An Etymological Dictionary of Astronomy and Astrophysics

Having considerable or great extent from side to side; broad. → wide binary, → wide field.

Etymology (EN): From M.E., from O.E. wid; akin to Du. wijd, Ger. weit, Old Norse vithr.

Etymology (PE): Bozorg, → large.
Gošâd, gošâdé “opened; ample, broad,” from gošudan “to open up, to loose,” → resolve.

Having considerable or great extent from side to side; broad. → wide binary, → wide field.

Etymology (EN): From M.E., from O.E. wid; akin to Du. wijd, Ger. weit, Old Norse vithr.

Etymology (PE): Bozorg, → large.
Gošâd, gošâdé “opened; ample, broad,” from gošudan “to open up, to loose,” → resolve.

An international collaboration, more accurately named SuperWASP, led by the United Kingdom, that aims at detecting → extrasolar planets by means of the → transit method.

SuperWASP consists of two robotic observatories that operate continuously all year around, providing coverage of the sky in both hemispheres. The first, SuperWASP-North, is located on the island of La Palma. The second, SuperWASP-South, is located at the site of the South African Astronomical Observatory (SAAO). The observatories each consist of eight wide-angle cameras that simultaneously monitor the sky for → planetary transit events. Using the array of cameras makes it possible to monitor millions of stars simultaneously at an → apparent visual magnitude from about 7 to 13.

See also: → wide; → angle; → search; → planet.

An international collaboration, more accurately named SuperWASP, led by the United Kingdom, that aims at detecting → extrasolar planets by means of the → transit method.

SuperWASP consists of two robotic observatories that operate continuously all year around, providing coverage of the sky in both hemispheres. The first, SuperWASP-North, is located on the island of La Palma. The second, SuperWASP-South, is located at the site of the South African Astronomical Observatory (SAAO). The observatories each consist of eight wide-angle cameras that simultaneously monitor the sky for → planetary transit events. Using the array of cameras makes it possible to monitor millions of stars simultaneously at an → apparent visual magnitude from about 7 to 13.

See also: → wide; → angle; → search; → planet.

A binary system with semi-major axis as large as 10,000 → astronomical units.

See also: → wide; → binary.

A binary system with semi-major axis as large as 10,000 → astronomical units.

See also: → wide; → binary.

A telescope → field of view which covers a relatively large → angular area on the sky.

See also: → wide; → field.

A telescope → field of view which covers a relatively large → angular area on the sky.

See also: → wide; → field.

A → NASA infrared astronomical → space telescope launched in December 2009 to carry out an → all-sky survey from 3 to 22 → microns. With its 40-cm → telescope telescope and → infrared cameras, WISE aimed at a wide variety of studies ranging from the evolution of → protoplanetary disks to the history of → star formation in normal galaxies. In early October 2010, after completing its prime science mission, the spacecraft ran out of → coolant that keeps its instrumentation cold. However, two of its four infrared cameras remained operational. Hence,
NASA extended the NEOWISE portion of the WISE mission by four months, with the primary purpose of hunting for more → asteroids and → comets,
and to finish one complete scan of the main → asteroid belt. In August 2013, the WISE telescope’s mission was extended for more three years to search for asteroids that could collide with Earth.

See also: → wide field; → infrared; → survey; → explorer.

A → NASA infrared astronomical → space telescope launched in December 2009 to carry out an → all-sky survey from 3 to 22 → microns. With its 40-cm → telescope telescope and → infrared cameras, WISE aimed at a wide variety of studies ranging from the evolution of → protoplanetary disks to the history of → star formation in normal galaxies. In early October 2010, after completing its prime science mission, the spacecraft ran out of → coolant that keeps its instrumentation cold. However, two of its four infrared cameras remained operational. Hence,
NASA extended the NEOWISE portion of the WISE mission by four months, with the primary purpose of hunting for more → asteroids and → comets,
and to finish one complete scan of the main → asteroid belt. In August 2013, the WISE telescope’s mission was extended for more three years to search for asteroids that could collide with Earth.

See also: → wide field; → infrared; → survey; → explorer.

An extent from side to side; breadth; wideness.
→ bandwidth; → beamwidth; → equivalent width; → slitwidth.

Etymology (EN): From wide, M.E., O.E. wid (cf. Du. wijd, O.H.G. wit, Ger. weit) + -th a suffix forming nouns of quality or condition, M.E. -th(e); O.E. -thu, -th.

Etymology (PE): Pahnâ, from pahn “wide, broad,” from Mid.Pers. pah(a)n; Av. paθana- “broad, wide, spacious.”

An extent from side to side; breadth; wideness.
→ bandwidth; → beamwidth; → equivalent width; → slitwidth.

Etymology (EN): From wide, M.E., O.E. wid (cf. Du. wijd, O.H.G. wit, Ger. weit) + -th a suffix forming nouns of quality or condition, M.E. -th(e); O.E. -thu, -th.

Etymology (PE): Pahnâ, from pahn “wide, broad,” from Mid.Pers. pah(a)n; Av. paθana- “broad, wide, spacious.”

For all metals the ratio of the → thermal conductivity, κ, to the → electrical conductivity,
σ, is directly proportional to the absolute temperature: K/σ = (1/3)(πk/e)²T, where k is → Boltzmann’s constant and e the electron’s charge.

See also: Named after the German physicists Gustav Heinrich Wiedemann (1826-1899) and Rudolph Franz (1826-1902); → law.

For all metals the ratio of the → thermal conductivity, κ, to the → electrical conductivity,
σ, is directly proportional to the absolute temperature: K/σ = (1/3)(πk/e)²T, where k is → Boltzmann’s constant and e the electron’s charge.

See also: Named after the German physicists Gustav Heinrich Wiedemann (1826-1899) and Rudolph Franz (1826-1902); → law.

The wavelength corresponding to the maximum emissive power of a black body is inversely proportional to the absolute temperature of the body: λ_max.T = 0.29 cm-deg. Wien’s law explains why objects of different temperature emit spectra that peak at different wavelengths. Hotter objects emit most of their radiation at shorter wavelengths; hence they will appear to be bluer. Wien’s law was an early attempt to describe the → blackbody radiation.
The law closely approximated the true shape of the blackbody spectrum at short wavelengths, but ultimately failed because it relied solely on classical physics. It was superseded by → Planck’s radiation law, which correctly describes the blackbody spectrum at all wavelengths.

See also: After the German physicist Wilhelm Wien (1864-1928), who found the law in 1896. He was awarded the 1911 Nobel Prize in physics; → displacement; → law.

The wavelength corresponding to the maximum emissive power of a black body is inversely proportional to the absolute temperature of the body: λ_max.T = 0.29 cm-deg. Wien’s law explains why objects of different temperature emit spectra that peak at different wavelengths. Hotter objects emit most of their radiation at shorter wavelengths; hence they will appear to be bluer. Wien’s law was an early attempt to describe the → blackbody radiation.
The law closely approximated the true shape of the blackbody spectrum at short wavelengths, but ultimately failed because it relied solely on classical physics. It was superseded by → Planck’s radiation law, which correctly describes the blackbody spectrum at all wavelengths.

See also: After the German physicist Wilhelm Wien (1864-1928), who found the law in 1896. He was awarded the 1911 Nobel Prize in physics; → displacement; → law.

A theorem used in signal processing whereby the → spectral density of a random signal is the → Fourier transform of the corresponding → autocorrelation function. In other words, the autocorrelation function and the spectral density function constitute a → Fourier transform pair. The Wiener-Khinchin theorem allows one to estimate the spectral density function from the Fourier transform of the autocorrelation function, which is easier to handle. The theorem has an important application particularly
in radio astronomy. The two following → Fourier integrals are called the Wiener-Khinchin relations: K(τ) = ∫ J(f)e^-iωτdf and J(f) = ∫ K(τ)e^iωτdτ (both summed over -∞ to +∞), where K(τ) is the autocorrelation function and J(f) is the spectral density.

See also: Named after Norbert Wiener (1894-1964), American mathematician, who
first published this theorem in 1930, and Aleksandr Khinchin (1894-1959), Russian mathematician, who did so independently in 1934; → theorem.

A theorem used in signal processing whereby the → spectral density of a random signal is the → Fourier transform of the corresponding → autocorrelation function. In other words, the autocorrelation function and the spectral density function constitute a → Fourier transform pair. The Wiener-Khinchin theorem allows one to estimate the spectral density function from the Fourier transform of the autocorrelation function, which is easier to handle. The theorem has an important application particularly
in radio astronomy. The two following → Fourier integrals are called the Wiener-Khinchin relations: K(τ) = ∫ J(f)e^-iωτdf and J(f) = ∫ K(τ)e^iωτdτ (both summed over -∞ to +∞), where K(τ) is the autocorrelation function and J(f) is the spectral density.

See also: Named after Norbert Wiener (1894-1964), American mathematician, who
first published this theorem in 1930, and Aleksandr Khinchin (1894-1959), Russian mathematician, who did so independently in 1934; → theorem.

Living in a state of nature; not tamed or domesticated (Dictionary.com).

Etymology (EN): M.E., from O.E. wilde; cognate with Du., O.H.G. wildi, Ger. wild, Sw. vild.

Etymology (PE): Towsan “wild,” cf. Av. disav- “a kind of night predator animal.”

Living in a state of nature; not tamed or domesticated (Dictionary.com).

Etymology (EN): M.E., from O.E. wilde; cognate with Du., O.H.G. wildi, Ger. wild, Sw. vild.

Etymology (PE): Towsan “wild,” cf. Av. disav- “a kind of night predator animal.”

Animals and plants living in their natural habitat.

See also: → wild; → life.

Animals and plants living in their natural habitat.

See also: → wild; → life.

A space telescope launched by NASA in 2001 which measures the temperature fluctuations in the → cosmic microwave background (CMB) radiation.
It creates a full-sky map of the CMB, with a 13 arcminute resolution via multi-frequency observations. WMAP is the first mission to use a → Lagrangian point L2 as its permanent observing station at a distance of 1.5 million km. WMAP completed its prime two years of mission operations in September 2003 and is continuing in 2009 its observations for still several years to come. WMAP’s measurements have played a considerable role in establishing the current standard model of cosmology. They are consistent with a Universe that is dominated by → dark energy, with negative pressure or a → cosmological constant. In this model, the age of the Universe is 13.73 ± 0.12 billion years. The current expansion rate of the Universe measured by the Hubble constant, is 70.5 ± 1.3 km·s^-1 Mpc^-1. The content of the Universe consists of 4.56% ± 0.15% ordinary → baryonic matter, 22.8% ± 1.3% → cold dark matter, and 72.6% ± 1.5% of → dark energy, that accelerates the → expansion of the Universe.

See also: WMAP, short for Wilkinson Microwave Anisotropy Probe, in honor of David Todd Wilkinson (1935-2002), who had been a member of the mission’s science team.

A space telescope launched by NASA in 2001 which measures the temperature fluctuations in the → cosmic microwave background (CMB) radiation.
It creates a full-sky map of the CMB, with a 13 arcminute resolution via multi-frequency observations. WMAP is the first mission to use a → Lagrangian point L2 as its permanent observing station at a distance of 1.5 million km. WMAP completed its prime two years of mission operations in September 2003 and is continuing in 2009 its observations for still several years to come. WMAP’s measurements have played a considerable role in establishing the current standard model of cosmology. They are consistent with a Universe that is dominated by → dark energy, with negative pressure or a → cosmological constant. In this model, the age of the Universe is 13.73 ± 0.12 billion years. The current expansion rate of the Universe measured by the Hubble constant, is 70.5 ± 1.3 km·s^-1 Mpc^-1. The content of the Universe consists of 4.56% ± 0.15% ordinary → baryonic matter, 22.8% ± 1.3% → cold dark matter, and 72.6% ± 1.5% of → dark energy, that accelerates the → expansion of the Universe.

See also: WMAP, short for Wilkinson Microwave Anisotropy Probe, in honor of David Todd Wilkinson (1935-2002), who had been a member of the mission’s science team.

The depression on the → Sun’s → photosphere associated with → sunspots and involving the → Wilson effect. The measured depression values vary between about 700 and 2,000 km.

See also: → Wilson effect; → depression.

The depression on the → Sun’s → photosphere associated with → sunspots and involving the → Wilson effect. The measured depression values vary between about 700 and 2,000 km.

See also: → Wilson effect; → depression.

A phenomenon in which the shape of → sunspots flattens as they approach the → Sun’s limb due to the → solar rotation. More specifically, when a sunspot approaches the → solar limbs the width of the → penumbra, relative to the → umbra, on the side facing the center of the Sun seems to become narrower than on the side facing the limb. This phenomenon arises from a projection effect, and is due to a geometrical depression (the → Wilson depression) in the layers of constant → optical depth in sunspots (see, e.g., Sami K. Solanki, 2003, Sunspots: An overview, The Astron. Astrophys. Rev., 11, 153).

See also: First noticed by Alexander Wilson (1714-1786); → effect.

A phenomenon in which the shape of → sunspots flattens as they approach the → Sun’s limb due to the → solar rotation. More specifically, when a sunspot approaches the → solar limbs the width of the → penumbra, relative to the → umbra, on the side facing the center of the Sun seems to become narrower than on the side facing the limb. This phenomenon arises from a projection effect, and is due to a geometrical depression (the → Wilson depression) in the layers of constant → optical depth in sunspots (see, e.g., Sami K. Solanki, 2003, Sunspots: An overview, The Astron. Astrophys. Rev., 11, 153).

See also: First noticed by Alexander Wilson (1714-1786); → effect.

The strong correlation between the equivalent width of Ca II → H and K lines of a late-type giant or supergiant star with the absolute visual magnitude of the star.

See also: O. C. Wilson & M. K. Vainu Bappu (1957, ApJ 125, 661); → effect.

The strong correlation between the equivalent width of Ca II → H and K lines of a late-type giant or supergiant star with the absolute visual magnitude of the star.

See also: O. C. Wilson & M. K. Vainu Bappu (1957, ApJ 125, 661); → effect.

A member of a broad class of hypothetical elementary particles moving with non-relativistical speeds at the time of structure formation in the early Universe. WIMPs have nonzero rest mass and participate only in the weak nuclear interaction. WIMPs are expected to have collapsed into a roughly isothermal, spherical halo within which the visible portion of our galaxy resides. → dark halo. The → neutralino, predicted by supersymmetric theories is the favorite WIMP candidate. Another candidate is the → axion. WIMPs are candidates for dark matter.

See also: → weak; → interction; → massive; → particle .

A member of a broad class of hypothetical elementary particles moving with non-relativistical speeds at the time of structure formation in the early Universe. WIMPs have nonzero rest mass and participate only in the weak nuclear interaction. WIMPs are expected to have collapsed into a roughly isothermal, spherical halo within which the visible portion of our galaxy resides. → dark halo. The → neutralino, predicted by supersymmetric theories is the favorite WIMP candidate. Another candidate is the → axion. WIMPs are candidates for dark matter.

See also: → weak; → interction; → massive; → particle .

1a) Meteo.: Air in motion, especially a natural and perceptible movement of air
relative to the ground.

1b) Astro.→ radiation-driven wind; → solar wind; → Galactic wind; → stellar wind.

2. To change direction; turn; to have a circular or spiral course or direction; to coil or twine about something.

Etymology (EN): 1) M.E., O.E. wind (cf. O.S., O.Fris., Du. wind, O.H.G. wind, Ger. Wind, Goth. winds).

2. M.E. windan, from O.E. windan “to turn, twist, curl,” cognate with Du. winden, O.H.G. wintan, Ger. winden, from PIE *wendh- “to turn, wind, weave.”

Etymology (PE): 1) Bâd, from Mid.Pers. wâd “wind;” Av. vāta- “wind;” cf. Skt. vāta- “wind, god of wind;” Gk. anemos “wind;”
L. ventus “wind” (Fr. vent); cognate with E. wind, as above.

2. Picidan “to twist, entwine, coil,” → spiral.

1a) Meteo.: Air in motion, especially a natural and perceptible movement of air
relative to the ground.

1b) Astro.→ radiation-driven wind; → solar wind; → Galactic wind; → stellar wind.

2. To change direction; turn; to have a circular or spiral course or direction; to coil or twine about something.

Etymology (EN): 1) M.E., O.E. wind (cf. O.S., O.Fris., Du. wind, O.H.G. wind, Ger. Wind, Goth. winds).

2. M.E. windan, from O.E. windan “to turn, twist, curl,” cognate with Du. winden, O.H.G. wintan, Ger. winden, from PIE *wendh- “to turn, wind, weave.”

Etymology (PE): 1) Bâd, from Mid.Pers. wâd “wind;” Av. vāta- “wind;” cf. Skt. vāta- “wind, god of wind;” Gk. anemos “wind;”
L. ventus “wind” (Fr. vent); cognate with E. wind, as above.

2. Picidan “to twist, entwine, coil,” → spiral.

A quasi-spherical accretion that is likely to occur in a → high-mass X-ray binary (HMXB) when the optical star of → early spectral class (O-B) does not fill its → Roche lobe, but has a significant → mass loss via → stellar wind. In → close binary systems another accretion regime, → disk accretion, occurs when the optical star overfills its Roche lobe.

See also: → wind; → accretion.

A quasi-spherical accretion that is likely to occur in a → high-mass X-ray binary (HMXB) when the optical star of → early spectral class (O-B) does not fill its → Roche lobe, but has a significant → mass loss via → stellar wind. In → close binary systems another accretion regime, → disk accretion, occurs when the optical star overfills its Roche lobe.

See also: → wind; → accretion.

A process whereby dense winds of very luminous O type stars modify the temperature and internal structure of the underlying photosphere by scattering back a considerable part of the coming photospheric radiation. Not to be confused with → line blanketing .

See also: Thus called because the wind acts like a blanket and heats the photosphere * by reflecting its radiation; → wind.

A process whereby dense winds of very luminous O type stars modify the temperature and internal structure of the underlying photosphere by scattering back a considerable part of the coming photospheric radiation. Not to be confused with → line blanketing .

See also: Thus called because the wind acts like a blanket and heats the photosphere * by reflecting its radiation; → wind.

The inhomogeneous property of a → radiation-driven wind, or the physical mechanism accounting for the → clumped wind.

See also: → clumpy; → wind.

The inhomogeneous property of a → radiation-driven wind, or the physical mechanism accounting for the → clumped wind.

See also: → clumpy; → wind.

The final kinetic energy of the → stellar wind expressed by:

(1/2)Mdot.v_∞² = (1/2)(v_∞/c)L

For an O6 star, L ~ 3 x 10⁵Lsun and v_∞ ~ 2000 km s^-1, which give a wind luminosity of ~ 1 x 10³⁷ erg s^-1, about 1% of the → stellar luminosity. See also → photon tiring limit.

See also: → wind; → luminosity.

The final kinetic energy of the → stellar wind expressed by:

(1/2)Mdot.v_∞² = (1/2)(v_∞/c)L

For an O6 star, L ~ 3 x 10⁵Lsun and v_∞ ~ 2000 km s^-1, which give a wind luminosity of ~ 1 x 10³⁷ erg s^-1, about 1% of the → stellar luminosity. See also → photon tiring limit.

See also: → wind; → luminosity.

The product of the → mass loss rate and → terminal velocity used in the → radiation-driven wind theory. See also → modified wind momentum.

See also: → wind; → momentum.

The product of the → mass loss rate and → terminal velocity used in the → radiation-driven wind theory. See also → modified wind momentum.

See also: → wind; → momentum.

A diagram showing the relative frequency of winds blowing from each of the 8 or 16 main points of the compass, sometimes within specified speed ranges, at a given location over a considerable period.

Etymology (EN): Translation of Ger. Windrose “compass card,” from Wind→ wind + Rose “rose,” → Rosette Nebula.

Etymology (PE): Bâdnaqš, from bâd, → wind, + naqš “painting, engraving, printing,” → map.

A diagram showing the relative frequency of winds blowing from each of the 8 or 16 main points of the compass, sometimes within specified speed ranges, at a given location over a considerable period.

Etymology (EN): Translation of Ger. Windrose “compass card,” from Wind→ wind + Rose “rose,” → Rosette Nebula.

Etymology (PE): Bâdnaqš, from bâd, → wind, + naqš “painting, engraving, printing,” → map.

An object that is balanced on a rotating axis and indicates the direction of the wind. Also called a weather vane.

Etymology (EN): → wind + vane “a blade, plate,” O.E. fana</i< “flag, weather-cock;” cf. Goth. fana “piece of cloth,” O.H.G. fano, Ger. Fahne “flag, standard.”

Etymology (PE): Bbâdnemâ “wind indicator,” from bâd, → wind, + nemâ, from nemudan, → planetarium.

An object that is balanced on a rotating axis and indicates the direction of the wind. Also called a weather vane.

Etymology (EN): → wind + vane “a blade, plate,” O.E. fana</i< “flag, weather-cock;” cf. Goth. fana “piece of cloth,” O.H.G. fano, Ger. Fahne “flag, standard.”

Etymology (PE): Bbâdnemâ “wind indicator,” from bâd, → wind, + nemâ, from nemudan, → planetarium.

The speed at which the → stellar wind is forced away from the star. Wind velocities of → hot stars are directly measured from → P Cygni profiles, which indicate velocities from several hundred to several thousand km s^-1. See also → escape velocity, → terminal velocity, → velocity law, → radiation-driven wind, → CAK model.

See also: → wind; → velocity.

The speed at which the → stellar wind is forced away from the star. Wind velocities of → hot stars are directly measured from → P Cygni profiles, which indicate velocities from several hundred to several thousand km s^-1. See also → escape velocity, → terminal velocity, → velocity law, → radiation-driven wind, → CAK model.

See also: → wind; → velocity.

The problem encountered in the explanation of the → spiral arms of galaxies if the material making up a spiral arm is static, that is
remains in the arm. Since galaxies exhibit → differential rotation, stars near the center take less time to orbit the center than those farther from the center. The arm would, after a few → galactic rotations, become increasingly curved and wind around the → galaxy ever tighter until it ultimately disappears. This is inconsistent with observations.

The problem encountered in the explanation of the → spiral arms of galaxies if the material making up a spiral arm is static, that is
remains in the arm. Since galaxies exhibit → differential rotation, stars near the center take less time to orbit the center than those farther from the center. The arm would, after a few → galactic rotations, become increasingly curved and wind around the → galaxy ever tighter until it ultimately disappears. This is inconsistent with observations.

1. Anything likened to a window in appearance or function.
   
2. In particular, the wavelength region in the electromagnetic spectrum that is relatively unaffected by atmospheric absorption. → atmospheric windows; → infrared window; → optical window; → radio window.

Etymology (EN): Window literally “wind eye,” from O.N. vindauga, from vindr, → wind, + auga,
→ eye.

Etymology (PE): Rowzané, from rowzan “window, aperture;” Mid.Pers. rocânak “window,” rôšn “light; bright, luminous,” from Av. raocana- “bright, shining, radiant,” raocah- “light, luminous; daylight,” related to Mod.Pers. ruz “day,” from Mid.Pers. rôc, O.Pers. raucah-; akin to Skt. rocaná- “bright, shining,” roka- “brightness, light;” Gk. leukos “white, clear;” L. lux “light” (also lumen, luna); PIE base *leuk- “light, brightness.” The Persian words rowšan “bright, clear,” foruq “light,” and afruxtan “to light, kindle” also belong to this family, as well as the E. light, Ger. Licht, and Fr. lumière; forusorx→ infrarouge.

1. Anything likened to a window in appearance or function.
   
2. In particular, the wavelength region in the electromagnetic spectrum that is relatively unaffected by atmospheric absorption. → atmospheric windows; → infrared window; → optical window; → radio window.

Etymology (EN): Window literally “wind eye,” from O.N. vindauga, from vindr, → wind, + auga,
→ eye.

Etymology (PE): Rowzané, from rowzan “window, aperture;” Mid.Pers. rocânak “window,” rôšn “light; bright, luminous,” from Av. raocana- “bright, shining, radiant,” raocah- “light, luminous; daylight,” related to Mod.Pers. ruz “day,” from Mid.Pers. rôc, O.Pers. raucah-; akin to Skt. rocaná- “bright, shining,” roka- “brightness, light;” Gk. leukos “white, clear;” L. lux “light” (also lumen, luna); PIE base *leuk- “light, brightness.” The Persian words rowšan “bright, clear,” foruq “light,” and afruxtan “to light, kindle” also belong to this family, as well as the E. light, Ger. Licht, and Fr. lumière; forusorx→ infrarouge.

A function whose value is zero outside a given interval. Applications of window functions include signal filtering and spectral analysis. The various types of windw functions include: → rectangular window, cosine window, triangular window, Gaussian window, Hanning window, and so on.

See also: → window; → function.

A function whose value is zero outside a given interval. Applications of window functions include signal filtering and spectral analysis. The various types of windw functions include: → rectangular window, cosine window, triangular window, Gaussian window, Hanning window, and so on.

See also: → window; → function.

The fermented juice of grapes, made in many varieties, such as red, white, sweet, dry, still, and sparkling, for use as a beverage, in cooking, in religious rites, etc., and usually having an alcoholic content of 14 percent or less (Dictionary.com).

Etymology (EN): M.E., O.E. win, cognate with O.H.G. win, Du. wijn, Ger. Wein, from L. vinum “wine,” from PIE *woin-o-, related Gk. word oinos.

Etymology (PE): Mey, variant mol “wine;” Mid.Pers. mad, may “wine;” Av. maδu- “wine;” cf. Skt. madhu- “wine, sweet drink, sweet;” Gk. methy “wine;” O.C.S. medu; Lith. medus “honey;” O.Irish mid; Welsh medd; Breton mez “mead;” O.E. medu; E. mead “fermented honey drink;” Russ. medved “(honey-eater) bear.”
Bâdé, from Mid.Pers. bâdag, from O.Pers. *bātu- “wine” (from bātu-gara- “cup, bowl”); cf. Khotanese Saka bātaa- “wine;” O.Pers. *batiaka- “cup, bowl” (cf. Pers. bâdiyé “bowl”) loaned in Gk. batiaké “bowl, cup.”
Nabid, “wine, date-wine,” ultimately from Proto-Ir. *paH- “to drink;” cf. Av. paitīš- “drink” in vīspô.paitīš- “having all sorts of drinks;” pitu- “juice, food;” Wakhi puv-, pəv-, pit-; Sanglechi pöv-/pövδ- “to drink;” Skt. pā- “to drink;” Gk. pinein “to drink;” L. bibere “to drink,” related to potare “to drink.”

The fermented juice of grapes, made in many varieties, such as red, white, sweet, dry, still, and sparkling, for use as a beverage, in cooking, in religious rites, etc., and usually having an alcoholic content of 14 percent or less (Dictionary.com).

Etymology (EN): M.E., O.E. win, cognate with O.H.G. win, Du. wijn, Ger. Wein, from L. vinum “wine,” from PIE *woin-o-, related Gk. word oinos.

Etymology (PE): Mey, variant mol “wine;” Mid.Pers. mad, may “wine;” Av. maδu- “wine;” cf. Skt. madhu- “wine, sweet drink, sweet;” Gk. methy “wine;” O.C.S. medu; Lith. medus “honey;” O.Irish mid; Welsh medd; Breton mez “mead;” O.E. medu; E. mead “fermented honey drink;” Russ. medved “(honey-eater) bear.”
Bâdé, from Mid.Pers. bâdag, from O.Pers. *bātu- “wine” (from bātu-gara- “cup, bowl”); cf. Khotanese Saka bātaa- “wine;” O.Pers. *batiaka- “cup, bowl” (cf. Pers. bâdiyé “bowl”) loaned in Gk. batiaké “bowl, cup.”
Nabid, “wine, date-wine,” ultimately from Proto-Ir. *paH- “to drink;” cf. Av. paitīš- “drink” in vīspô.paitīš- “having all sorts of drinks;” pitu- “juice, food;” Wakhi puv-, pəv-, pit-; Sanglechi pöv-/pövδ- “to drink;” Skt. pā- “to drink;” Gk. pinein “to drink;” L. bibere “to drink,” related to potare “to drink.”

1. Either of the two limbs of a bird allowing her to fly. → Pegasus.
   

2. Either of the large flat structures in an aircraft’s body that provide the main source of lift.
   

3. In spectroscopy, same as → line wing.

Etymology (EN): M.E. wenge from O.N. vængr “wing of a bird, aisle, etc.” (cf. Dan., Swed. vinge “wing”).

Etymology (PE): Bâl “wing,” Mid.Pers. bâl, variant of par / parr “feather, " with the conversion of p to b and r to l; Av. parəna- “feather;” cf. Skt. parnam;
O.H.G. farn “fern;” PIE pornom “feather.”

1. Either of the two limbs of a bird allowing her to fly. → Pegasus.
   

2. Either of the large flat structures in an aircraft’s body that provide the main source of lift.
   

3. In spectroscopy, same as → line wing.

Etymology (EN): M.E. wenge from O.N. vængr “wing of a bird, aisle, etc.” (cf. Dan., Swed. vinge “wing”).

Etymology (PE): Bâl “wing,” Mid.Pers. bâl, variant of par / parr “feather, " with the conversion of p to b and r to l; Av. parəna- “feather;” cf. Skt. parnam;
O.H.G. farn “fern;” PIE pornom “feather.”

A spectral feature at 9850-10200 Å appearing in the spectrum of some late-type → M dwarfs. It is attributed to iron hybrid (FeH), a typical signature of the atmospheres of the coolest stars.

See also: First detected by R. F. Wing and W. K. Ford (1969, PASP 81, 527); → band.

A spectral feature at 9850-10200 Å appearing in the spectrum of some late-type → M dwarfs. It is attributed to iron hybrid (FeH), a typical signature of the atmospheres of the coolest stars.

See also: First detected by R. F. Wing and W. K. Ford (1969, PASP 81, 527); → band.

The season beginning at the → winter solstice, about December 22 and lasting until the → vernal equinox, about March 21.

Etymology (EN): M.E., OE; cf. O.Fris., Du. winter, O.S., O.H.G. wintar, Ger. winter, Dan., Swed. vinter, Goth. wintrus “winter”),

Etymology (PE): Zemestân “winter,” related to zam “cold,” Mid.Pers. zam, zamistân “winter;” Av. zimô “winter;” cf. Skt. hima- “cold, frost;” Ossetic zymæg/zumæg “winter;” Gk. xeimon “winter;” L. hiems “winter;” Lith. ziema “winter;” PIE *gheim- “snow, winter.”

The season beginning at the → winter solstice, about December 22 and lasting until the → vernal equinox, about March 21.

Etymology (EN): M.E., OE; cf. O.Fris., Du. winter, O.S., O.H.G. wintar, Ger. winter, Dan., Swed. vinter, Goth. wintrus “winter”),

Etymology (PE): Zemestân “winter,” related to zam “cold,” Mid.Pers. zam, zamistân “winter;” Av. zimô “winter;” cf. Skt. hima- “cold, frost;” Ossetic zymæg/zumæg “winter;” Gk. xeimon “winter;” L. hiems “winter;” Lith. ziema “winter;” PIE *gheim- “snow, winter.”

The moment in the northern hemisphere when the → Sun attains its lowest → declination of -23°26’ (or -23°.44) with respect the → equator plane. It happens when the Earth’s axis is orientated directly away from the Sun, on 21 or 22 December. During the northern winter solstice the Sun appears to be directly overhead at noon for places situated at → latitude 23.44 degrees south, known as the → tropic of Capricorn. The winter solstice can occur at any moment during the day. Two successive winter solstices are shifted in time by about 6 h. The winter solstice in the northern hemisphere is the → summer solstice in the southern hemisphere.

See also: → winter; → solstice..

The moment in the northern hemisphere when the → Sun attains its lowest → declination of -23°26’ (or -23°.44) with respect the → equator plane. It happens when the Earth’s axis is orientated directly away from the Sun, on 21 or 22 December. During the northern winter solstice the Sun appears to be directly overhead at noon for places situated at → latitude 23.44 degrees south, known as the → tropic of Capricorn. The winter solstice can occur at any moment during the day. Two successive winter solstices are shifted in time by about 6 h. The winter solstice in the northern hemisphere is the → summer solstice in the southern hemisphere.

See also: → winter; → solstice..

A slender flexible thread or rod of metal.

Etymology (EN): M.E., O.E. wir, cf. O.N. viravirka “filigree work,” Swed. vira “to twist,” O.H.G. wiara “fine gold work.”

Etymology (PE): Sim “wire,” initially “strand of silver,” from sim “silver,” from Mid.Pers. asêm “silver,” from Gk. asemon “without mark, uncoined, shapeless, formless,” from argurion asemon “uncoined money.” For semantic similarity, see → silver.

A slender flexible thread or rod of metal.

Etymology (EN): M.E., O.E. wir, cf. O.N. viravirka “filigree work,” Swed. vira “to twist,” O.H.G. wiara “fine gold work.”

Etymology (PE): Sim “wire,” initially “strand of silver,” from sim “silver,” from Mid.Pers. asêm “silver,” from Gk. asemon “without mark, uncoined, shapeless, formless,” from argurion asemon “uncoined money.” For semantic similarity, see → silver.

The quality or state of being → wise; knowledge of what is true or right coupled with just judgment as to action; sagacity, discernment, or insight (Dictionary.com). Wisdom is gained over the years through experience. It is the insight in knowing the probable outcome learned through experience. In contrast, → reason is using the → rational → reasoning to evaluate pros and cons in making a decision.

Etymology (EN): M.E.; O.E. wisdom, from wis “→ wise”

• -dom. The first component is related to → vision and Pers. bin, didan “to see.”

Etymology (PE): Xerad “understanding, judjement, intellect, wisdom;” Mid.Pers. xrad “reason, intellect, intelligence, wisdom, understanding;” O.Pers. xraθu- “wisdom;” Av. xratu- “intelligence, understanding, wisdom; will, purpose, council;” cf. Skt. krátu- “power, will-power;” Gk. kratos “power, strength.”

The quality or state of being → wise; knowledge of what is true or right coupled with just judgment as to action; sagacity, discernment, or insight (Dictionary.com). Wisdom is gained over the years through experience. It is the insight in knowing the probable outcome learned through experience. In contrast, → reason is using the → rational → reasoning to evaluate pros and cons in making a decision.

Etymology (EN): M.E.; O.E. wisdom, from wis “→ wise”

• -dom. The first component is related to → vision and Pers. bin, didan “to see.”

Etymology (PE): Xerad “understanding, judjement, intellect, wisdom;” Mid.Pers. xrad “reason, intellect, intelligence, wisdom, understanding;” O.Pers. xraθu- “wisdom;” Av. xratu- “intelligence, understanding, wisdom; will, purpose, council;” cf. Skt. krátu- “power, will-power;” Gk. kratos “power, strength.”

Having the power of discerning and judging properly as to what is true or right; possessing discernment, judgment, or discretion (Dictionary.com).

Etymology (EN): From M.E. wis, wys, from O.E. wis (“wise”), cognate with Du. wijs, Ger. weise, Norw. and Swed. vis.

Etymology (PE): Xeradmand, from xerad, → wisdom,

• -mand relatrion and possession suffix.

Having the power of discerning and judging properly as to what is true or right; possessing discernment, judgment, or discretion (Dictionary.com).

Etymology (EN): From M.E. wis, wys, from O.E. wis (“wise”), cognate with Du. wijs, Ger. weise, Norw. and Swed. vis.

Etymology (PE): Xeradmand, from xerad, → wisdom,

• -mand relatrion and possession suffix.