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X-ray burster - перевод на русский
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[eksrei'bə:stə]
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![Model of the arrangement of water molecules in ice, revealing the [[hydrogen bond]]s (1) that hold the solid together.](https://commons.wikimedia.org/wiki/Special:FilePath/3D model hydrogen bonds in water.svg?width=200 "Model of the arrangement of water molecules in ice, revealing the [[hydrogen bond]]s (1) that hold the solid together.")
![The incoming beam (coming from upper left) causes each scatterer to re-radiate a small portion of its intensity as a spherical wave. If scatterers are arranged symmetrically with a separation ''d'', these spherical waves will be in sync (add constructively) only in directions where their path-length difference 2''d'' sin θ equals an integer multiple of the [[wavelength]] λ. In that case, part of the incoming beam is deflected by an angle 2θ, producing a ''reflection'' spot in the [[diffraction pattern]].](https://commons.wikimedia.org/wiki/Special:FilePath/Bragg diffraction 2.svg?width=200 "The incoming beam (coming from upper left) causes each scatterer to re-radiate a small portion of its intensity as a spherical wave. If scatterers are arranged symmetrically with a separation ''d'', these spherical waves will be in sync (add constructively) only in directions where their path-length difference 2''d'' sin θ equals an integer multiple of the [[wavelength]] λ. In that case, part of the incoming beam is deflected by an angle 2θ, producing a ''reflection'' spot in the [[diffraction pattern]].")
![tetrahedrally]] and held together by single [[covalent bond]]s, making it strong in all directions. By contrast, graphite is composed of stacked sheets. Within the sheet, the bonding is covalent and has hexagonal symmetry, but there are no covalent bonds between the sheets, making graphite easy to cleave into flakes.](https://commons.wikimedia.org/wiki/Special:FilePath/Diamond and graphite2.jpg?width=200 "tetrahedrally]] and held together by single [[covalent bond]]s, making it strong in all directions. By contrast, graphite is composed of stacked sheets. Within the sheet, the bonding is covalent and has hexagonal symmetry, but there are no covalent bonds between the sheets, making graphite easy to cleave into flakes.")
![backbone]] from its N-terminus to its C-terminus.](https://commons.wikimedia.org/wiki/Special:FilePath/Myoglobin.png?width=200 "backbone]] from its N-terminus to its C-terminus.")
![Rocknest]]", October 17, 2012).<ref name="NASA-20121030" />](https://commons.wikimedia.org/wiki/Special:FilePath/PIA16217-MarsCuriosityRover-1stXRayView-20121017.jpg?width=200 "Rocknest]]\", October 17, 2012).<ref name=\"NASA-20121030\" />")
![A protein crystal seen under a [[microscope]]. Crystals used in X-ray crystallography may be smaller than a millimeter across.](https://commons.wikimedia.org/wiki/Special:FilePath/Protein crystal.jpg?width=200 "A protein crystal seen under a [[microscope]]. Crystals used in X-ray crystallography may be smaller than a millimeter across.")
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X-ray bursters are one class of X-ray binary stars exhibiting X-ray bursts, periodic and rapid increases in luminosity (typically a factor of 10 or greater) that peak in the X-ray region of the electromagnetic spectrum. These astrophysical systems are composed of an accreting neutron star and a main sequence companion 'donor' star. There are two types of X-ray bursts, designated I and II. Type I bursts are caused by thermonuclear runaway, while type II arise from the release of gravitational (potential) energy liberated through accretion. For type I (thermonuclear) bursts, the mass transferred from the donor star accumulates on the surface of the neutron star until it ignites and fuses in a burst, producing X-rays. The behaviour of X-ray bursters is similar to the behaviour of recurrent novae. In the latter case the compact object is a white dwarf that accretes hydrogen that finally undergoes explosive burning.
The compact object of the broader class of X-ray binaries is either a neutron star or a black hole; however, with the emission of an X-ray burst, the compact object can immediately be classified as a neutron star, since black holes do not have a surface and all of the accreting material disappears past the event horizon. X-ray binaries hosting a neutron star can be further subdivided based on the mass of the donor star; either a high mass (above 10 solar masses (M☉)) or low mass (less than 1 M☉) X-ray binary, abbreviated as HMXB and LMXB, respectively.
X-ray bursts typically exhibit a sharp rise time (1–10 seconds) followed by spectral softening (a property of cooling black bodies). Individual burst energetics are characterized by an integrated flux of 1032–1033 joules, compared to the steady luminosity which is of the order 1030 W for steady accretion onto a neutron star. As such the ratio α of the burst flux to the persistent flux ranges from 10 to 1000 but is typically on the order of 100. The X-ray bursts emitted from most of these systems recur on timescales ranging from hours to days, although more extended recurrence times are exhibited in some systems, and weak bursts with recurrence times between 5–20 minutes have yet to be explained but are observed in some less usual cases. The abbreviation XRB can refer either to the object (X-ray burster) or to the associated emission (X-ray burst).
