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Journal articles on the topic 'X-ray astronomy'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

MURAKAMI, Toshio. "X-ray Astronomy." Journal of the Visualization Society of Japan 15, no. 59 (1995): 259–64. http://dx.doi.org/10.3154/jvs.15.59_259.

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2

Patchett, B. E. "X-ray astronomy." Contemporary Physics 30, no. 2 (1989): 77–88. http://dx.doi.org/10.1080/00107518908225508.

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3

Coats, Glenn S., and Richard B. Gunderman. "X-Ray Astronomy." Journal of the American College of Radiology 9, no. 1 (2012): 3–6. http://dx.doi.org/10.1016/j.jacr.2011.08.013.

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4

Grenier, Isabelle A., та Philippe Laurent. "X-ray and γ-ray astronomy". Europhysics News 32, № 6 (2001): 218–20. http://dx.doi.org/10.1051/epn:2001606.

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5

Serio, Salvatore, and Luigi Stella. "X‐Ray Astronomy 2000." Publications of the Astronomical Society of the Pacific 113, no. 786 (2001): 1022–23. http://dx.doi.org/10.1086/322913.

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6

Bradt, Hale V. D., Takaya Ohashi, and Kenneth A. Pounds. "X-Ray Astronomy Missions." Annual Review of Astronomy and Astrophysics 30, no. 1 (1992): 391–427. http://dx.doi.org/10.1146/annurev.aa.30.090192.002135.

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7

Pounds, K. A. "2. X-Ray Astronomy." Transactions of the International Astronomical Union 19, no. 1 (1985): 616–25. http://dx.doi.org/10.1017/s0251107x00006660.

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The period leading up to the last IAU General Assembly was dominated in X-ray Astronomy by the results from the Einstein Observatory. This first application of a large, satellite-borne, high resolution X-ray telescope to the study of cosmic sources had led, by the end of orbital operation in April 1981, to the detection of X-ray fluxes from a wide variety of astronomical objects and the full maturing of X-ray Astronomy. During the past three years a strong scientific output has continued to flow from the analysis of the more than 5600 separate Einstein observations, many of which are now widel

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8

Pounds, K. A. "2. X-Ray Astronomy." Transactions of the International Astronomical Union 20, no. 01 (1988): 602–7. http://dx.doi.org/10.1017/s0251107x00007410.

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X-ray astronomy has continued to flourish in the three years covered by the present report (to June 1987) despite the continuing scarcity of new missions. The European EXOSAT has probably made the greatest impact during this period, carrying out over 2000 separate observations up to it’s loss of attitude control in April 1986. A major reason for the success of EXOSAT was the unusual spacecraft orbit which provided uniquely long source exposures, uninterrupted by Earth occultation, of up to 70 hours duration. The continuous light curves of many galactic and extragalactic sources have proved par

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9

Schmitt, J. H. M. M. "Stellar X-ray astronomy." Advances in Space Research 10, no. 2 (1990): 115–24. http://dx.doi.org/10.1016/0273-1177(90)90129-n.

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10

Gursky, H. "ASTRONOMY: X-ray Astronomy-40 Years on." Science 297, no. 5586 (2002): 1485–86. http://dx.doi.org/10.1126/science.1075482.

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11

White, Nicholas E. "Next-Generation X-Ray Astronomy." Proceedings of the International Astronomical Union 7, S285 (2011): 159–64. http://dx.doi.org/10.1017/s174392131200052x.

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AbstractThis review of future timing capabilities in X-ray astronomy includes missions in implementation (astro-h, gems, srg and astrosat), those under study (currently nicer, athena and loft), and new technologies that may be the seeds for future missions, such as lobster-eye optics. Those missions and technologies will offer exciting new capabilities that will take X-ray Astronomy into a new generation of achievements.

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12

MAKINO, Fumiyoshi. "X-ray astronomy satellite "Ginga"." Journal of the Japan Society for Precision Engineering 54, no. 5 (1988): 860–64. http://dx.doi.org/10.2493/jjspe.54.860.

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13

Koyama, Katsuji. "X-Ray Astronomy: The Present." TRENDS IN THE SCIENCES 3, no. 5 (1998): 17–20. http://dx.doi.org/10.5363/tits.3.5_17.

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14

Makino, F. "X-Ray Astronomy Satellite Ginga." International Astronomical Union Colloquium 123 (1990): 41–48. http://dx.doi.org/10.1017/s0252921100076880.

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AbstractThe X-ray astronomy satellite Ginga carries three scientific instruments, the Large Area proportional Counters (LAC), All Sky X-ray Monitor (ASM) and Gamma-ray Burst Detector (GBD). The LAC is the main instrument with an effective area of 4000 cm2 giving it the highest sensitivity to hard X-rays so far achieved. Ginga observed about 250 targets up to the end of 1989.

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15

Singh, Kulinder Pal. "Techniques in X-ray astronomy." Resonance 10, no. 7 (2005): 8–20. http://dx.doi.org/10.1007/bf02867103.

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16

Ramsey, Brian D., Robert A. Austin, and Rudolf Decher. "Instrumentation for X-ray astronomy." Space Science Reviews 69, no. 1-2 (1994): 139–204. http://dx.doi.org/10.1007/bf00756035.

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17

Elvis, Martin. "X-ray astronomy in 2019." Nature Astronomy 4, no. 1 (2019): 23–25. http://dx.doi.org/10.1038/s41550-019-0937-2.

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18

Singh, Kulinder Pal. "Techniques in X-ray astronomy." Resonance 10, no. 6 (2005): 15–23. http://dx.doi.org/10.1007/bf02895791.

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19

Tanaka, Yasuo. "X-Ray Astronomy Satellite Tenma." Publications of the Astronomical Society of Japan 36, no. 4 (1985): 641–58. https://doi.org/10.1093/pasj/36.4.641.

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Abstract Instruments and performance of the X-ray astronomy satellite Tenma are described. Tenma is a spin-stabilized satellite orbiting along a circle of about 500-km altitude and an inclination of 31°.5. Gas scintillation proportional counters with a large effective area covering the energy range 2–60 keV provide good-quality spectral and temporal X-ray data. A one-dimensional focusing telescope cover the lower energy range 0.1–2 keV. A wide sky region around the spin axis is continuously monitored by a transient source monitor. A small background monitor which also serves the gamma-ray burs

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20

Pounds, Ken. "X-ray UK." Astronomy & Geophysics 61, no. 1 (2020): 1.32–1.37. http://dx.doi.org/10.1093/astrogeo/ataa010.

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21

Tanaka, Yasuo. "Recent Advances in X-Ray Astronomy." Highlights of Astronomy 10 (1995): 3–16. http://dx.doi.org/10.1017/s1539299600010327.

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X-ray astronomy was born in June 1962 with a totally unexpected discovery of a bright X-ray source (presently known as Sco X-1) in a historic rocket flight conducted by Riccardo Giacconi, Herb Gursky, Frank Paolini and late Bruno Rossi. In the last 30 years, astronomy through the newly opened window has made a dramatic expansion.The universe contains enormously rich varieties which had been left unexplored until recent times. From 40’s through 60’s, new wavelength windows, radio, infrared and X-rays successively opened. As a result, the presence of objects and regions distributed over an extre

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22

Mitsuda, Kazuhisa. "TES X-ray microcalorimeters for X-ray astronomy and material analysis." Physica C: Superconductivity and its Applications 530 (November 2016): 93–97. http://dx.doi.org/10.1016/j.physc.2016.03.018.

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23

Biggin, Susan. "Astronomy: X-ray satellite takes off." Physics World 9, no. 6 (1996): 13. http://dx.doi.org/10.1088/2058-7058/9/6/15.

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24

Rich, Vera. "X-ray astronomy: British–Soviet collaboration." Nature 324, no. 6093 (1986): 101. http://dx.doi.org/10.1038/324101c0.

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25

Fabian, A. C. "Astronomy: First X-ray-ionized nebula." Nature 322, no. 6079 (1986): 496. http://dx.doi.org/10.1038/322496a0.

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26

Tanaka, Y. "Recent Advances of X-ray Astronomy." Science 263, no. 5143 (1994): 42–44. http://dx.doi.org/10.1126/science.263.5143.42.

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27

Pounds, Ken. "X-ray astronomy and Eddington winds." Astronomy & Geophysics 58, no. 6 (2017): 6.29–6.34. http://dx.doi.org/10.1093/astrogeo/atx215.

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28

Wilkes, Belinda J. "Chandra's revolution in X-ray astronomy." Astronomy & Geophysics 60, no. 6 (2019): 6.19–6.25. http://dx.doi.org/10.1093/astrogeo/atz191.

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29

Tucker, W. H. "The History of X-Ray Astronomy." Publications of the Astronomical Society of the Pacific 101 (October 1989): 889. http://dx.doi.org/10.1086/132597.

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30

Taylor, B. G., and A. Peacock. "ESA’s X-Ray Astronomy Mission, XMM." International Astronomical Union Colloquium 123 (1990): 129–40. http://dx.doi.org/10.1017/s0252921100076971.

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AbstractESA’s X-ray Astronomy Mission, XMM, scheduled for launch in 1998, is the second of four cornerstones of ESA’s long term science program Horizon 2000. Covering the range from about 0.1 to 10 keV, it will provide a high throughput of 5000 cm2 at 7 keV with three independant telescopes, and have a spatial resolution better than 30 arcsec. Broadband spectrophotometry is provided by CCD cameras while reflection gratings provide medium resolution spectroscopy (resolving power of about 400) in the range 0.3–3 keV. Long uninterrupted observations will be made from the 24 hr period, highly ecce

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31

Dean, A. J. "Hard X-ray astronomy from balloons." Advances in Space Research 5, no. 1 (1985): 93–103. http://dx.doi.org/10.1016/0273-1177(85)90433-8.

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32

Giacconi, Riccardo. "The Dawn of X-Ray Astronomy." International Journal of Modern Physics A 18, no. 18 (2003): 3127–49. http://dx.doi.org/10.1142/s0217751x03016112.

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33

Andersson, H., T. Andersson, J. Heino, et al. "Gem detectors for X-ray astronomy." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 513, no. 1-2 (2003): 155–58. http://dx.doi.org/10.1016/j.nima.2003.08.022.

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34

Li, T. P. "Imaging in Hard X-ray Astronomy." Symposium - International Astronomical Union 214 (2003): 70–83. http://dx.doi.org/10.1017/s0074180900194173.

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The energy range of hard X-rays is a key waveband to the study of high energy processes in celestial objects, but still remains poorly explored. In contrast to direct imaging methods used in the low energy X-ray and high energy gamma-ray bands, currently imaging in the hard X-ray band is mainly achieved through various modulation techniques. A new inversion technique, the direct demodulation method, has been developed since early 90s. with this technique, wide field and high resolution images can be derived from scanning data of a simple collimated detector. The feasibility of this technique h

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35

Butler, R. C. "The X-ray Astronomy Satellite SAX." International Astronomical Union Colloquium 115 (1990): 302–6. http://dx.doi.org/10.1017/s0252921100012501.

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AbstractThe SAX satellite is forseen for launch at the end of 1992 to study the X-ray emission from galactic and extra-galactic sources in the energy range 0.1-200 keV. The payload consists of four concentrator/spectrometer systems (3 units 1-10keV, 1 unit 0.1-10keV), a high pressure gas scintillation proportional counter (3-120keV), a phoswich scintillation counter (15-200keV), and two wide field cameras (2-30keV). Together these instruments will perform the following:- - Broad band spectroscopy (E/ΔE=12) in the energy range 0.1-10 keV with imaging resolution of 1 arcmin- Continuum and cyclot

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36

Holt, Stephen S. "Thermal Detectors for X-ray Astronomy." International Astronomical Union Colloquium 115 (1990): 346–56. http://dx.doi.org/10.1017/s0252921100012562.

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AbstractSpectroscopy is traditionally characterized by the sacrifice of quantum efficiency for high spectral resolution. Since X-ray astronomy is a photon-limited discipline, the choice between high resolution for very few sources versus much lower resolution for many more has not always been an easy one. The development of new thermal detectors offers the opportunity to “have one’s cake and eat it, too.”

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37

MARSHALL, E. "X-Ray Astronomy: The Unkindest Cut." Science 254, no. 5031 (1991): 508–10. http://dx.doi.org/10.1126/science.254.5031.508.

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38

Elvis, Martin. "'Plan B' for X-ray astronomy." Nature 472, no. 7344 (2011): 418. http://dx.doi.org/10.1038/472418b.

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39

Inoue, H. "The X-ray astronomy satellite “ASCA”." Experimental Astronomy 4, no. 1 (1993): 1–10. http://dx.doi.org/10.1007/bf01581810.

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40

Perola, G. C. "The X-ray astronomy mission sax." Advances in Space Research 10, no. 2 (1990): 287–95. http://dx.doi.org/10.1016/0273-1177(90)90153-q.

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41

Gorenstein, Paul. "Focusing X-Ray Optics for Astronomy." X-Ray Optics and Instrumentation 2010 (December 27, 2010): 1–19. http://dx.doi.org/10.1155/2010/109740.

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Focusing X-ray telescopes have been the most important factor in X-ray astronomy’s ascent to equality with optical and radio astronomy. They are the prime tool for studying thermal emission from very high temperature regions, non-thermal synchrotron radiation from very high energy particles in magnetic fields and inverse Compton scattering of lower energy photons into the X-ray band. Four missions with focusing grazing incidence X-ray telescopes based upon the Wolter 1 geometry are currently operating in space within the 0.2 to 10 keV band. Two observatory class missions have been operating si

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42

Gorenstein, Paul. "X-ray astronomy from the moon." Advances in Space Research 14, no. 6 (1994): 61–68. http://dx.doi.org/10.1016/0273-1177(94)90007-8.

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43

Tanaka, Yasuo, Hajime Inoue, and Stephen S. Holt. "The X-Ray Astronomy Satellite ASCA." Publications of the Astronomical Society of Japan 46, no. 3 (1994): L37—L41. https://doi.org/10.1093/pasj/46.3.37.

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Abstract ASCA is a high-throughput X-ray astronomy observatory which is capable of simultaneous imaging and spectroscopic observations over a wide energy range 0.5–10 keV. The scientific capabilities of ASCA and some aspects related to its operation and observations are briefly described.

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44

Brickhouse, Nancy S. "Atomic Data Needs for X-ray Astronomy." Highlights of Astronomy 12 (2002): 82–83. http://dx.doi.org/10.1017/s1539299600012909.

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AbstractWith the launches of the Chandra X-ray Observatory and XMM-Newton, high resolution X-ray spectra of cosmic sources are broadening our understanding of the physical conditions, such as temperature, density, ionization state, and elemental abundances. X-ray emitting astrophysical plasmas can be generally classified by their dominant ionization mechanism, either collisional ionization or X-ray photoionization. The atomic data needs are significantly different for these two cases; however, for both cases it is important that we identify robust and accurate diagnostics and that we verify co

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45

Cash, Webster. "X-ray Interferometry." Symposium - International Astronomical Union 205 (2001): 457–62. http://dx.doi.org/10.1017/s0074180900221761.

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X-rays have tremendous potential for imaging at the highest angular resulution. The high surface brightness of many x-ray sources will reveal angular scales heretofore thought unreachable. The short wavelengths make instrumentation compact and baselines short. We discuss how practical x-ray interferometers can be built for astronomy using existing technology. We describe the Maxim Pathfinder and Maxim missions which will achieve 100 and 0.1 micro-arcsecond imaging respectively. The science to be tackled with resolution of up to one million times that of HST will be outlined, with emphasis on e

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46

Blamire, Mark. "Superconducting detectors target soft X-ray astronomy." Physics World 6, no. 7 (1993): 25–26. http://dx.doi.org/10.1088/2058-7058/6/7/30.

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47

Gorenstein, Paul. "Grazing incidence telescopes for x-ray astronomy." Optical Engineering 51, no. 1 (2012): 011010. http://dx.doi.org/10.1117/1.oe.51.1.011010.

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48

Takahashi, Tadayuki, Motohide Kokubun, Kazuhisa Mitsuda, et al. "Hitomi (ASTRO-H) X-ray Astronomy Satellite." Journal of Astronomical Telescopes, Instruments, and Systems 4, no. 02 (2018): 1. http://dx.doi.org/10.1117/1.jatis.4.2.021402.

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49

Glanz, J. "Astronomy: Adding Depth to X-ray Maps." Science 271, no. 5251 (1996): 908. http://dx.doi.org/10.1126/science.271.5251.908.

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50

Carstairs, Ian. "X-ray astronomy in the new millennium." Astronomy and Geophysics 43, no. 2 (2002): 2.27–2.28. http://dx.doi.org/10.1046/j.1468-4004.2002.43227.x.

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