An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



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Number of Results: 602
infrared galaxy
  کهکشان ِ فروسرخ   
kahkešân-e forusorx (#)

Fr.: galaxie infrarouge   

A galaxy that emits most of its energy in the infrared region of the spectrum. Such galaxies are thought to have unusually high rates of star formation and are also described as → starburst galaxies.

infrared; → galaxy.

infrared imaging
  تصویرگری ِ فروسرخ   
tasvirgari-ye forusorx (#)

Fr.: imagerie infrarouge   

Imaging with an infrared detector.

infrared; → imaging.

infrared radiation
  تابش ِ فروسرخ   
tâbeš-e forusorx (#)

Fr.: rayonnement infrarouge   

That part of the → electromagnetic radiation lying beyond the red, between the radio and the visible regions of the → electromagnetic spectrum. The wavelengths range from about 0.8 → microns (μm) to about 1000 μm. See also: → near-infrared; → mid-infrared; → far-infrared; → submillimeter radiation.

infrared; → radiation.

Infrared Space Observatory (ISO)
  نپاهشگاه ِ فضایی ِ فروسرخ   
nepâhešgâh-e fazâyi-ye forusorx

Fr.: Satellite ISO   

A European Space Agency satellite which carried the most sensitive infrared telescope ever launched. It operated between November 1995 and April 1998 and made particularly important observations of the dusty regions of the Universe. ISO was equipped with four science instruments: an infrared camera (CAM), a long-wavelength spectrometer (LWS), a photo-polarimeter (PHT), and a short-wavelength spectrometer (SWS). The instruments jointly covered wavelengths from 2.5 to around 240 microns with spatial resolutions ranging from 1.5 arcseconds to 90 arcseconds. Its 60 cm diameter telescope was cooled by superfluid liquid helium to temperatures of 2-4 K. The mission was a great technical, operational and scientific success. During its routine operational phase, ISO successfully made some 30,000 individual imaging, photometric, spectroscopic, and polarimetric observations ranging from objects in our own solar system to the most distant extragalactic sources.

infrared; → space; → observatory.

infrared survey
  بردید ِ فروسرخ   
bardid-e forusorx

Fr.: relevé infrarouge   

Observing a large area of sky (or the whole sky) in infrared wavelengths.

infrared; → survey.

infrared telescope
  دوربین ِ فروسرخ، تلسکوپ ِ ~   
durbin-e forusorx (#), teleskop-e ~ (#)

Fr.: télescope infrarouge   

A telescope capable of observing → infrared radiation from astronomical objects.

infrared; → telescope.

infrared window
  روزنه‌ی ِ فروسرخ   
rowzane-ye forusorx (#)

Fr.: fenêtre infrarouge   

A range of infrared wavelengths to which the Earth's atmosphere is relatively transparent, and at which observations can be made from the ground. Infrared windows are found near wavelengths of 1.25, 1.65, 2.2, 3.6, 5.0, 10, 20, and 30 microns, and beyond 300 microns.

infrared; → window.


Fr.: infra-son   

A sound wave whose frequency is below the audible range of about 20 → Hz to 20,000 Hz. → sound wave; → ultrasound; → subsonic.

infra- + → sound.


Fr.: ingrédient   

That which enters into a → compound or → mixture.

M.E., from L. ingredient- (nominative ingrediens) "that which enters into," p.p. of ingredi "to go in, enter," from → in- + gradi "to go, to walk," → egress.

Darâné, literally "brought into," from dar-, → in-, + ân present stem of ânidan "to bring, to lead," → relate, + nuance suffix .


Fr.: immersion   

Same as → immersion.

From → in- + gress, → egress.

  ریگن بردن، دریگیدن   
rigan bordan, darigidan

Fr.: hériter   

To take or receive (property, a right, a title, etc.) by succession or will, as an → heir (


  ریگن‌بردنی، دریگیدنی   
riganbordani, darigidani

Fr.: dont on peut hériter, qui peut hériter   

1) Capable of being inherited.
2) Capable of inheriting; qualified to inherit (

inherit; → -able.

  ریگن‌برد، ریگنبرد، دریگش   
riganbord, darigeš

Fr.: hériter   

1) Something that is or may be inherited; property passing at the owner's death to the heir or those entitled to succeed; legacy; something, as a quality, characteristic, or other immaterial possession, received from progenitors or predecessors as if by succession.
2) The genetic characters transmitted from parent to offspring, taken collectively.
3) The act or fact of inheriting by succession, as if by succession, or genetically (

Verbal noun of → inherit.

  ریگن‌بر، ریگنبر   

Fr.: héritier   

A person who → inherits; → heir.

inherit; → -or.

nâhamgeni (#)

Fr.: inhomogénéité   

The condition or an instance of not being homogeneous.

in- "not" + → homogeneity.

nâhamgen (#)

Fr.: inhomogène   

Lack of homogeneity; something that is not → homogeneous.

in- "not" + → homogeneous.

âqâzin (#)

Fr.: initial   

Of, pertaining to, or occurring at the beginning.

Initial, from L. initialis, from initium "a beginning, an entrance," from p.p. stem of inire "to go into, begin," from → in- + ire "to go," → ion.

Âqâzin "pertaing to the beginning," from âqâz "beginning," from Proto-Iranian *āgāza-, from prefix ā- + *gāz- "to take, receive," cf. Sogdian āγāz "beginning, start," pcγz "reception, taking."

initial conditions
  بوتارهای ِ آغازین   
butârhâ-ye âqâzin

Fr.: conditions initiales   

1) Conditions at an initial time t = t0 from which a physical system or a given set of mathematical equations evolves.
2) Meteo.: A prescription of the state of a → dynamical system at a specified time; for all subsequent times, the → equation of motion and → boundary conditions determine the state of the system.

initial; → condition.

initial mass
  جرم ِ آغازین   
jerm-e âqâzin (#)

Fr.: masse initiale   

The mass of a star at its arrival on the → main sequence.

initial; → mass.

initial mass function (IMF)
  کریا‌ی ِ آغازین ِ جرم   
karyâ-ye âqâzin-e jerm

Fr.: fonction initiale de masse   

A mathematical expression describing the relative number of stars found in different ranges of mass for a cluster of stars at the time of its formation. It is defined as φ(log M) = dN / dlog M ∝ M, where M is the mass of a star and N is the number of stars in a logarithmic mass interval. The value of the slope found by Salpeter (1955) for → low-mass and → intermediate-mass stars in the → solar neighborhood is Γ = 1.35. The IMF can be expressed also in linear mass units: χ(M) = dN / DM ∝ M. Note that χ(M) = (1 / M lm 10) φ(log M), and α = Γ + 1. In this formalism the Salpeter slope is α = 2.35. There is a third way for representing the IMF, in which the exponent is x = -α. The IMF is not a single power law over all masses, from → brown dwarfs to → very massive stars (Kroupa, 2002, Science 295, 82). Different slopes have been found for different mass segments, as follows: α = 1.3 for 0.08 ≤ Msolar < 0.5; α = 2.3 for 0.5 ≤ Msolar < 1; α = 2.3 for 1 ≤ Msolar. The IMF at low masses can be fitted by a → lognormal distribution (See Bastian et al., 2010, ARAA 48, 339 and references therein). See also → canonical IMF.

initial; → mass; → function.

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