1 respectively.

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Watson, A. "ASTROPHYSICS:Z Mimics X-rays From Neutron Star." Science 286, no. 5447 (1999): 2059. http://dx.doi.org/10.1126/science.286.5447.2059.

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Kaspi, Victoria M. "The Neutron Star Zoo." Proceedings of the International Astronomical Union 13, S337 (2017): 3–8. http://dx.doi.org/10.1017/s1743921317010390.

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AbstractSince their discovery 50 years ago, neutron stars have continually astonished. From the first-discovered radio pulsars to the powerful “magnetars” that emit sudden bursts of X-rays and γ-rays, from the so-called Isolated Neutron Stars to Central Compact Objects, observational manifestations of neutron stars are surprisingly varied, with most properties totally unpredicted. The challenge is to cement an overarching physical theory of neutron stars and their birth properties that can explain this great diversity. Here I briefly survey the disparate neutron star classes, describe their pr

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Babel, J. "Diffusion, Winds and X-Rays from Magnetic Stars." Highlights of Astronomy 11, no. 2 (1998): 674–75. http://dx.doi.org/10.1017/s1539299600018426.

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AbstractWe propose a self-consistent approach of the CP star phenomenon and try to solve simultaneously the problems of abundance spots, wind and X-ray emission from these stars. We also discuss the periodic X-ray emission from the 07V star θ1 Orionis C and its link with Bp stars.

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Fabian, A. C., and P. A. Thomas. "X-Rays from Elliptical Galaxies." Symposium - International Astronomical Union 127 (1987): 155–65. http://dx.doi.org/10.1017/s0074180900185146.

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X-ray observations have shown that early-type galaxies contain a hot interstellar medium. This implies that the galaxies have a) a low supernova rate; b) high total gravitational binding masses and c) continuous star formation. Much of the gas in isolated galaxies is probably due to stellar mass-loss. The details of its behaviour are complex.

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Kumagai, S. "X-Rays and γ-Rays from SN 1987A". International Astronomical Union Colloquium 145 (1996): 173–81. http://dx.doi.org/10.1017/s0252921100008046.

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Theoretical light curves and spectra of X-rays and γ-rays from SN 1987A are calculated by the Monte Carlo method, based on a model built up from the early observations of neutrinos and optical light. Comparison of the predicted radiation with observational results obtained later confirms the radiation mechanism of supernovae: γ-rays are emitted in the decays of radioactive 56Co and X-rays are generated by the Compton degradation of these γ-rays. It also suggests that large scale mixing occurred and clumpy structure was formed inside the ejecta. These findings lead us to construct the model wit

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Wolk, Scott J., Ignazio Pillitteri, and Katja Poppenhaeger. "Observed effects of star-planet interaction." Proceedings of the International Astronomical Union 11, S320 (2015): 382–87. http://dx.doi.org/10.1017/s1743921316000272.

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AbstractSince soon after the discovery of hot Jupiters, it had been suspected that interaction of these massive bodies with their host stars could give rise to observable signals. We discuss the observational evidence for star-planet interactions (SPI) of tidal and magnetic origin observed in X-rays and FUV. Hot Jupiters can significantly impact the activity of their host stars through tidal and magnetic interaction, leading to either increased or decreased stellar activity – depending on the internal structure of the host star and the properties of the hosted planet. In HD 189733, X-ray and F

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Nomoto, Ken’ichi, and Sachiko Tsuruta. "Thermal Radiation from a Neutron Star in SN 1987A." International Astronomical Union Colloquium 108 (1988): 448–49. http://dx.doi.org/10.1017/s0252921100094367.

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The supernova 1987A in the Large Magellanic Cloud has provided a new opportunity to study the evolution of a young neutron star right after its birth. A proto-neutron star first cools down by emitting neutrinos that diffuse out of the interior within a minutes. After the neutron star becomes transparent to neutrinos, the neutron star core with > 1014 g cm−3 cools predominantly by Urca neutrino emission. However, the surface layers remain hot because it takes at least 100 years before the cooling waves from the central core reach the surface layers (Nomoto and Tsuruta 1981, 1986, 1987).From

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Thèses sur le sujet "X-rays: star"

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Sasaki, Manami. "X-rays tracing the star formation history of the Magellanic clouds." [S.l.] : [s.n.], 2001. http://deposit.ddb.de/cgi-bin/dokserv?idn=964798824.

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Sasaki, Manami. "X-rays tracing the star formation history of the Magellanic clouds." Diss., lmu, 2002. http://nbn-resolving.de/urn:nbn:de:bvb:19-4438.

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Güver, Tolga, Feryal Özel, Herman Marshall, Dimitrios Psaltis, Matteo Guainazzi, and Maria Díaz-Trigo. "SYSTEMATIC UNCERTAINTIES IN THE SPECTROSCOPIC MEASUREMENTS OF NEUTRON STAR MASSES AND RADII FROM THERMONUCLEAR X-RAY BURSTS. III. ABSOLUTE FLUX CALIBRATION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621974.

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Many techniques for measuring neutron star radii rely on absolute flux measurements in the X-rays. As a result, one of the fundamental uncertainties in these spectroscopic measurements arises from the absolute flux calibrations of the detectors being used. Using the stable X-ray burster, GS 1826-238, and its simultaneous observations by Chandra HETG/ACIS-S and RXTE/PCA as well as by XMM-Newton EPIC-pn and RXTE/PCA, we quantify the degree of uncertainty in the flux calibration by assessing the differences between the measured fluxes during bursts. We find that the RXTE/PCA and the Chandra grati

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Gregory, Scott G. "T Tauri stars : mass accretion and X-ray emission." Thesis, St Andrews, 2007. http://hdl.handle.net/10023/336.

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Igance, Richard. "Modeling X-ray Emission Line Profiles from Massive Star Winds - A Review." Digital Commons @ East Tennessee State University, 2016. https://dc.etsu.edu/etsu-works/2686.

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The Chandra and XMM-Newton X-ray telescopes have led to numerous advances in the study and understanding of astrophysical X-ray sources. Particularly important has been the much increased spectral resolution of modern X-ray instrumentation. Wind-broadened emission lines have been spectroscopically resolved for many massive stars. This contribution reviews approaches to the modeling of X-ray emission line profile shapes from single stars, including smooth winds, winds with clumping, optically thin versus thick lines, and the effect of a radius-dependent photoabsorption coefficient.

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Hubrig, S., M. Schöller, A. Kholtygin, et al. "New Multiwavelength Observations of the Of?p Star CPD -28◦ 2561." Digital Commons @ East Tennessee State University, 2015. https://dc.etsu.edu/etsu-works/6241.

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A rather strong mean longitudinal magnetic field of the order of a few hundred gauss was detected a few years ago in the Of?p star CPD −28° 2561 using FORS2 (FOcal Reducer low dispersion Spectrograph 2) low-resolution spectropolarimetric observations. In this work, we present additional low-resolution spectropolarimetric observations obtained during several weeks in 2013 December using FORS 2 mounted at the 8-m Antu telescope of the Very Large Telescope (VLT). These observations cover a little less than half of the stellar rotation period of 73.41 d mentioned in the literature. The behaviour o

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RIGOSELLI, MICHELA. "X-ray emission from the magnetic polar caps of old rotation-powered pulsars." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2020. http://hdl.handle.net/10281/277373.

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Le stelle di neutroni sono il risultato dell'evoluzione di stelle massive dopo l'esplosione di supernova. Il progetto di questa Tesi di PhD consiste nello studio dell'emissione di raggi X da parte di stelle di neutroni isolate di età superiore a 100000 anni. Sono stati analizzati dati provenienti dal satellite XMM-Newton (ESA). Per estrarre la miglior informazione possibile dai dati, ho implementato un metodo di maximum likelihood (ML) e l'ho utilizzato per estrarre spettri e profili pulsati di pulsar vecchie in banda X, che poi sono stati analizzati con raffinati di emissione. La Tesi è strut

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Leto, P., Corrado Trigilio, Lidia M. Oskinova, et al. "The Detection of Variable Radio Emission from the Fast Rotating Magnetic Hot B-Star HR 7355 and Evidence for Its X-Ray Aurorae." Digital Commons @ East Tennessee State University, 2017. https://dc.etsu.edu/etsu-works/2695.

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In this paper we investigate the multiwavelengths properties of the magnetic early B-type star HR7355. We present its radio light curves at several frequencies, taken with the Jansky Very Large Array, and X-ray spectra, taken with the XMM X-ray telescope. Modeling of the radio light curves for the Stokes I and V provides a quantitative analysis of the HR7355 magnetosphere. A comparison between HR7355 and a similar analysis for the Ap star CUVir, allows us to study how the different physical parameters of the two stars affect the structure of the respective magnetospheres where the non-thermal

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Leto, P., Courtney Trigilio, Lidia M. Oskinova, et al. "A Combined Multiwavelength VLA/ALMA/Chandra Study Unveils the Complex Magnetosphere of the B-Type Star HR5907." Digital Commons @ East Tennessee State University, 2018. https://dc.etsu.edu/etsu-works/2682.

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We present new radio/millimeter measurements of the hot magnetic star HR 5907 obtained with the VLA and ALMA interferometers. We find that HR 5907 is the most radio luminous early type star in the cm–mm band among those presently known. Its multi-wavelength radio light curves are strongly variable with an amplitude that increases with radio frequency. The radio emission can be explained by the populations of the non-thermal electrons accelerated in the current sheets on the outer border of the magnetosphere of this fast-rotating magnetic star. We classify HR 5907 as another member of the growi

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Oskinova, Lidia M., Richard Ignace, and D. P. Huenemoerder. "X-ray Diagnostics of Massive Star Winds." Digital Commons @ East Tennessee State University, 2016. https://dc.etsu.edu/etsu-works/2703.

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Observations with powerful X-ray telescopes, such as XMM-Newton and Chandra, significantly advance our understanding of massive stars. Nearly all early-type stars are X-ray sources. Studies of their X-ray emission provide important diagnostics of stellar winds. High-resolution X-ray spectra of O-type stars are well explained when stellar wind clumping is taking into account, providing further support to a modern picture of stellar winds as non-stationary, inhomogeneous outflows. X-ray variability is detected from such winds, on time scales likely associated with stellar rotation. High-resoluti

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Livres sur le sujet "X-rays: star"

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United States. National Aeronautics and Space Administration., ed. X-rays from the youngest stars. National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., ed. X-rays from the youngest stars. National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., ed. X-rays from the youngest stars. National Aeronautics and Space Administration, 1994.

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United States. National Aeronautics and Space Administration., ed. A deep PSPC observation of the Cyg OB2 association: Final report. National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. A deep PSPC observation of the Cyg OB2 association: Final report. National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. A deep PSPC observation of the Cyg OB2 association: Final report. National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. A deep PSPC observation of the Cyg OB2 association: Final report. National Aeronautics and Space Administration, 1995.

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Masayuki, Itoh, Nagase F. 1941-, and United States. National Aeronautics and Space Administration., eds. A search for X-ray evidence of a compact companion to the unusual Wolf-Rayet star HD 50896 (EZ CMa). Elsevier, 1998.

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Masayuki, Itoh, Nagase F. 1941-, and United States. National Aeronautics and Space Administration., eds. A search for X-ray evidence of a compact companion to the unusual Wolf-Rayet star HD 50896 (EZ CMa). Elsevier, 1998.

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United States. National Aeronautics and Space Administration., ed. An investigation of the largest flares in active cool star binaries with ALEXIS: Final report. National Aeronautics and Space Administration, 1998.

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Chapitres de livres sur le sujet "X-rays: star"

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White, Richard L., and Wan Chen. "Particle Acceleration, X-Rays, and Gamma-Rays from Winds." In Instability and Variability of Hot-Star Winds. Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0315-2_23.

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Tatischeff, V., A. Decourchelle, and G. Maurin. "Nonthermal X-Rays from Low-Energy Cosmic Rays in the Arches Cluster Region." In Cosmic Rays in Star-Forming Environments. Springer Berlin Heidelberg, 2013. http://dx.doi.org/10.1007/978-3-642-35410-6_31.

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Feigelson, Eric D. "MYStIX: Massive Young Stellar Cluster Study in Infrared and X-Rays." In The Labyrinth of Star Formation. Springer International Publishing, 2014. http://dx.doi.org/10.1007/978-3-319-03041-8_97.

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Montmerle, Thierry, and Nicolas Grosso. "X-Rays from Star-Forming Regions in the VLT Era." In The Origins of Stars and Planets: The VLT View. Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-40277-1_59.

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Hornsey, Richard. "Distant Scintillating Star: Starlight, X-rays, and Television, 1891–1908." In International Archives of the History of Ideas Archives internationales d'histoire des idées. Springer International Publishing, 2023. http://dx.doi.org/10.1007/978-3-031-40243-2_9.

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Macfarlane, J. J. "Effects of X-rays on the Ionization State of Be Star Winds." In Pulsation, Rotation and Mass Loss in Early-Type Stars. Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1030-3_51.

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Pollock, A. M. T., G. Tagliaferri, and R. Pallavicini. "X-rays from both components of the flare star binary Gliese 867." In Surface Inhomogeneities on Late-Type Stars. Springer Berlin Heidelberg, 1992. http://dx.doi.org/10.1007/3-540-55310-x_186.

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Bourke, T. L., S. J. Wolk, M. Vigil, and J. Alves. "The Massive Star Forming Region RCW 38 — from X-Rays to Molecular Gas." In Springer Proceedings in Physics. Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-642-18902-9_111.

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Schmitt, J. H. M. M., and B. Stelzer. "Nuclear Burning Stars." In The Universe in X-Rays. Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34412-4_10.

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Staubert, R. "Accreting Neutron Stars." In The Universe in X-Rays. Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34412-4_15.

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Actes de conférences sur le sujet "X-rays: star"

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Zhang, Wenhui, J. Lukas Dresselhaus, Holger Fleckenstein, et al. "Efficient hard X-ray projection imaging at a sub-10 nm resolution." In Computational Optical Sensing and Imaging. Optica Publishing Group, 2024. http://dx.doi.org/10.1364/cosi.2024.cth1b.4.

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A noise-robust sub-10 nanometer imaging resolution from a Siemens star sample was achieved, by ptychographically reconstructing projection holograms recorded at an effective magnification of more than 11,800 in the regime of hard X-rays.

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Robrade, J., J. H. M. M. Schmitt, and Eric Stempels. "Altair—the hottest ‘cool’ star in X-rays." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099190.

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Kholtygin, A., I. Yakunin, E. Ryspaeva, and D. Mokshin. "A nature of the X-ray and optical emission from gamma Cassiopeia stars." In Modern astronomy: from the Early Universe to exoplanets and black holes. Special Astrophysical Observatory of the Russian Academy of Sciences, 2024. https://doi.org/10.26119/vak2024.063.

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To test the origin of the X-ray and optical emission from the $\gamma$ Cas-type stars, we analyzed their optical spectra obtained on the 6-m telescope BTA, the 1.25-m telescope of the Crimean station of the State Astronomical Institute (SAI, Moscow), the 2.5-m telescope SAI25 of SAI, and the photometric TESS light curves. We compare the optical variability of the $\gamma$ Cas-type stars with variations of their X-ray luminosity. An overlap between the periods of line profile variations in the spectra of $\gamma$ Cas stars and the variations in their X-ray brightness allows us to assume that a

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Spaans, Marco, Aycin Aykutalp, John H. Wise, and Rowin Meijerink. "The effects of x-rays on star formation and black hole growth in young galaxies." In FIRST STARS IV – FROM HAYASHI TO THE FUTURE –. AIP, 2012. http://dx.doi.org/10.1063/1.4754342.

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Demina, Natalya. "DEVELOPMENT OF NEW METHODS OF AUTO- AND CROSS-CORRELATION ANALYSIS OF QUASI-STAR OBJECTS� X-RAYS INTENSITY." In 18th International Multidisciplinary Scientific GeoConference SGEM2018. Stef92 Technology, 2018. http://dx.doi.org/10.5593/sgem2018/6.1/s28.074.

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Trushkin, S., A. Shevchenko, N. Bursov, P. Tsybulev, and N. Nizhelsky. "Long-term multi-frequency studies of flaring activity from microquasars." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.196.

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The long-term monitoring at RATAN-600 of studies of bright X-ray binary stars in various ranges of the electromagneticspectrum, a search and detailed study of correlations between variable X-ray, radio and gamma radiation was carried out.It is a key point for understanding the formation of jet emissions from accreting matter onto a black hole (or neutron star).From April 2019 For a year, we began to use the multi-azimuth measurement mode on the Southern Sector antenna systemwith a ﬂat reﬂector, when 31 measurements of ﬂux densities at frequencies 4.7, 8.6, 15 and 30 GHz of several giant Cygnus

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Ryspaeva, E. B. "X-ray emission fromHerbig stars." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.42.

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The archived X-ray observations of 9 Ae/Be Herbig stars obtained on the XMM-Newton space observatory are analysed for checking the hypotheses of their X-rays formation. An analysis of the dependences of the X-ray radiation characteristics for Herbig stars on the parameters of the stars revealed a close relationship between the magnetic activity and the processes of generation of X-ray radiation from Herbig stars, as well as the possible presence of a non-thermal component of the X-ray spectra.

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Nagase, F. "Transient Be star binary systems." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434639.

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Blaes, Omer. "Coalescence of neutron star binaries." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.46017.

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Postnov, K., A. Kuranov, L. Yungelson, and M. Gil’fanov. "X-ray luminosity function of accreting neutron stars and black holes." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.114.

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We model X-ray luminosity functions (XLF) of accreting neutron stars and black holes in 10 35 ≤ L X ≤ 10 41 erg s −1range in star-forming galaxies and galaxies with the initial star formation burst. XLFs are obtained by combining a fastgeneration of compact object+normal star population using the binary population synthesis code BSE and calculation ofthe subsequent detailed binary evolution by the MESA code.

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Rapports d'organisations sur le sujet "X-rays: star"

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Nilsen, Joseph. X-ray Lasers: The evolution from Star Wars to the table-top. Office of Scientific and Technical Information (OSTI), 2020. http://dx.doi.org/10.2172/1759988.

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Tournear, Derek M. Non-Quiescent X-ray Emission from Neutron Stars and Black Holes. Office of Scientific and Technical Information (OSTI), 2003. http://dx.doi.org/10.2172/815297.

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Tournear, Derek M. X-ray Bursts in Neutron Star and Black Hole Binaries from USA Data: Detections and Upper Limits. Office of Scientific and Technical Information (OSTI), 2003. http://dx.doi.org/10.2172/813180.

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Sun, Yipeng. Design and Start-to-End Simulation of an X-Band RF Driven Hard X-Ray FEL with LCLS Injector. Office of Scientific and Technical Information (OSTI), 2012. http://dx.doi.org/10.2172/1049749.

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in't Zand, J. J. M., Christopher M. Malone, D. Altamirano, et al. The LOFT perspective on neutron star thermonuclear bursts: White paper in support of the mission concept of the large observatory for X-ray timing. Office of Scientific and Technical Information (OSTI), 2015. http://dx.doi.org/10.2172/1167485.

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X-ray diffraction analysis of cuttings from Happy Valley A-10, Happy Valley B-12, Kenai Beluga Unit 31-18, Ninilchik Unit G Oskolkoff 1, Ninilchik Unit G Oskolkoff 2, Ninilchik Unit G Oskolkoff 3, Ninilchik Unit G Oskolkoff 5, Ninilchik Unit G Oskolkoff 8, Star 1, Swanson River Unit 24-15, Swanson River Unit 32C-15, Swanson River Unit 34-10, and Swanson River Unit 34-16 wells. Alaska Division of Geological & Geophysical Surveys, 2017. http://dx.doi.org/10.14509/29810.

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