Relevant bibliographies by topics / X-rays: stars

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'X-rays: stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 10 March 2023

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Journal articles on the topic "X-rays: stars"

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Güdel, Manuel. "X–rays from stars." Philosophical Transactions of the Royal Society of London. Series A: Mathematical, Physical and Engineering Sciences 360, no. 1798 (July 30, 2002): 1935–49. http://dx.doi.org/10.1098/rsta.2002.1045.

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Petit, V., D. H. Cohen, Y. Nazé, M. Gagné, R. H. D. Townsend, M. A. Leutenegger, A. ud-Doula, S. P. Owocki, and G. A. Wade. "X-rays from magnetic massive OB stars." Proceedings of the International Astronomical Union 9, S302 (August 2013): 330–33. http://dx.doi.org/10.1017/s1743921314002427.

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AbstractThe magnetic activity of solar-type and low-mass stars is a well known source of coronal X-ray emission. At the other end of the main sequence, X-rays emission is instead associated with the powerful, radiatively driven winds of massive stars. Indeed, the intrinsically unstable line-driving mechanism of OB star winds gives rise to shock-heated, soft emission (~0.5 keV) distributed throughout the wind. Recently, the latest generation of spectropolarimetric instrumentation has uncovered a population of massive OB-stars hosting strong, organized magnetic fields. The magnetic characteristics of these stars are similar to the apparently fossil magnetic fields of the chemically peculiar ApBp stars. Magnetic channeling of these OB stars' strong winds leads to the formation of large-scale shock-heated magnetospheres, which can modify UV resonance lines, create complex distributions of cooled Halpha emitting material, and radiate hard (~2-5 keV) X-rays. This presentation summarizes our coordinated observational and modelling efforts to characterize the manifestation of these magnetospheres in the X-ray domain, providing an important contrast between the emission originating in shocks associated with the large-scale fossil fields of massive stars, and the X-rays associated with the activity of complex, dynamo-generated fields in lower-mass stars.
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Luna, G. J. M., J. L. Sokoloski, K. Mukai, and T. Nelson. "Symbiotic stars in X-rays." Astronomy & Astrophysics 559 (October 28, 2013): A6. http://dx.doi.org/10.1051/0004-6361/201220792.

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Ayres, Thomas R. "X‐Rays from Hybrid Stars." Astrophysical Journal 618, no. 1 (January 2005): 493–501. http://dx.doi.org/10.1086/425891.

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Cohen, David H. "X-ray Emission from O Stars." Proceedings of the International Astronomical Union 3, S250 (December 2007): 17–24. http://dx.doi.org/10.1017/s1743921308020309.

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AbstractYoung O stars are strong, hard, and variable X-ray sources; properties that strongly affect their circumstellar and galactic environments. After ≈ 1 Myr, these stars settle down to become steady sources of soft X-rays. I will use high-resolution X-ray spectroscopy and MHD modeling to show that young O stars like θ1 Ori C are well explained by the magnetically channeled wind shock scenario. After their magnetic fields dissipate, older O stars produce X-rays via shock heating in their unstable stellar winds. Here too I will use X-ray spectroscopy and numerical modeling to confirm this scenario. In addition to elucidating the nature and cause of the O star X-ray emission, modeling of the high-resolution X-ray spectra of O supergiants provides strong evidence that mass-loss rates of these O stars have been overestimated.
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Robrade, J. "eROSITA - Nearby Young Stars in X-rays." Proceedings of the International Astronomical Union 10, S314 (November 2015): 280–85. http://dx.doi.org/10.1017/s1743921315005943.

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AbstractX-ray surveys are well suited to detect, identify and study young stars based on their high levels of magnetic activity and thus X-ray brightness. The eROSITA instrument onboard the Spectrum-Roentgen-Gamma (SRG) satellite will perform an X-ray all-sky survey that surpasses existing data by a sensitivity increase of more than an order of magnitude. The 4 yr survey is expected to detect more than half a million stars and stellar systems in X-rays.
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Cassinelli, Joseph P., and David H. Cohen. "ROSAT Observations of B and Be Stars." Symposium - International Astronomical Union 162 (1994): 189–99. http://dx.doi.org/10.1017/s0074180900214824.

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We present results from a survey of X-ray emission properties of near main-sequence B stars, including several Be and β Cephei stars. The main conclusions of our survey are: 1) The X-rays are soft, probably because the shock velocity jumps are small since the terminal wind speeds are small. 2) A major fraction of the wind emission measure is hot, assuming wind theory estimates for the density distribution. A large fraction of the wind is not expected to be hot in current wind shock models. 3) A hard component is found to be present in τ Sco; possible causes are discussed. 4) For the Be stars, the X-rays emission is from a normal B-star wind that is coming from the poles as in the WCD model of Be stars. 5) None of the stars, including the β Cep stars, show noticeable variability in their X-rays. For the normal B stars we conclude from the lack of variability that the shocks are in the form of fragments in the wind instead of spherical shells. 6) Our observations suggest that all B stars are X-ray sources and that there is a basal amount of X-ray luminosity of about 10-8.5Lboi. The hot component in τ Sco and the high X-ray luminosity of B stars detected in the all-sky survey suggests that there is a source of X-ray emission in addition to wind shocks in some B stars.
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Nuñez, N. E., T. Nelson, K. Mukai, J. L. Sokoloski, and G. J. M. Luna. "SYMBIOTIC STARS IN X-RAYS. III.SUZAKUOBSERVATIONS." Astrophysical Journal 824, no. 1 (June 7, 2016): 23. http://dx.doi.org/10.3847/0004-637x/824/1/23.

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Hayakawa, Satio. "X-rays from accreting neutron stars." Physics Reports 121, no. 6 (May 1985): 317–406. http://dx.doi.org/10.1016/0370-1573(85)90053-5.

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Parker, Eugene N. "Why Do Stars Emit X Rays?" Physics Today 40, no. 7 (July 1987): 36–42. http://dx.doi.org/10.1063/1.881079.

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Dissertations / Theses on the topic "X-rays: stars"

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Medin, Zach, Marina von Steinkirch, Alan C. Calder, Christopher J. Fontes, Chris L. Fryer, and Aimee L. Hungerford. "MODEL ATMOSPHERES FOR X-RAY BURSTING NEUTRON STARS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/624031.

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The hydrogen and helium accreted by X-ray bursting neutron stars is periodically consumed in runaway thermonuclear reactions that cause the entire surface to glow brightly in X-rays for a few seconds. With models of the emission, the mass and radius of the neutron star can be inferred from the observations. By simultaneously probing neutron star masses and radii, X-ray bursts (XRBs) are one of the strongest diagnostics of the nature of matter at extremely high densities. Accurate determinations of these parameters are difficult, however, due to the highly non-ideal nature of the atmospheres where XRBs occur. Observations from X-ray telescopes such as RXTE and NuStar can potentially place strong constraints on nuclear matter once uncertainties in atmosphere models have been reduced. Here we discuss current progress on modeling atmospheres of X-ray bursting neutron stars and some of the challenges still to be overcome.
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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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Massa, Derek, Lidi Oskinova, Raman Prinja, and Richard Ignace. "Coordinated UV and X-Ray Spectroscopic Observations of the O-type Giant ξ Per: The Connection between X-Rays and Large-scale Wind Structure." Digital Commons @ East Tennessee State University, 2019. https://dc.etsu.edu/etsu-works/5501.

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We present new, contemporaneous Hubble Space Telescope STIS and XMM-Newton observations of the O7 III(n)((f)) star ξ Per. We supplement the new data with archival IUE spectra, to analyze the variability of the wind lines and X-ray flux of ξ Per. The variable wind of this star is known to have a 2.086-day periodicity. We use a simple, heuristic spot model that fits the low-velocity (near-surface) IUE wind line variability very well, to demonstrate that the low-velocity absorption in the new STIS spectra of N iv λ1718 and Si iv λ1402 vary with the same 2.086-day period. It is remarkable that the period and amplitude of the STIS data agree with those of the IUE spectra obtained 22 yr earlier. We also show that the time variability of the new XMM-Newton fluxes is also consistent with the 2.086-day period. Thus, our new, multiwavelength coordinated observations demonstrate that the mechanism that causes the UV wind line variability is also responsible for a significant fraction of the X-rays in single O stars. The sequence of events for the multiwavelength light-curve minima is Si iv λ1402, N iv λ1718, and X-ray flux, each separated by a phase of about 0.06 relative to the 2.086-day period. Analysis of the X-ray fluxes shows that they become softer as they weaken. This is contrary to expectations if the variability is caused by periodic excess absorption. Furthermore, the high-resolution X-ray spectra suggest that the individual emission lines at maximum are more strongly blueshifted. If we interpret the low-velocity wind line light curves in terms of our model, it implies that there are two bright regions, i.e., regions with less absorption, separated by 180°, on the surface of the star. We note that the presence and persistence of two spots separated by 180° suggest that a weak dipole magnetic field is responsible for the variability of the UV wind line absorption and X-ray flux in ξ Per.
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Kastner, Joel H., David A. Principe, Kristina Punzi, Beate Stelzer, Uma Gorti, Ilaria Pascucci, and Costanza Argiroffi. "M STARS IN THE TW HYA ASSOCIATION: STELLAR X-RAYS AND DISK DISSIPATION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621232.

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To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L-X) of M stars in the similar to 8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing L-X/L-bol with decreasing T-eff for TWA M stars, wherein the earliest-type (M0-M2) stars cluster near log(L-X/L-bol) approximate to -3.0 and then log(L-X/L-bol) decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.
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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 gratings measurements agree with each other within their formal uncertainties, increasing our confidence in these flux measurements. In contrast, XMM-Newton EPIC-pn measures 14.0 +/- 0.3% less flux than the RXTE/PCA. This is consistent with the previously reported discrepancy with the flux measurements of EPIC-pn, compared with EPIC MOS1, MOS2, and ACIS-S detectors. We also show that any intrinsic time-dependent systematic uncertainty that may exist in the calibration of the satellites has already been implicity taken into account in the neutron star radius measurements.
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Watson, Casey Richard. "The cosmological X-ray evolution of stars, AGN, and galaxies." The Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc_num=osu1148410557.

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González, Galán Ana. "Fundamental properties of High Mass X-ray Binaries." Doctoral thesis, Universidad de Alicante, 2014. http://hdl.handle.net/10045/41723.

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The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neutron stars) accreting material from the wind of their supergiant companions. The X-rays are produced in the interaction of the accreted material with the strong gravitational field of the neutron star that accelerates this material and heats it up to ~ 107 K. The study of HMXBs has strong implications in several areas of Physics and Astrophysics. They contain neutron stars whose study is essential to constrain the equation of state of nuclear dense matter, and provides insights on the astrophysical models of core collapse and Supernovae explosions. HMXBs considered as a population give information on the properties of the galaxy. In addition they are excellent test-beds to study accretion physics and outflows. The X-ray behaviour of these systems determines the class of system (classical HMXBs, Supergiant Fast X-ray Transients, Be/X-ray Binaries). The differences in the X-ray emission are supposed to be due to the different properties of the binary systems, such as the orbital properties, the magnetic field of the neutron star or the spectral type of the donor star. HMXBs in this thesis are wind-fed systems, therefore, the properties of the wind (which depend on the spectral type) and the interaction of this wind with the gravitational field of the compact object are key elements to understand the X-ray emission. Therefore, in this thesis an orbital solution for each target of study has been determined using optical spectra of the donor star. Moreover, to check if wind variability is related to the orbit of the binary system, analysis of Ha variations have been carried out. Furthermore, in the case of IGR J00370+6122 and XTE J1855-026 we have obtained an atmosphere model for each of the donor stars allowing us to characterise the atmospheres of these stars, and consequently to determine physical parameters such as the Teff or the log g. Finally publicly available X-ray light curves have been analysed to study the X-ray emission of the different sources against their orbital periods. As a general conclusion, it seems there is a continuum of properties of these systems more than a strict classification. A combination of factors, of which some of them could be unknown, might be the cause of their different X-ray flux behaviours. The outline of this thesis is as follows: the scientific context is given in Chapter 1 an overview of the analysis performed for each of the sources of study is presented in Chapter 2; Chapter 3 is dedicated to the description of a pipeline optimised for the reduction of FRODOSpec spectra of obscured red sources (donor stars of the targets of study); Chapters (4, 5 and 6) present the characterization of the four sources in this thesis, which are different kind of wind-fed systems; and finally general conclusions and future work are given in Chapter 7.
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Toalá, Jesus A., Lidia M. Oskinova, and Richard Ignace. "On the Absence of Non-thermal X-Ray Emission around Runaway O Stars." Digital Commons @ East Tennessee State University, 2017. https://dc.etsu.edu/etsu-works/2687.

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Theoretical models predict that the compressed interstellar medium around runaway O stars can produce high-energy non-thermal diffuse emission, in particular, non-thermal X-ray and γ-ray emission. So far, detection of non-thermal X-ray emission was claimed for only one runaway star, AE Aur. We present a search for non-thermal diffuse X-ray emission from bow shocks using archived XMM-Newton observations for a clean sample of six well-determined runaway O stars. We find that none of these objects present diffuse X-ray emission associated with their bow shocks, similarly to previous X-ray studies toward ζ Oph and BD+43°3654. We carefully investigated multi-wavelength observations of AE Aur and could not confirm previous findings of non-thermal X-rays. We conclude that so far there is no clear evidence of non-thermal extended emission in bow shocks around runaway O stars.
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Ignace, Richard, Z. Damrau, and K. T. Hole. "Variability in X-ray Line Ratios in Helium-Like Ions of Massive Stars: The Wind-Driven Case." Digital Commons @ East Tennessee State University, 2019. https://dc.etsu.edu/etsu-works/5500.

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Context. High spectral resolution and long exposure times are providing unprecedented levels of data quality of massive stars at X-ray wavelengths. Aims. A key diagnostic of the X-ray emitting plasma are the fir lines for He-like triplets. In particular, owing to radiative pumping effects, the forbidden-to-intercombination line luminosity ratio, R = f∕i, can be used to determine the proximity of the hot plasma to the UV-bright photospheres of massive stars. Moreover, the era of large observing programs additionally allows for investigation of line variability. Methods. This contribution is the second to explore how variability in the line ratio can provide new diagnostic information about distributed X-rays in a massive star wind. We focus on wind integration for total line luminosities, taking account of radiative pumping and stellar occultation. While the case of a variable stellar radiation field was explored in the first paper, the effects of wind variability are emphasized in this work. Results. We formulate an expression for the ratio of line luminosities f∕i that closely resembles the classic expression for the on-the-spot result. While there are many ways to drive variability in the line ratio, we use variable mass loss as an illustrative example for wind integration, particularly since this produces no variability for the on-the-spot case. The f∕i ratio can be significantly modulated owing to evolving wind properties. The extent of the variation depends on how the timescale for the wind flow compares to the timescale over which the line emissivities change. Conclusions. While a variety of factors can ellicit variable line ratios, a time-varying mass-loss rate serves to demonstrate the range of amplitude and phased-dependent behavior in f∕i line ratios. Importantly, we evaluate how variable mass loss might bias measures of f∕i. For observational exposures that are less than the timescale of variable mass loss, biased measures (relative to the time-averaged wind) can result; if exposures are long, the f∕i ratio is reflective of the time-averaged spherical wind.
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MAZZOLA, Simona Michela. "Accretion onto Neutron Stars: spectral and timing investigation of Low Mass X-ray Binaries." Doctoral thesis, Università degli Studi di Palermo, 2021. http://hdl.handle.net/10447/500712.

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Books on the topic "X-rays: stars"

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

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

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

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United States. National Aeronautics and Space Administration., ed. Investigation of X-Ray variability in highly active cool stars: Final report. [Washington, DC: National Aeronautics and Space Administration, 1989.

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Stern, Robert A. Coronal temperatures of unusually active K-Dwarf binary systems: Final report. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Stern, Robert A. Investigation of X-Ray variability in highly active cool stars: Final report. [Washington, DC: National Aeronautics and Space Administration, 1989.

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1959-, Greiner Jochen, ed. Supersoft X-ray sources: Proceedings of the international workshop held in Garching, Germany, 28 February-1 March 1996. Berlin: Springer, 1996.

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Q, Lamb Donald, Patterson Joseph, and North American Workshop on Cataclysmic Variables, (7th : 1983 : Cambridge, Mass.), eds. Cataclysmic variables and low-mass x-ray binaries: Proceedings of the 7th North American workshop held in Cambridge, Massachusetts, U.S.A., January 12-15, 1983. Dordrecht: Reidel, 1985.

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Q, Lamb Donald, and Patterson Joseph, eds. Cataclysmic variables and low-mass X-ray binaries: Proceedings of the 7th North American Workshop held in Cambridge, Massachusetts, U.S.A., January 12-15, 1983. Dordrecht: D. Reidel Pub. Co., 1985.

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United States. National Aeronautics and Space Administration., ed. Astro-D observations of flares: Detecting the impulsive phase : final report. Palo Alto, CA: Lockheed Martin Palo Alto Research Laboratory, 1995.

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Book chapters on the topic "X-rays: stars"

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Schmitt, J. H. M. M., and B. Stelzer. "Nuclear Burning Stars." In The Universe in X-Rays, 97–131. Berlin, Heidelberg: 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, 217–36. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34412-4_15.

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Becker, W., F. Haberl, and J. Trümper. "Pulsars and Isolated Neutron Stars." In The Universe in X-Rays, 183–216. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-34412-4_14.

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Mastichiadis, Apostolos. "X-Rays from a Possible Pulsar in Supernova 1987A." In Timing Neutron Stars, 305–15. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_26.

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Wood, Kent S. "Neutron Stars, X-Rays, and Gravitational Waves." In Cosmic Gamma Rays, Neutrinos, and Related Astrophysics, 609–16. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0921-2_42.

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Zavlin, Vyacheslav E. "Studying millisecond pulsars in X-rays." In Isolated Neutron Stars: From the Surface to the Interior, 297–307. Dordrecht: Springer Netherlands, 2007. http://dx.doi.org/10.1007/978-1-4020-5998-8_38.

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Greiner, J., M. Boër, P. Kahabka, C. Motch, and W. Voges. "Search for Quiescent X Rays from GRB Sources." In The Lives of the Neutron Stars, 519–22. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0159-2_49.

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Babel, J. "Diffusion, Winds and X-Rays from Magnetic Stars." In Highlights of Astronomy, 674–75. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-4778-1_20.

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Chiu, Hong-Yee. "Possible New X-Ray Sources: Soliton Stars." In Cosmic Gamma Rays, Neutrinos, and Related Astrophysics, 617–26. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0921-2_43.

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Shu, Frank H., and Hsien Shang. "Protostellar X-rays, Jets, and Bipolar Outflows." In Herbig-Haro Flows and the Birth of Low Mass Stars, 225–39. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5608-0_19.

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Conference papers on the topic "X-rays: stars"

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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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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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Rühling, U., C. Sandin, M. Steffen, D. Schönberner, W. R. Hamann, H. Todt, Klaus Werner, and T. Rauch. "Diffuse X-rays from PNe with WR-type central stars." In 17TH EUROPEAN WHITE DWARF WORKSHOP. AIP, 2010. http://dx.doi.org/10.1063/1.3527807.

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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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Holt, Stephen S. "Telescope systems for x-ray astronomy." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1987. http://dx.doi.org/10.1364/oam.1987.wp2.

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Because of the opacity of the atmosphere, x-ray astronomy must be conducted from space. Twenty-five years ago, the first detections of nonsolar x rays were made with simple proportional counters from sounding rockets. Collimated counters aboard rockets and satellites were used to follow up these discoveries, and more recently true x-ray telescopes have been used for the study of x rays from the cosmos. There are now thousands of cataloged x-ray sources ranging from nearby stars to distant quasars. The primary advantages afforded by telescopes for x-ray astronomy are twofold: direct imagery allows finer angular resolution than otherwise possible, and it also betters the sensitivity of the x-ray detectors via the minimization of nonsource background. The primary disadvantages are associated with the necessary grazing-incidence geometry: the effective focal length is limited by the actual telescope length, and the short-wavelength response is, therefore, sharply limited by the shallowness of the grazing angle. Examples are presented of important astronomical results that have been obtained from x-ray telescopes in space. Also presented are conceptual designs (and prototypical test results) from three different types of next-generation telescope for x-ray astronomy.
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Caballero, José A., and Eric Stempels. "Stars and brown dwarfs, spatial distribution, multiplicity, X-rays, discs, and the complete mass function of the σ Orionis cluster." 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/10.1063/1.3099266.

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Khangulyan, D. "On the formation of energy spectra of synchrotron X-rays and inverse Compton γ-rays in binary systems with luminous optical stars." In HIGH ENERGY GAMMA-RAY ASTRONOMY: 2nd International Symposium on High Energy Gamma-Ray Astronomy. AIP, 2005. http://dx.doi.org/10.1063/1.1878430.

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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 CygnusX-3 flares, SS433 [1] and GRS1915+105 bright flashes were carried out for 5–6 hours around the culmination of the source.In January 2020, Cyg X-3 switched to a hyper-soft X-ray state, the exit from which in early February led to the brightest theradio flash for the all history of its observations. The Cygnus X-3 flow density increased from 5 mJy to 20 Jy at a frequencyof 4.7 GHz and up to 22 Jy at 2.3 GHz in 2–3 days. In multi-azimuthal observations in the beginning phase, we registered alinear law of increase in the flux at times from 1 to 5 hours. Comparing the data of the space Gamma-ray telescopes (Swift,AGILE and Fermi) and the MAXI and NICER X-ray monitors on board the ISS, we found that flaring events from the radioto the Gamma-rays are interrelated, which is a reflection of the causal relationship of physical processes in the accretiondisk and in jet emissions. The spectral and time dependence of the evolution of flares allow us to model the synchrotronradiation of microquasars based on changes in the volume of jet emissions, the strength of their magnetic field and the modeof generation and absorption of radio radiation from relativistic electrons. Radio flares of the microquasar GRS1915+105,as a clear manifestation of a new jet activity, always have the character of a reaction to changes in the conditions forgenerating X-rays in the accretion disk (MAXI) and in the corona (Swift). We have studied in details periodic radio flaresfrom the X-ray binary with bright Gamma-ray radiation LSI+61d303 for more than 60 orbital periods. Undoubtedly, thenature of these flares changes dramatically depending on the known super-orbital 4.6-year period.
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Motch, C. "Isolated neutron stars discovered by ROSAT." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434638.

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Wheatley, Peter J. "The X-ray spectra of symbiotic stars." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434796.

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Reports on the topic "X-rays: stars"

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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), August 2003. http://dx.doi.org/10.2172/815297.

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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), December 2020. http://dx.doi.org/10.2172/1759988.

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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), August 2012. http://dx.doi.org/10.2172/1049749.

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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), February 2003. http://dx.doi.org/10.2172/813180.

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in't Zand, J. J. M., Christopher M. Malone, D. Altamirano, D. R. Ballantyne, S. Bhattacharyya, E. F. Brown, Y. Cavecchi, 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), January 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, November 2017. http://dx.doi.org/10.14509/29810.

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