An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



<< < abs arg Cop dis Ham hyp int Mod per per per per per per pro Sma sup sup sup tem upp > >>

Number of Results: 420 Search : per
proton temperature
  دمای ِ پروتونی   
damâ-ye protoni

Fr.: température protonique   

The temperature in the → solar wind, as derived from the mean kinetic energy of protons: mv2/2 = (3/2)kTp, where k is → Boltzmann's constant. There are two types of proton temperature: parallel temperature, measured from protons moving parallel to the magnetic field, and perpendicular temperature relating to protons at right angles to the magnetic field. The proton temperature is usually derived using particle detectors on board space probes that determine the velocity → distribution function of the particles from their energies (N. Meyer-Vernet, 2007, Basics of the Solar Wind, Cambridge Univ. Press). See also → electron temperature.

proton; → temperature.

pulsational pair-instability supernova
  ابر-نووای ِ ناپایداری ِ تپشی ِ جفت، اَبَر-نو‌اختر ~ ~ ~   
abar-novâ-ye nâpâydâri-ye tapeši-ye joft, abar-now-axtar-e ~ ~ ~

Fr.: supernova à instabilité pulsationnelle de paires   

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.

pulsational; → pair; → instability.

quantum-mechanical operator
  آپارگر ِ مکانیک ِ کو‌آنتومی   
âpârgar-e mekânik-e kuântomi

Fr.: opérateur en mécanique quantique   

A linear → Hermitian operator associated with a physical quantity.

quantum; → mechanics; → operator.

quasiperiodic motion
  جنبش ِ چونان-دوره‌ای   
jonbeš-e cunân-dowreyi

Fr.: mouvement quasipériodique   

In a dynamical system, a form of motion that is regular but never exactly repeating. Quasiperiodic motion appears when the system contains two or more incommensurate frequencies.

quasi-; → periodic; → motion.

Quaternary period
  دوران ِ چهارم   
dowrân-e cahârom

Fr.: quaternaire   

The last two million years of geologic time, comprising the Pleistocene and Holocene glacial epochs. Estimates of the date of the beginning of the Quaternary vary between 2.5 and 1.6 million years ago.

Quaternary, from L. quaternarius "consisting of four," from quatern(i) "fourt at a time" + -arius "-ary;" → period.

Dowrân, → period; cahârom "fourth," from cahâr "four" + -om "-th."

radiation temperature
  دمای ِ تابش   
damâ-ye tâbeš

Fr.: température de rayonnement   

The temperature of a source calculated assuming that it behaves as a → blackbody that radiates with the same intensity at the same frequency. Compared to the → effective temperature, the radiation temperature is measured over a narrow region of the → electromagnetic spectrum.

radiation; → temperature.

random experiments
  آزمایش‌های ِ کاتوره   
âzmâyešhâ-ye kâturé (#)

Fr.: expériences aléatoires   

Statistics: Experiments in which results will not be essentially the same even though conditions may be nearly identical.

random; → experiment.

real-time operation
  آپارش در زمان ِ هسیا   
âpâreš dar zamân-e hasyâ

Fr.: opération en temps réel   

The operation of a computer during the actual time that the related physical processes take place so that the results can be used to guide the physical processes.

real; → time; → operation.

red supergiant
  ابَرغول ِ سرخ   
abarqul-e sorx (#)

Fr.: supergéante rouge   

A supergiant star with spectral type K or M. Red supergiants are the largest stars in the Universe, but not necessarily the most massive. Betelgeuse and Antares are the best known examples of a red supergiant.

red; → supergiant.

relative permeability
  تراوایی ِ بازانی   
tarâvâyi-ye bâzâni

Fr.: perméabilité relative   

magnetic permeability.

relative; → permeability.

rotation period
  دوره‌ی ِ چرخش   
dowre-ye carxeš (#)

Fr.: période de rotation   

The interval of time during which an object turns once about its axis.

rotation; → period.

rotational period
  دوره‌ی ِ چرخش   
dowre-ye carxeš

Fr.: période de rotation   

rotation period.

rotational; → period.

scalar perturbation
  پرتورش ِ مرپلی   
partureš-e marpeli

Fr.: perturbation scalaire   

The energy density fluctuations in the → photon-baryon plasma that bring about hotter and colder regions. This perturbation creates velocity distributions that are out of phase with the acoustic density mode. The fluid velocity from hot to cold regions causes blueshift of the photons, resulting in → quadrupole anisotropy.

scalar; → perturbation.

secular perturbation
  پرتورش ِ دیریاز   
partureš-e diryâz

Fr.: perturbation séculaire   

A variation of planetary orbital elements which is always in the same direction as time increases.

secular; → perturbation.

Shapley supercluster
  ابرخوشه‌ی ِ شپلی   
abarxuše-ye Shapley

Fr.: superamas de Shapley   

The richest → supercluster of galaxies in the nearby → Universe at a → redshift going from z ~0.03 to z ~0.05 (680 million → light-years), and extending over several square degrees on the plane of the sky. It lies behind the → Centaurus supercluster. Also called the Shapley concentration, it is made up of 25 → galaxy clusters with a total mass of about 1016solar masses. At the core of the Shapley supercluster is a remarkable complex formed by several rich clusters of galaxies from the → Abell catalog; the central and most massive of them is A3558.

Shapley's wing; → supercluster

short-period comet
  دنباله‌دار ِ کوتاه-دوره   
dombâledâr-e kutâh-dowré

Fr.: comète à courte période   

A comet with a period less than 200 years. Same as → periodic comet.

short; → period; → comet.

short-period variable
  ورتنده‌ی ِ کوتاه-دوره   
vartande-ye kutâh-dowré

Fr.: variable à courte période   

A variable star that has a relatively short period with respect to stars of similar types.

short; → period; → variable.

sidereal period
  دوره‌ی ِ اختری   
dowre-ye axtari (#)

Fr.: période sidérale   

sidereal revolution period; → sidereal rotation period.

sidereal; → period.

sidereal revolution period
  دوره‌ی ِ گردش ِ اختری   
dowre-ye gardeš-e axtari (#)

Fr.: période de révolution sidérale   

The time taken by a planet or satellite to complete one revolution about its primary with respect to stars. For Earth, same as → sidereal year. Sidereal periods of the solar system planets, interms of the sidereal year, are as follows: Mercury 0.240846 (87.9691 days); Venus 0.615 (225 days); Earth 1 (365.25636 solar days); Mars 1.881; Jupiter 11.86; Satrurn 29.46; Uranus 84.01; and Neptune 164.8. That of the Moon is 0.0748 (27.32 days) and for → Sedna 12050.

sidereal; → revolution; → period.

sidereal rotation period
  دوره‌ی ِ چرخش ِ اختری   
dowre-ye carxeš-e axtari

Fr.: période de rotation sidérale   

The rotation period of a celestial body with respect to fixed stars. For Earth, same as → sidereal day.

sidereal; → rotation; → period.

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