An Etymological Dictionary of Astronomy and Astrophysics

A configuration of magnetic field lines around a → magnetic null point resembling a cross. See also → O-point.

See also: X, the letter of alphabet whose shape evokes the configuration; → point.

A configuration of magnetic field lines around a → magnetic null point resembling a cross. See also → O-point.

See also: X, the letter of alphabet whose shape evokes the configuration; → point.

The → electromagnetic radiation with → wavelengths shorter than that of
→ ultraviolet radiation and greater than that of → gamma rays.

Typical X-rays have a wavelength ranging from 0.1 to 100 Å (0.01 to 10 → nanometers), corresponding to frequencies in the range 3 × 10¹⁶ to 3 × 10¹⁹ Hz and energies in the range 100 eV to 100 → keV.

X-rays are produced artificially when high-speed → electrons collide with a heavy metal target such as tungsten. Astrophysical sources of X-rays include → plasmas with → temperatures in the range 10⁶-10⁸ K, and deceleration process of rapidly moving charges upon interaction with matter
(→ bremsstrahlung). X-rays were discovered in 1895 by Wilhelm Röntgen, a German physics professor (→ roentgen). For this discovery he won the first Nobel prize in physics in 1901. See also: → soft X-rays, → hard X-rays.

See also: X stand for “unknown,” since Röntgen was not sure what they were; → ray.

The → electromagnetic radiation with → wavelengths shorter than that of
→ ultraviolet radiation and greater than that of → gamma rays.

Typical X-rays have a wavelength ranging from 0.1 to 100 Å (0.01 to 10 → nanometers), corresponding to frequencies in the range 3 × 10¹⁶ to 3 × 10¹⁹ Hz and energies in the range 100 eV to 100 → keV.

X-rays are produced artificially when high-speed → electrons collide with a heavy metal target such as tungsten. Astrophysical sources of X-rays include → plasmas with → temperatures in the range 10⁶-10⁸ K, and deceleration process of rapidly moving charges upon interaction with matter
(→ bremsstrahlung). X-rays were discovered in 1895 by Wilhelm Röntgen, a German physics professor (→ roentgen). For this discovery he won the first Nobel prize in physics in 1901. See also: → soft X-rays, → hard X-rays.

See also: X stand for “unknown,” since Röntgen was not sure what they were; → ray.

The study of celestial bodies using their X-ray emission. X-ray astronomy deals mainly with Galactic and extragalactic phenomena involving very high-energy photon emissions, covering a band of energies between 0.1 keV and 500 keV. The research field includes: → X-ray binaries,
→ cataclysmic variables, → pulsars, → black holes, → dark matter, → active galaxies, → galactic clusters → X-ray transients. The Earth’s atmosphere absorbs most X-rays coming from outer space. X-ray astronomy therefore requires observations to be done above atmosphere. The first rocket flight which successfully detected a cosmic source of X-ray emission was launched in 1962 by an American research group. A very bright source was detected that they named → Scorpius X-1.
Since then several dedicated X-ray astronomy satellites have been launched, among which: Uhuru, INTEGRAL, ROSAT, Rossi X-ray Timing Explorer (RXTE), → Chandra X-ray Observatory, and
→ XMM-Newton, which have contributed to important advances in astronomy.

See also: → X-ray; → astronomy.

The study of celestial bodies using their X-ray emission. X-ray astronomy deals mainly with Galactic and extragalactic phenomena involving very high-energy photon emissions, covering a band of energies between 0.1 keV and 500 keV. The research field includes: → X-ray binaries,
→ cataclysmic variables, → pulsars, → black holes, → dark matter, → active galaxies, → galactic clusters → X-ray transients. The Earth’s atmosphere absorbs most X-rays coming from outer space. X-ray astronomy therefore requires observations to be done above atmosphere. The first rocket flight which successfully detected a cosmic source of X-ray emission was launched in 1962 by an American research group. A very bright source was detected that they named → Scorpius X-1.
Since then several dedicated X-ray astronomy satellites have been launched, among which: Uhuru, INTEGRAL, ROSAT, Rossi X-ray Timing Explorer (RXTE), → Chandra X-ray Observatory, and
→ XMM-Newton, which have contributed to important advances in astronomy.

See also: → X-ray; → astronomy.

A diffuse background radiation in X-ray wavelengths which has several origins. At very low energies it is due to hot gas in the → Local Bubble. In the → soft X-ray energy band it comes from active galaxies at moderate redshifts. In → hard X-ray range the background is thought to be due to integrated emission from many → quasars at various redshifts.

See also: → X-ray; → background.

A diffuse background radiation in X-ray wavelengths which has several origins. At very low energies it is due to hot gas in the → Local Bubble. In the → soft X-ray energy band it comes from active galaxies at moderate redshifts. In → hard X-ray range the background is thought to be due to integrated emission from many → quasars at various redshifts.

See also: → X-ray; → background.

A binary star system where one of the stars has evolved and collapsed into an extremely dense body such as a → white dwarf,
a → neutron star, or a → black hole.
The enormous gravitational attraction of the massive, dense, but dim component pulls material from the brighter, less massive star in an → accretion disk. The gravitational potential energy of the accreted matter is converted to heat by → viscosity and eventually to high-energy photons in the X-ray range. The brightest X-ray binary is → Scorpius X-1.

See also: → X-ray; → binary.

A binary star system where one of the stars has evolved and collapsed into an extremely dense body such as a → white dwarf,
a → neutron star, or a → black hole.
The enormous gravitational attraction of the massive, dense, but dim component pulls material from the brighter, less massive star in an → accretion disk. The gravitational potential energy of the accreted matter is converted to heat by → viscosity and eventually to high-energy photons in the X-ray range. The brightest X-ray binary is → Scorpius X-1.

See also: → X-ray; → binary.

A rapid and intense surge of X-ray emission from some
sources. They often last less than one second followed by an
exponential decrease of typically a few seconds to a minute. Most X-ray bursts are believed to arise in → X-ray binary systems due to nuclear fusion of material accreted onto a compact companion.

See also: → X-ray; → burst.

A rapid and intense surge of X-ray emission from some
sources. They often last less than one second followed by an
exponential decrease of typically a few seconds to a minute. Most X-ray bursts are believed to arise in → X-ray binary systems due to nuclear fusion of material accreted onto a compact companion.

See also: → X-ray; → burst.

The diffraction of X-rays by the atoms or ions of a crystal. The wavelength of X-rays are comparable to the size of interatomic spacings in solids. Since the atoms in a crystal are arranged in a set of regular planes, crystals serve as three-dimensional diffraction gratings for X-rays. Planes of repetition within the atomic structure of the mineral diffract the X-rays. The pattern of diffraction thus obtained is therefore used to identify minerals by bombarding them with X-rays.

See also: → X-ray; → diffraction.

The diffraction of X-rays by the atoms or ions of a crystal. The wavelength of X-rays are comparable to the size of interatomic spacings in solids. Since the atoms in a crystal are arranged in a set of regular planes, crystals serve as three-dimensional diffraction gratings for X-rays. Planes of repetition within the atomic structure of the mineral diffract the X-rays. The pattern of diffraction thus obtained is therefore used to identify minerals by bombarding them with X-rays.

See also: → X-ray; → diffraction.

A member of a class of isolated, radio-silent → pulsars with peculiar properties. They show
a purely thermal spectrum at X-ray energies with no evidence for a high-energy, power-law component often detected in other → isolated neutron star classes. The X-ray luminosity is 10³¹ - 10³² erg s^-1, fully consistent with surface blackbody emission with temperatures ~ 40-100 eV and (radiation) radii of a few kilometers, as derived from X-ray spectral fits. With the only exception of RX J1856.5-3754, broad absorption features have been found in all XDINSs. These features have energies ~ 300 - 700 eV, equivalent widths of ~ 50 - 150 eV and, as in the case of RX J0720.4-3125, may be variable.

See also: → X-ray; → dim; → isolated; → neutron; → star.

A member of a class of isolated, radio-silent → pulsars with peculiar properties. They show
a purely thermal spectrum at X-ray energies with no evidence for a high-energy, power-law component often detected in other → isolated neutron star classes. The X-ray luminosity is 10³¹ - 10³² erg s^-1, fully consistent with surface blackbody emission with temperatures ~ 40-100 eV and (radiation) radii of a few kilometers, as derived from X-ray spectral fits. With the only exception of RX J1856.5-3754, broad absorption features have been found in all XDINSs. These features have energies ~ 300 - 700 eV, equivalent widths of ~ 50 - 150 eV and, as in the case of RX J0720.4-3125, may be variable.

See also: → X-ray; → dim; → isolated; → neutron; → star.

A region of → molecular clouds whose chemistry is affected by → X-rays from neighboring sources.

See also: → X-ray; → dissociation; → region.

A region of → molecular clouds whose chemistry is affected by → X-rays from neighboring sources.

See also: → X-ray; → dissociation; → region.

An → X-ray source that does not display emission → outbursts, in contrast to → X-ray transients.

See also: → X-ray; → persistent.

An → X-ray source that does not display emission → outbursts, in contrast to → X-ray transients.

See also: → X-ray; → persistent.

A regularly variable X-ray source in which the pulsation is associated with the rotation of a magnetized neutron star in an → X-ray binary. Periods range from a few seconds to a few minutes. Examples include Hercules X-1, Centaurus X-3, Cygnus X-3.

See also: → X-ray; → pulsar.

A regularly variable X-ray source in which the pulsation is associated with the rotation of a magnetized neutron star in an → X-ray binary. Periods range from a few seconds to a few minutes. Examples include Hercules X-1, Centaurus X-3, Cygnus X-3.

See also: → X-ray; → pulsar.

An astronomical object whose dominant mechanism of radiation is through X-ray emission. X-ray sources contain an extremely hot gas at temperatures from 10⁶ to 10⁸ K. They are generated by various physical processes involving high energies, such as accretion on to a compact object, shock waves from
supernovae, stellar winds, hot gas in stellar coronae, or hot spaces between galaxies in a cluster. The first celestial X-ray source, after the Sun, to be detected was → Scorpius X-1 by means of rocket flight (Giacconi et al. 1962).

See also: → X-ray; → source.

An astronomical object whose dominant mechanism of radiation is through X-ray emission. X-ray sources contain an extremely hot gas at temperatures from 10⁶ to 10⁸ K. They are generated by various physical processes involving high energies, such as accretion on to a compact object, shock waves from
supernovae, stellar winds, hot gas in stellar coronae, or hot spaces between galaxies in a cluster. The first celestial X-ray source, after the Sun, to be detected was → Scorpius X-1 by means of rocket flight (Giacconi et al. 1962).

See also: → X-ray; → source.

An instrument for producing an X-ray spectrum and measuring the wavelengths of its components.

See also: → X-ray; → spectrometer.

An instrument for producing an X-ray spectrum and measuring the wavelengths of its components.

See also: → X-ray; → spectrometer.

A telescope designed to focus X-rays from astronomical objects. X-ray telescopes function from orbital satellites because X-rays are absorbed by the Earth’s atmosphere. These telescopes require special techniques since the conventional methods used in optical and radio telescopes are not adequate. → grazing-incidence telescope; → Bragg angle.

See also: → X-ray; → telescope.

A telescope designed to focus X-rays from astronomical objects. X-ray telescopes function from orbital satellites because X-rays are absorbed by the Earth’s atmosphere. These telescopes require special techniques since the conventional methods used in optical and radio telescopes are not adequate. → grazing-incidence telescope; → Bragg angle.

See also: → X-ray; → telescope.

An → X-ray source that enhances its emission well above its usual level for a period typically longer than a week. Recurrences can be → periodic or → aperiodic, but there is no obvious correlation between recurrence time and the luminosity amplitude of the → outburst.

X-ray transients seem to be divided into two classes: those associated with → high-mass X-ray binary (HMXB) stars and those associated with → low-mass X-ray binary (LMXB) stars. The HMXBs contain a → neutron star or → black hole paired with a → massive star. Often, the stellar companion is a → Be star, Be star, which sometimes sheds material from its equatorial region. In these systems, the transient event is characterized by having more higher energy X-rays in the spectrum. The LMXBs contain a neutron star or black hole orbiting around a cooler, → low-mass star. These transient events often generate more lower-energy X-rays.

See also: → X-ray; → transient.

An → X-ray source that enhances its emission well above its usual level for a period typically longer than a week. Recurrences can be → periodic or → aperiodic, but there is no obvious correlation between recurrence time and the luminosity amplitude of the → outburst.

X-ray transients seem to be divided into two classes: those associated with → high-mass X-ray binary (HMXB) stars and those associated with → low-mass X-ray binary (LMXB) stars. The HMXBs contain a → neutron star or → black hole paired with a → massive star. Often, the stellar companion is a → Be star, Be star, which sometimes sheds material from its equatorial region. In these systems, the transient event is characterized by having more higher energy X-rays in the spectrum. The LMXBs contain a neutron star or black hole orbiting around a cooler, → low-mass star. These transient events often generate more lower-energy X-rays.

See also: → X-ray; → transient.

A → magnetocentrifugal model for → accretion and → outflow in → protostars, which considers the interaction between the → magnetosphere of a → young stellar object and an & rarr; accretion disk.
The model assumes that the → magnetic field originates from the protostar, and the outflow is driven from a small region near the inner edge of the disk, called X, where the inner disk corotates with the star (→ corotation radius). The accretion disk is → truncated in its central region, that is the disk does not extend to the protostar. The matter spiraling toward the protostar is either funneled by the magnetic field connecting the star to the disk, or blown outward under the effect of
→ centrifugal force.
The X-wind model is able to account for many observations in one fairly self-consistent model. The observations include time variable accretion/wind phenomena in → T Tauri stars, the slow rotation rates of T Tauri stars, protostellar X-ray activity, and a number of the properties of → bipolar jets and → molecular outflows (F. H. Shu et al., 2000, in Protostars and Planets IV, V. Mannings et al. (eds.),
Tucson: Univ. Arizona Press, 789).

See also: X, referring to a configuration of the magnetic field where the lines of force intersect with an “X” shape; → wind; → model.

A → magnetocentrifugal model for → accretion and → outflow in → protostars, which considers the interaction between the → magnetosphere of a → young stellar object and an & rarr; accretion disk.
The model assumes that the → magnetic field originates from the protostar, and the outflow is driven from a small region near the inner edge of the disk, called X, where the inner disk corotates with the star (→ corotation radius). The accretion disk is → truncated in its central region, that is the disk does not extend to the protostar. The matter spiraling toward the protostar is either funneled by the magnetic field connecting the star to the disk, or blown outward under the effect of
→ centrifugal force.
The X-wind model is able to account for many observations in one fairly self-consistent model. The observations include time variable accretion/wind phenomena in → T Tauri stars, the slow rotation rates of T Tauri stars, protostellar X-ray activity, and a number of the properties of → bipolar jets and → molecular outflows (F. H. Shu et al., 2000, in Protostars and Planets IV, V. Mannings et al. (eds.),
Tucson: Univ. Arizona Press, 789).

See also: X, referring to a configuration of the magnetic field where the lines of force intersect with an “X” shape; → wind; → model.