An Etymological Dictionary of Astronomy and Astrophysics

1a) The community or people in general.

1b) A particular group of people with a common interest, aim, etc.

2a) Of, relating to, or concerning the people as a whole.

2b) Open or accessible to all.

Related concepts:

→ all, → general, → omni-, → total, → universal.

Etymology (EN): M.E., from L. publicus “of the people; of the state,” also “common, general, public; ordinary,” and as a noun, “a commonwealth; public property,” from Old L. poplicus “pertaining to the people.” from populus “people.”

Etymology (PE): Hamegân, from hamé, → all, + -gân suffix forming plural entities, from Mid.Pers. -gânag, -gâna.

1a) The community or people in general.

1b) A particular group of people with a common interest, aim, etc.

2a) Of, relating to, or concerning the people as a whole.

2b) Open or accessible to all.

Related concepts:

→ all, → general, → omni-, → total, → universal.

Etymology (EN): M.E., from L. publicus “of the people; of the state,” also “common, general, public; ordinary,” and as a noun, “a commonwealth; public property,” from Old L. poplicus “pertaining to the people.” from populus “people.”

Etymology (PE): Hamegân, from hamé, → all, + -gân suffix forming plural entities, from Mid.Pers. -gânag, -gâna.

The collective opinion of many people on some issue, problem, etc., especially as a guide to action, decision, or the like (Dictionary.com).

See also: → public; → opinion.

The collective opinion of many people on some issue, problem, etc., especially as a guide to action, decision, or the like (Dictionary.com).

See also: → public; → opinion.

1. The act of publishing a book, periodical, map, piece of music, engraving, or the like.
   

2. The act of bringing before the public; announcement.
   

3. The state or fact of being published (Dictionary.com).

See also: Verbal noun of → publish.

1. The act of publishing a book, periodical, map, piece of music, engraving, or the like.
   

2. The act of bringing before the public; announcement.
   

3. The state or fact of being published (Dictionary.com).

See also: Verbal noun of → publish.

1. Extensive mention in the news media or by word of mouth or other means of communication.
   

2. The state of being public, or open to general observation or knowledge (Dictionary.com).

See also: → public; → -ity.

1. Extensive mention in the news media or by word of mouth or other means of communication.
   

2. The state of being public, or open to general observation or knowledge (Dictionary.com).

See also: → public; → -ity.

To give publicity to; bring to public notice, advertise.

See also: → public; → -ize.

To give publicity to; bring to public notice, advertise.

See also: → public; → -ize.

To issue (printed or otherwise reproduced textual or graphic material, computer software, etc.) for sale or distribution to the public (Dictionary.com).

Etymology (EN): M.E. publisshen, O.Fr. publier “make public, spread out, communicate,” from L. publicare “make public,” from publicus, → public.

Etymology (PE): Vâgândan “to diffuse, scatter, disperse,” on the model of parâgandan, parâkandan “scatter, disperse,” from vâ- “asunder, apart, off, away,” → dis-,

• gân variant of gan, kan (cf. Av. vikān- “to destroy,” Kurd. nikândin “to bury”), from Proto-Ir. *kan- “to throw, place, put,” → scatter.

To issue (printed or otherwise reproduced textual or graphic material, computer software, etc.) for sale or distribution to the public (Dictionary.com).

Etymology (EN): M.E. publisshen, O.Fr. publier “make public, spread out, communicate,” from L. publicare “make public,” from publicus, → public.

Etymology (PE): Vâgândan “to diffuse, scatter, disperse,” on the model of parâgandan, parâkandan “scatter, disperse,” from vâ- “asunder, apart, off, away,” → dis-,

• gân variant of gan, kan (cf. Av. vikān- “to destroy,” Kurd. nikândin “to bury”), from Proto-Ir. *kan- “to throw, place, put,” → scatter.

A person or company whose business is the publishing of books, periodicals, engravings, computer software, etc. (Dictionary.com).

See also: Agent noun from → publish; → -er.

A person or company whose business is the publishing of books, periodicals, engravings, computer software, etc. (Dictionary.com).

See also: Agent noun from → publish; → -er.

1. The soft fleshy part of a fruit.
   

   2. A soft moist shapeless mass of matter.

Etymology (EN): M.E., from L. pulpa “animal or plant pulp; pith of wood.”

Etymology (PE): Gup, from Jâski gup “fleshy, fat;” cf. Gilaki quppe “watermelon core.”

1. The soft fleshy part of a fruit.
   

   2. A soft moist shapeless mass of matter.

Etymology (EN): M.E., from L. pulpa “animal or plant pulp; pith of wood.”

Etymology (PE): Gup, from Jâski gup “fleshy, fat;” cf. Gilaki quppe “watermelon core.”

A rotating → neutron star that emits a radio → beam that is centered on the → magnetic axis of the neutron star. As the magnetic axis and hence the beam are inclined to the → rotation axis, a → pulse is seen every time the → rotation brings the → magnetic pole region of the neutron star into view. In this way the pulsar acts much as a light house does, sweeping a beam of radiation through space. The pulse or spin periods range from 1.4 milliseconds to 8.5 seconds. As neutron stars concentrate an average of 1.4 → solar masses on a diameter of only 20 km, pulsars are exceedingly → dense and → compact,
representing the densest matter in the observable Universe. The pulsar radiation,
chiefly emitted in → radio frequencies (0.1-1 GHz), is highly → polarized. The exact mechanism by which a pulsar radiates is still a matter of vigorous investigation.
Simply put, an enormous electric field is induced by the rotation of a magnetized neutron star. The force of this field
exceeds gravity by ten to twelve orders of magnitudes. Charged particles are whereby pulled out from the stellar surface resulting in a dense, magnetized plasma that surrounds the pulsar (→ magnetosphere). The charged particles flow out
of the magnetic → polar caps of the neutron star, following the open
magnetic field lines. The acceleration of the charged particles along the curved magnetic field lines will cause them to radiate (see, e.g., M. Kramer, 2010, astro-ph/1008.5032).

See also:
→ accreting neutron star, → anomalous X-ray pulsar, → binary pulsar, → black-widow pulsar, → Crab pulsar, → double pulsar, → Hulse-Taylor pulsar, → isolated neutron star (INS), → millisecond pulsar, → neutron star, → nulling fraction, → nulling pulsar, → optical pulsar, → pulsar glitch, → pulsar magnetosphere, → pulsar nulling, → pulsar planet, → pulsar wind nebula, → radio pulsar, → recycled pulsar, → rotation-powered pulsar (RPP), → Vela pulsar, → X-ray Dim Isolated Neutron Star (XDINS), → X-ray pulsar.

Etymology (EN): Pulsar, from puls(e) or puls(ing) + (st)ar.

Etymology (PE): Tapâr, from tap, → pulse, + (set)âr(é), from setâré, → star.

A rotating → neutron star that emits a radio → beam that is centered on the → magnetic axis of the neutron star. As the magnetic axis and hence the beam are inclined to the → rotation axis, a → pulse is seen every time the → rotation brings the → magnetic pole region of the neutron star into view. In this way the pulsar acts much as a light house does, sweeping a beam of radiation through space. The pulse or spin periods range from 1.4 milliseconds to 8.5 seconds. As neutron stars concentrate an average of 1.4 → solar masses on a diameter of only 20 km, pulsars are exceedingly → dense and → compact,
representing the densest matter in the observable Universe. The pulsar radiation,
chiefly emitted in → radio frequencies (0.1-1 GHz), is highly → polarized. The exact mechanism by which a pulsar radiates is still a matter of vigorous investigation.
Simply put, an enormous electric field is induced by the rotation of a magnetized neutron star. The force of this field
exceeds gravity by ten to twelve orders of magnitudes. Charged particles are whereby pulled out from the stellar surface resulting in a dense, magnetized plasma that surrounds the pulsar (→ magnetosphere). The charged particles flow out
of the magnetic → polar caps of the neutron star, following the open
magnetic field lines. The acceleration of the charged particles along the curved magnetic field lines will cause them to radiate (see, e.g., M. Kramer, 2010, astro-ph/1008.5032).

See also:
→ accreting neutron star, → anomalous X-ray pulsar, → binary pulsar, → black-widow pulsar, → Crab pulsar, → double pulsar, → Hulse-Taylor pulsar, → isolated neutron star (INS), → millisecond pulsar, → neutron star, → nulling fraction, → nulling pulsar, → optical pulsar, → pulsar glitch, → pulsar magnetosphere, → pulsar nulling, → pulsar planet, → pulsar wind nebula, → radio pulsar, → recycled pulsar, → rotation-powered pulsar (RPP), → Vela pulsar, → X-ray Dim Isolated Neutron Star (XDINS), → X-ray pulsar.

Etymology (EN): Pulsar, from puls(e) or puls(ing) + (st)ar.

Etymology (PE): Tapâr, from tap, → pulse, + (set)âr(é), from setâré, → star.

A sudden change in the pulsar period due to a sudden shift in the crust of the → neutron star (a → starquake).

See also: → pulsar; → glitch.

A sudden change in the pulsar period due to a sudden shift in the crust of the → neutron star (a → starquake).

See also: → pulsar; → glitch.

A dense zone of magnetized → plasma surrounding a → pulsar. The magnetosphere, lying between the surface of the → neutron star and the → light cylinder,
corotates with the pulsar like a rigid body under the effect of strong magnetic field. The magnetosphere’s thickness is determined by the constraint that the corotation velocity of its upper surface should not exceed the → speed of light.

See also: → pilsar; → magnetosphere.

A dense zone of magnetized → plasma surrounding a → pulsar. The magnetosphere, lying between the surface of the → neutron star and the → light cylinder,
corotates with the pulsar like a rigid body under the effect of strong magnetic field. The magnetosphere’s thickness is determined by the constraint that the corotation velocity of its upper surface should not exceed the → speed of light.

See also: → pilsar; → magnetosphere.

A phenomenon in which the → pulsar  → emission abruptly drops to zero or near zero for a certain number of → pulse  → periods, then suddenly returns to normal. Nulling is relatively common in pulsars. The → nulling fraction can be more than 80%. Investigating the emission behaviors of → nulling pulsars is important to understand the pulsar emission mechanism.

See also: → pulsar; → null; → -ing.

A phenomenon in which the → pulsar  → emission abruptly drops to zero or near zero for a certain number of → pulse  → periods, then suddenly returns to normal. Nulling is relatively common in pulsars. The → nulling fraction can be more than 80%. Investigating the emission behaviors of → nulling pulsars is important to understand the pulsar emission mechanism.

See also: → pulsar; → null; → -ing.

A planet orbiting a → pulsar. The first such planet to be discovered was around a → millisecond pulsar known as PSR 1257+12.

See also: → pulsar; → planet.

A planet orbiting a → pulsar. The first such planet to be discovered was around a → millisecond pulsar known as PSR 1257+12.

See also: → pulsar; → planet.

Same as → plerion.

See also: → pulsar; → wind; → nebula.

Same as → plerion.

See also: → pulsar; → wind; → nebula.

To expand and contract rhythmically.

See also: Verb from → pulse.

To expand and contract rhythmically.

See also: Verb from → pulse.

A type of → variable star that changes its brightness by changing its volume through expansion and contraction. Classical pulsating stars, including → Cepheids, → RR Lyrae, and
→ Delta Scuti variables, are located in a quite narrow almost vertical region in the → H-R diagram, known as → instability strip. See also → kappa mechanism.

See also: Pulsating, verbal adj. of → pulsate; → star.

A type of → variable star that changes its brightness by changing its volume through expansion and contraction. Classical pulsating stars, including → Cepheids, → RR Lyrae, and
→ Delta Scuti variables, are located in a quite narrow almost vertical region in the → H-R diagram, known as → instability strip. See also → kappa mechanism.

See also: Pulsating, verbal adj. of → pulsate; → star.

Same as → oscillating Universe.

See also: Pulsating, verbal adj. of → pulsate; → universe.

Same as → oscillating Universe.

See also: Pulsating, verbal adj. of → pulsate; → universe.

The act of pulsating; beating or throbbing; vibration or undulation. → stellar pulsation.

See also: Verbal noun of → pulse.

The act of pulsating; beating or throbbing; vibration or undulation. → stellar pulsation.

See also: Verbal noun of → pulse.

The way in which pulsations occur in a star due to the fact that stars act as resonant cavities, as studied in → asteroseismology. A star may pulsate either with approximately spherical symmetry (radial pulsation), or as a series of waves running across the surface (non-radial pulsation). Pulsation may occur in a single mode or in multiple modes, depending on the type of star. Three different modes of pulsations have been detected through the → helioseismology of the → Sun: → p mode, → g mode, and → f mode, generated by acoustic, gravity, and surface gravity waves respectively. Also called → oscillation mode.

See also: → pulsation; → mode.

The way in which pulsations occur in a star due to the fact that stars act as resonant cavities, as studied in → asteroseismology. A star may pulsate either with approximately spherical symmetry (radial pulsation), or as a series of waves running across the surface (non-radial pulsation). Pulsation may occur in a single mode or in multiple modes, depending on the type of star. Three different modes of pulsations have been detected through the → helioseismology of the → Sun: → p mode, → g mode, and → f mode, generated by acoustic, gravity, and surface gravity waves respectively. Also called → oscillation mode.

See also: → pulsation; → mode.

Of or pertaining to → pulsation. → pulsational instability; → pulsational pair-instability supernova.

See also: → pulsation; → -al

Of or pertaining to → pulsation. → pulsational instability; → pulsational pair-instability supernova.

See also: → pulsation; → -al

A term used to describe irregularly spaced, fine-scale structure in optically thick rings. The process relies on a combination of viscosity and self-gravity of ring material to produce this fine structure. Also known as overstability (Ellis et al., 2007, Planetary Ring Systems, Springer).

See also: → pulsational; → instability.

A term used to describe irregularly spaced, fine-scale structure in optically thick rings. The process relies on a combination of viscosity and self-gravity of ring material to produce this fine structure. Also known as overstability (Ellis et al., 2007, Planetary Ring Systems, Springer).

See also: → pulsational; → instability.

A → supernova resulting from the → pair instability that generates several successive explosions. According to models, a first pulse ejects many solar masses of hydrogen layers as a shell. After the first explosion, the remaining core contracts and searches for a stable burning state. When the next explosion occurs a few years later, several solar masses of material are again ejected, which collide with the earlier ejecta. This collision can radiate 10⁵⁰ erg of light, about a factor of ten more than an ordinary → core-collapse supernova. After each pulse, the remaining core contracts, radiates neutrinos and light, and searches again for a stable burning state. Later ejections have lower mass, but have higher energy. They quickly catch up with the first shell, where the collision dissipates most of their kinetic energy as radiation. The first SNe from → Population III stars are likely due to pulsational pair instability (Woosley et al. 2007, Nature 450, 390). See also → pair-instability supernova.

See also: → pulsational;
→ pair; → instability.

A → supernova resulting from the → pair instability that generates several successive explosions. According to models, a first pulse ejects many solar masses of hydrogen layers as a shell. After the first explosion, the remaining core contracts and searches for a stable burning state. When the next explosion occurs a few years later, several solar masses of material are again ejected, which collide with the earlier ejecta. This collision can radiate 10⁵⁰ erg of light, about a factor of ten more than an ordinary → core-collapse supernova. After each pulse, the remaining core contracts, radiates neutrinos and light, and searches again for a stable burning state. Later ejections have lower mass, but have higher energy. They quickly catch up with the first shell, where the collision dissipates most of their kinetic energy as radiation. The first SNe from → Population III stars are likely due to pulsational pair instability (Woosley et al. 2007, Nature 450, 390). See also → pair-instability supernova.

See also: → pulsational;
→ pair; → instability.

1. Something that pulsates or beats.
   

   2. A → pulsating star. See also → hybrid pulsator.

See also: → pulsator; → -or.

1. Something that pulsates or beats.
   

   2. A → pulsating star. See also → hybrid pulsator.

See also: → pulsator; → -or.

1a) (v.) To → beat, to → vibrate.

1b) (v.) Physics: To → emit  → particles or → radiation  → periodically in short → bursts.

2a) (n.) Physics: A variation of a quantity whose value is normally constant. The essential characteristics of a pulse are: a → rise, a finite → duration, and a → decay.

2b) (n.) Physics: A single, abrupt emission of particles or radiation. See also → pulse counter, → pulse nulling, → pulse width, → pulsed laser, → precursor pulse.

Etymology (EN): M.E., from M.Fr. pous, from L. pulsus “a beat,” p.p. of pellere “to push, drive,” from PIE *pel- “to shake, swing.”

Etymology (PE): Tapidan “to beat, throb,” Mid.Pers. tapīdan “to be anguished; to suffer; to grow hot, to be hot,” variant tâftan, tâpidan “to stir up, to excite; to shine;” tâp “fever;” Av. tap- “to be hot, to grow hot,” tafnah-, tafnu- “fever, feverish heat;” cf. Skt. tap- “to spoil, injure, damage,; to suffer; to give out heat, to be hot,” tápati; L. tepere “to be warm;” PIE base *tep- “warm.”

1a) (v.) To → beat, to → vibrate.

1b) (v.) Physics: To → emit  → particles or → radiation  → periodically in short → bursts.

2a) (n.) Physics: A variation of a quantity whose value is normally constant. The essential characteristics of a pulse are: a → rise, a finite → duration, and a → decay.

2b) (n.) Physics: A single, abrupt emission of particles or radiation. See also → pulse counter, → pulse nulling, → pulse width, → pulsed laser, → precursor pulse.

Etymology (EN): M.E., from M.Fr. pous, from L. pulsus “a beat,” p.p. of pellere “to push, drive,” from PIE *pel- “to shake, swing.”

Etymology (PE): Tapidan “to beat, throb,” Mid.Pers. tapīdan “to be anguished; to suffer; to grow hot, to be hot,” variant tâftan, tâpidan “to stir up, to excite; to shine;” tâp “fever;” Av. tap- “to be hot, to grow hot,” tafnah-, tafnu- “fever, feverish heat;” cf. Skt. tap- “to spoil, injure, damage,; to suffer; to give out heat, to be hot,” tápati; L. tepere “to be warm;” PIE base *tep- “warm.”

A device that records counts the total number of pulses received over a given time interval.

See also: → pulse; → counter.

A device that records counts the total number of pulses received over a given time interval.

See also: → pulse; → counter.

A phenomenon seen in the → radio  → emission of many → pulsars where the emission appears to cease, or is greatly diminished, for a certain number of pulse periods. Typical time scales of nulling are of the order of a few pulse periods, however it may last for up to many hours in certain pulsars. For example, PSR B0826-34 is active for only about 20% of the time. Same as → pulsar nulling.

See also: → pulse + verbal noun of → null.

A phenomenon seen in the → radio  → emission of many → pulsars where the emission appears to cease, or is greatly diminished, for a certain number of pulse periods. Typical time scales of nulling are of the order of a few pulse periods, however it may last for up to many hours in certain pulsars. For example, PSR B0826-34 is active for only about 20% of the time. Same as → pulsar nulling.

See also: → pulse + verbal noun of → null.

The interval of time between two successive pulses. Also called pulse length, pulse duration.

See also: → pulse; → width.

The interval of time between two successive pulses. Also called pulse length, pulse duration.

See also: → pulse; → width.

A laser that emits short pulses of coherent light in fixed intervals, rather than a continuous flow of photons. → laser; → high power laser.

See also: Pulsed adj. of → pulse; → laser.

A laser that emits short pulses of coherent light in fixed intervals, rather than a continuous flow of photons. → laser; → high power laser.

See also: Pulsed adj. of → pulse; → laser.

To raise, drive, supply or inject as if by using a pump.

Etymology (EN): From M.E. pumpe, from M.Du. pompe “water conduit, pipe,” or M.L.G. pumpe “pump.”

Etymology (PE): Pompidan infinitive, from pomp, loan from Fr. pompe

To raise, drive, supply or inject as if by using a pump.

Etymology (EN): From M.E. pumpe, from M.Du. pompe “water conduit, pipe,” or M.L.G. pumpe “pump.”

Etymology (PE): Pompidan infinitive, from pomp, loan from Fr. pompe

The act or process of pumping. → optical pumping.

See also: Verbal noun of → pump.

The act or process of pumping. → optical pumping.

See also: Verbal noun of → pump.

1. In the → eye, the apparently black opening in the center of the → iris that permits light to pass and be focused on the → retina.
   

2. In a → lens, the → image of the → aperture stop as seen from → object and → image space. Same as → entrance pupil.

Etymology (EN): From M.E. pupille, from O.Fr. pupille, from L. pupilla, originally “little girl-doll,” diminutive of pupa “girl, doll” (Fr. poupée), so called from the tiny image one sees of himself reflected in the eye of another.

Etymology (PE): Mardomak “little man,” the allusion being to the tiny image of himself reflected in the eye of another, from mardom “man, human being, mankind, people;”
→ people, + diminutive suffix -ak.

1. In the → eye, the apparently black opening in the center of the → iris that permits light to pass and be focused on the → retina.
   

2. In a → lens, the → image of the → aperture stop as seen from → object and → image space. Same as → entrance pupil.

Etymology (EN): From M.E. pupille, from O.Fr. pupille, from L. pupilla, originally “little girl-doll,” diminutive of pupa “girl, doll” (Fr. poupée), so called from the tiny image one sees of himself reflected in the eye of another.

Etymology (PE): Mardomak “little man,” the allusion being to the tiny image of himself reflected in the eye of another, from mardom “man, human being, mankind, people;”
→ people, + diminutive suffix -ak.

A method for reaching the → diffraction-limited  → angular resolution of a monolithic telescope by using an → interferometric technique. A mask with several small openings is placed in the telescope pupil plane or in a conjugated plane so as to only pass light from selected regions, thus transforming the telescope into an array of small subapertures without redundancy. When the light from each of these separate subapertures is combined, → interference fringes are formed which encode information on the spatial structure of the source (Haniff et al. 1987, Nature 328, 694).
Coupled with a novel technique which filters the → atmospheric turbulence through fibers, pupil masking allows reaching a high dynamic range (Perrin et al. 2006, MNRAS 373, 747), which is necessary for detecting very faint objects, such as → exoplanets, adjacent to bright stars.

See also: → pupil; → masking.

A method for reaching the → diffraction-limited  → angular resolution of a monolithic telescope by using an → interferometric technique. A mask with several small openings is placed in the telescope pupil plane or in a conjugated plane so as to only pass light from selected regions, thus transforming the telescope into an array of small subapertures without redundancy. When the light from each of these separate subapertures is combined, → interference fringes are formed which encode information on the spatial structure of the source (Haniff et al. 1987, Nature 328, 694).
Coupled with a novel technique which filters the → atmospheric turbulence through fibers, pupil masking allows reaching a high dynamic range (Perrin et al. 2006, MNRAS 373, 747), which is necessary for detecting very faint objects, such as → exoplanets, adjacent to bright stars.

See also: → pupil; → masking.

The Stern. One of the larger constellations of the southern hemisphere representing the stern of the ship Argo Navis, located at 7h 30m right ascension, 40° south declination. Its brightest star is → Naos. Abbreviation: Pup; genitive: Puppis.

Etymology (EN): From L. puppis “stern, poop, the rear, or aft part of a ship or boat.”

Etymology (PE): Pasâl, from pas “behind” (e.g.: pas-e pardé “behind the curtain”), variant pošt “back; the back; behind” (Mid.Pers. pas “behind, before, after;” O.Pers. pasā “after;” Av. pasca “behind (of space); then, afterward (of time);” cf. Skt. paścā “behind, after, later;” L. post, as above; O.C.S. po “behind, after;” Lith. pas “at, by;” PIE *pos-, *posko-) + -âl, → -al. → prow = farâl (فرال).

The Stern. One of the larger constellations of the southern hemisphere representing the stern of the ship Argo Navis, located at 7h 30m right ascension, 40° south declination. Its brightest star is → Naos. Abbreviation: Pup; genitive: Puppis.

Etymology (EN): From L. puppis “stern, poop, the rear, or aft part of a ship or boat.”

Etymology (PE): Pasâl, from pas “behind” (e.g.: pas-e pardé “behind the curtain”), variant pošt “back; the back; behind” (Mid.Pers. pas “behind, before, after;” O.Pers. pasā “after;” Av. pasca “behind (of space); then, afterward (of time);” cf. Skt. paścā “behind, after, later;” L. post, as above; O.C.S. po “behind, after;” Lith. pas “at, by;” PIE *pos-, *posko-) + -âl, → -al. → prow = farâl (فرال).

A → supernova remnant in the constellation → Puppis, and one of the brightest sources in the X-ray sky. The → supernova occurred about 4000 years ago at a distance of about 6,000 light-years.
Also called SNR G260.4-03.4. Its X-ray designation is 2U 0821-42.

See also: → Puppis.

A → supernova remnant in the constellation → Puppis, and one of the brightest sources in the X-ray sky. The → supernova occurred about 4000 years ago at a distance of about 6,000 light-years.
Also called SNR G260.4-03.4. Its X-ray designation is 2U 0821-42.

See also: → Puppis.

The degree to which → impurity is incorporated into a semiconductor material.

Etymology (EN): M.E., from O.Fr. pureté, from L.L. puritatem (nom. puritas) “cleanness, pureness,” from purus “clean;” cf. Av. pūitika- “serving for purification,” Mod.Pers. pâk “clean;” Skt. pavi- “to become clean,” pávate “purifies, cleanses;” O.H.G. fouwen, fewen “to sift;” PIE base *peu- “to purify, cleanse.”

Etymology (PE): Žâvi, noun from adj. žâv “pure.”

The degree to which → impurity is incorporated into a semiconductor material.

Etymology (EN): M.E., from O.Fr. pureté, from L.L. puritatem (nom. puritas) “cleanness, pureness,” from purus “clean;” cf. Av. pūitika- “serving for purification,” Mod.Pers. pâk “clean;” Skt. pavi- “to become clean,” pávate “purifies, cleanses;” O.H.G. fouwen, fewen “to sift;” PIE base *peu- “to purify, cleanse.”

Etymology (PE): Žâvi, noun from adj. žâv “pure.”

The increasing sensibility of the retina for light of shorter wavelength as the brightness decreases. In those conditions red objects are perceived to fade faster than blue objects of the same brightness.

See also: Named after the Czech anatomist Jan Evangelista Purkynne (1787-1869), who discovered the effect; → effect.

The increasing sensibility of the retina for light of shorter wavelength as the brightness decreases. In those conditions red objects are perceived to fade faster than blue objects of the same brightness.

See also: Named after the Czech anatomist Jan Evangelista Purkynne (1787-1869), who discovered the effect; → effect.

The reason for which something exists or is done, made, used, etc. (Dictionary.com).

Etymology (EN): M.E. purpos, from O.Fr. porpos “aim, intention,” from porposer “to put forth,” from por- “forth,” from L. → pro- “forth;” + O.Fr. poser “to put, place,” → position.

Etymology (PE): Farneh, literally “put forth,” from far-, variant of farâ-, → pro-,

• neh present stem of nehâdan “to pose, place, lay,” → position.

The reason for which something exists or is done, made, used, etc. (Dictionary.com).

Etymology (EN): M.E. purpos, from O.Fr. porpos “aim, intention,” from porposer “to put forth,” from por- “forth,” from L. → pro- “forth;” + O.Fr. poser “to put, place,” → position.

Etymology (PE): Farneh, literally “put forth,” from far-, variant of farâ-, → pro-,

• neh present stem of nehâdan “to pose, place, lay,” → position.

Having a purpose; determined; resolute.

Etymology (EN): → purpose + -ful a suffix meaning “full of,” “characterized by.”

Etymology (PE): Farnehmand, from farneh, → purpose, + -mand, → -al.

Having a purpose; determined; resolute.

Etymology (EN): → purpose + -ful a suffix meaning “full of,” “characterized by.”

Etymology (PE): Farnehmand, from farneh, → purpose, + -mand, → -al.

1. Intentionally; deliberately.
   

2. With the particular purpose specified; expressly (Dictionary.com).

See also: → purpose; → -ly.

1. Intentionally; deliberately.
   

2. With the particular purpose specified; expressly (Dictionary.com).

See also: → purpose; → -ly.

1. A problem that cannot be easily or readily solved.
   

2. A game, question, or problem designed for testing ingenuity.

Etymology (EN): Of unknown origin.

Etymology (PE): Cistân from cist “what is?,” + -ân noun suffix.

1. A problem that cannot be easily or readily solved.
   

2. A game, question, or problem designed for testing ingenuity.

Etymology (EN): Of unknown origin.

Etymology (PE): Cistân from cist “what is?,” + -ân noun suffix.