An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



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Number of Results: 160 Search : and
standard temperature and pressure (STP)
  دما و فشار ِ استانده   
damâ o fešâr-e estândé

Fr.: conditions normales de température et de pression   

1) The most commonly used definition is temperature of 273.15 K (0 °C) and pressure of 1 → atmosphere.
2) Chemistry: Temperature of 273.15 K (0 °C) and pressure of 105  → pascal (Pa)s (1 → bar). International Union of Pure and Applied Chemistry (IUPAC) recommends that the former use of the pressure of 1 atm as standard pressure (equivalent to 1.01325 × 105 Pa) should be discontinued.

standard; → temperature; → pressure.

standard time
  زمان ِ استانده   
zamân-e estândé

Fr.: temps standard   

The time in any of the 24 internationally agreed time zones into which the Earth's surface is divided. The primary zone is centered on the Greenwich meridian (0° longitude).

standard; → time.

standard values
  ارزش‌های ِ استانده   
arzešhâ-ye estândé

Fr.: valeurs standard   

Photometric values of selected stars in a standard system.

standard; → value.

standing wave
  موج ِ ایستان   
mowj-e istân

Fr.: onde stationnaire   

A wave produced by the simultaneous transmission of two similar wave motions in opposite directions. Same as stationary wave.

Standing verbal adjective from stand, cognate with Pers. istâdan, as below; → wave.

Istân pr.p. of istâdan "to stand;" Mid.Pers. êstâtan; O.Pers./Av. sta- "to stand, stand still; set;" Av. hištaiti; cf. Skt. sthâ- "to stand;" Gk. histemi "put, place, weigh," stasis "a standing still;" L. stare "to stand;" Lith. statau "place;" O.N. standa, Goth. standan, O.H.G. stantan, Swed. stå, Du. staan, Ger. stehen; O.E. standan; PIE base *sta- "to stand;" mowj, → wave.

super-Chandrasekhar SN Ia
  ابر-نو-اختر ِ گونه‌ی ِ Ia ی ِ ابر-چاندراسکهار   
abar-now-axtar-e gune-ye Ia-ye abar-Chandrasekhar

Fr.: supernova de type Ia super-Chandrasekhar   

A superluminous → Type Ia supernova which is characterized by a bright → light curve peak, a slow light curve evolution during the photospheric phase, and moderately low ejecta velocities. Modeling suggests ejecta masses far in excess of the → Chandrasekhar limit of mass for non-rotating → white dwarfs and the production of about 1.5 Msun of 56Ni. This precludes the interpretation of these events as thermonuclear explosions of Chandrasekhar-mass white dwarfs.

super-; → Chandrasekhar limit.

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.

Swan band
  باند ِ سوان   
bând-e Swan

Fr.: bande de Swan   

One of the three prominent bands in the spectra of comets and carbon stars caused by diatomic carbon (C2).

Named after the Scottish physicist William Swan (1818-1894) who first studied the spectral analysis of radical carbon C2 in 1856; → band.

telluric band
  باند ِ جوّی   
bând-e javvi

Fr.: bande tellurique   

A band seen in the spectra of celestial objects, which is due to absorption by gases such as oxygen, water vapor, and carbon dioxide in the Earth's atmosphere

telluric; → band.

TiO band
  باند ِ TiO   
bând-e TiO

Fr.: bandes TiO   

Any of the several → absorption bands due to the molecule → titanium oxide that are prominent in the spectra of cool → K and → M stars.

titanium oxide; → band.

Tisserand's parameter
  پارامون ِ تیسران   
pârâmun-e Tisserand

Fr.: paramètre de Tisserand   

In celestial mechanics, a combination of orbital elements commonly used to distinguish between comets and asteroids. Objects whose Tisserand's parameter value is smaller than 3 are considered to be dynamically cometary, and those with a value larger than 3 asteroidal. Also called Tisserand's invariant.

Named after François Félix Tisserand (1845-1896), French astronomer, Director of the Paris Observatory (1892).

TRAnsiting Planets and PlanetesImals Small Telescope (TRAPPIST)


A Belgian facility devoted to the detection and characterization of → exoplanets and to the study of → comets (→ transiting planet) and other → small solar system bodies. It consists of two 60 cm robotic telescopes located at the → European Southern Observatory, → La Silla, in Chile and at Oukaïmden Observatory in Marroco.

transit; → planet; → planetesimal; → small; → telescope.

transmission band
  باند ِ تراگسیل   
bând-e tarâgosil (#)

Fr.: bande de transmission   

The frequency range above the cutoff frequency in a waveguide or transmission line.

transmission; → band.

fahmidan (#)

Fr.: comprendre   

To perceive the meaning of.

M.E. understanden, understonden, O.E. understandan "comprehend, grasp the idea of," probably literally "to stand in the midst of," from → under- + standan "to stand," cognate with Pers. istâdan, → standard.

Fahmidan, from Ar. fahm + infinitive suffix -idan.

fahm (#)

Fr.: compréhension, entendement, intelligence   

The ability to understand something; the → power of → abstract  → thought.

understand; → -ing.

Unidentified Infrared Band (UIB)
  باند ِ فروسرخ ِ نا-ایدانیده   
bând-e forusorx-e nâ-idânidé

Fr.: bande infrarouge non identifiée   

A no longer in general use name for → Aromatic Infrared Band.

unidentified; → infrared; → band.

valence band
  باند ِ ارزایی   
bând-e arzâyi

Fr.: bande de valence   

The range of energy states in the spectrum of a solid crystal which includes the energies of all the electrons binding the crystal together.

valence; → band.


Fr.: bande de longueur d'onde   

A portion of the electromagnetic spectrum which is defined because of its characteristics or for its use.

wave; → band.

Werner band
  باند ِ ورنر   
bând-e Werner

Fr.: bande de Werner   

A sequence of → permitted transitions in the → ultraviolet from an → excited state (C) of the → molecular hydrogen (H2) to the electronic → ground state, with ΔE > 12.3 eV and λ ranging from 1160 Å to 1250 Å. When a hydrogen molecule absorbs such a photon, it undergoes a transition from the ground electronic state to the excited state (C). The following rapid → decay creates an → absorption band in that wavelength range. See also → Lyman band; → Lyman-Werner photon.

Named after the Danish physicist Sven Theodor Werner (1898-1984), who discovered the band (S. Werner, 1926, Proc. R. Soc. London Ser. A, 113, 107); → band.

Wing-Ford band
  باند ِ وینگ-فورد   
bând-e Wing-Ford

Fr.: bande de Wing-Ford   

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.

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

ZrO band
  باند ِ ZrO   
bând-e ZrO

Fr.: bande ZrO   

Any of the three → absorption bands due to the molecule → zirconium oxide present in the blue and visual spectral regions → S-type stars. The bands are centered on the wavelengths 4614, 5551, and 6468 Å.

zirconium oxide; → band.

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