An Etymological Dictionary of Astronomy and Astrophysics
English-French-Persian

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 1381
superheterodyne receiver
  گیرنده‌ی ِ اَبَر-هترودینی   
girande-ye abar-heterodini (#)

Fr.: récepteur superhétérodyne   

A radio receiver which uses the → superheterodyne technique.

super-; → heterodyne; → receiver.

superheterodyne technique
  تشنیک ِ اَبَر-هترودین   
tašnik-e abar-heterodin

Fr.: technique superhétérodyne   

The technique used in a radio receiver in which the frequency of an incoming signal is changed by adding it to a signal generated within the receiver to produce fluctuations or beats of a frequency equal to the difference between the two signals. See also → mixer.

superheterodyne receiver; → technique.

superion
  ابریون   
abaryon

Fr.: superion   

An ion which is responsible for the existence of a strong → P Cygni profile observed in many early O stars. Since the → effective temperature of the star is too low to produce such an ion appreciably, the ion is termed a superion. For example, the ion O5+ which is at the origin of a strong O VI λλ1031, 1038 P Cygni profile observed in many O stars. Similarly, the lines due to N V λλ1238, 1242 belong to the superion category, while in later spectral types C IV λλ1548, 1552 also falls into this category. Initial modeling of the → ultraviolet line superions assumed the → stellar winds were smooth and homogeneous. However it is now generally accepted that the winds are (→ clumped wind), and this can have a profound influence on the formation of the superion profiles. We know that the strength of lines due to the superions is strongly influenced by the → interclump medium. Indeed, the interclump medium may be more important for producing the lines than are the clumps -- this is simply a consequence of the higher ionization in the interclump medium which occurs because of its lower density (see D. John Hillier, 2020, https://www.mdpi.com/2075-4434/8/3/60/htm, and references therein).

super-; → ion.

superior
  زبرین   
zabarin (#)

Fr.: supérieur   

Upper or situated higher up in rank, degree, etc.

M.E., from O.Fr., from L. superiorem (nominative superior) "higher," comparative of superus "situated above, upper," from super "above, over," → super-.

Zabar, from Mid.Pers. azabar "above," related to abar (Mod.Pers. bar- "on, upon, up"); O.Pers. upariy "above; over, upon, according to;" Av. upairi "above, over," upairi.zəma- "located above the earth;" cf. Gk. hyper- "over, above;" L. super-, as above; O.H.G. ubir "over" + -in comparative suffix.

superior conjunction
  هم‌ایستان ِ زبرین   
hamistân-e zabarin

Fr.: conjonction supérieure   

The conjunction of a planet with the Sun which occurs when the planet is beyond the Sun. → inferior conjunction.

superior; → conjunction.

superior culmination
  بالست ِ زبرین   
bâlest-e zabarin

Fr.: culmination supérieure   

The meridian transit of a star between the celestial pole and the south point of the horizon. Same as → upper culmination. → inferior culmination.

superior; → culmination.

superior planet
  سیاره‌ی ِ زبرین   
sayyâre-ye zabarin

Fr.: planète supérieure   

A planet whose orbit lies outside that of the Earth. The superior planets are Mars, Jupiter, Saturn, Uranus, and Neptune. → planet.

superior; → planet.

superluminal motion
  جنبش ِ اَبَر-نوری   
jonbeš-e abar-nuri

Fr.: mouvement superluminal   

Apparent proper motion exceeding the velocity of light seen toward certain astronomical objects, such as the jets of radio galaxies and quasars. However, these jets are not actually moving at speeds in excess of the speed of light: the apparent superluminal motion is a projection effect caused by objects moving near the speed of light and at a small angle to the line of sight.

super-; luminal, from → lumen; → motion.

Jonbeš, → motion; abarsuper-; nur, → light.

superluminous
  ابر-تابان   
abartâbân

Fr.: superlumineux   

The quality of an object whose luminosity exceeds a certain value.

super-; → luminous.

superluminous supernova
  ابر-نو-اختر ِ ابر-تابان   
abarnowaxtar-e abartâbân

Fr.: supernova superlumineuse   

A → supernova with an → absolute magnitude of about -22 in optical. Examples of these newly discovered SNe include SN 2006gy, SN 2005ap, and SNe 2003ma. The nature of these objects is poorly known. Some of them are powered by the circumstellar interaction, or by the shock breakout from the dense circumstellar medium, as suggested by the presence of narrow emission lines in superluminous → Type II-N supernovae. It is also argued that superluminous SNe could be powered by a large amount of 56Ni which is synthesized as a result of energetic → core-collapse supernovae. Other scenarios include the interaction between shells ejected by the pulsational → pair-instability. See, e.g. Tanaka et al. 2012, MNRAS 422, 2675, arXiv:1202.3610, and references therein.

superluminous; → supernova.

supermassive
  اَبَر-پرجرم   
abar-porjerm

Fr.: supermassif   

Having a mass highly exceeding a certain limit. → supermassive black hole, → supermassive neutron star, → supermassive star.

super-; → massive.

supermassive black hole (SMBH)
  سیه‌چال ِ اَبَر-پرجرم   
siyahcâl-e abar-porjerm

Fr.: trou noir supermassif   

A → black hole of tremendous mass, equivalent to those of millions or even billions of stars, which is believed to exist and occupy the centers of many galaxies. The supermassive black hole residing in the center of our → Milky Way Galaxy is the object → Sgr A* with a mass of 4 x 106solar masses within a radius of 100 → astronomical units.

supermassive; → black hole.

supermassive neutron star
  ستاره‌ی ِ نوترونی ِ ِ اَبَر-پرجرم   
setâre-ye notroni-ye abar-porjerm

Fr.: étoile à neutron supermassive   

A → neutron star of mass above the typical value that is temporarily prevented from → collapseing into a → black hole because of its rapid → rotation.

supermassive; → neutron; → star.

supermassive star
  ستاره‌ی ِ اَبَر-پرجرم   
setâre-ye abar-porerm

Fr.: étoile supermassive   

A star with an initial mass over about 120 solar masses. The existence of such stars is the present Universe is not confirmed. Such stars were proposed as an explanation for very bright O type stars in the Large Magellanic Cloud, but these are now known to be clusters of ordinary O stars. → very massive star; → massive star.

supermassive; → star.

supermoon
  ابرمانگ   
abarmâng

Fr.: super lune   

Same as → perigee full Moon.

super-; → moon.

supermultiplet
  اَبَر-بستایه   
abar-bastâyé

Fr.: supermultiplet   

A generalization of the concept of multiplet to the case when there are several quantum numbers that describe the quantum-mechanical states.

super-; multiplet.

supernatural
  ابر-زاستاری   
abar-zâstâri

Fr.: supernaturel   

1) Of, pertaining to, or being above or beyond what is natural; unexplainable by natural; abnormal.
2) Of, pertaining to, characteristic of, or attributed to God or a deity (Dictionary.com).

super-; → natural.

supernaturalism
  ابر-زاستارگرایی، ابر-زاستارباوری   
abar-zâstâr-gerâyi, abar-zâstâr-bâvari

Fr.: supernaturalisme   

Belief in the doctrine of supernatural or divine agency as manifested in the world, in human events, religious revelation, etc. (Dictionary.com).

super-; → naturalism.

supernova
  اَبَر-نووا، اَبَر-نو‌اختر   
abar-novâ, abar-now-axtar

Fr.: supernova   

A violent stellar explosion which blows off all or most of the star's material at high velocity leaving a compact stellar remnant such as a → neutron star or → black hole. At → maximum light, the supernova can have → luminosity about 108 or 109 times the → solar luminosity. The phenomenon results from the later evolution of stars when an instability sets in the core following the → nucleosynthesis of → iron. In → massive stars, the supernova occurs when the star has used up all its available → nuclear fuel and it reaches a lower energy state through → gravitational collapse to form a more compact object. In → white dwarfs forming → binary systems, → accretion of mass onto the surface of a neutron star can be sufficient to take the star over the upper mass limit for stability as a white dwarf. Consequently, the white dwarf collapses in a → supernova explosion to form a neutron star. There are several → supernova types.

super-; → nova.

supernova candidate
  نامزد ِ اَبَر-نو‌اختر   
nâmzad-e abar-now-axtar

Fr.: candidat supernova   

A star which according to observational data could become a supernova.

supernova; → candidate.

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