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: 13176 Search : in
setup
  بربشت   
barbešt

Fr.: installation   

1) The process of connecting and preparing a software program, hardware device, or computer to function properly. Setup is a file commonly called "setup.exe" that is executed to begin installing a software program onto a computer. See also → set up.
2) Equipment designed for a particular purpose; an apparatus.
3) The fashion in which something is organized or arranged.

set; → up.

Barbešt, from prefix bar-, → on-.

seven
  هفت   
haft (#)

Fr.: sept   

A → cardinal number between → six and → eight.

From M.E. seoven(e), seofne, seven, O.E. seofon, cognate with M.Du. seven, Du. zeven, O.H.G. sibun, Ger. sieben, related to Pers. haft, as below, from PIE *septm "seven."

Haft, from Mid.Pers. haft, Av. hapta Skt. sapta, Gk. hepta, L. septem.

sexagesimal
  شست-شستی   
šast-šasti (#)

Fr.: sexagésimal   

Relating to, or based on, the number 60.

From M.L. sexagesimalis, from L. sexagesimus "sixtieth," from sexaginta "sixty."

Šast-šasti, from Šast, → sixty.

sexagesimal system
  راژمان ِ شست-شستی   
râžmân-e šast-šasti

Fr.: système sexagésimal   

A number system whose base is 60. It originated with the ancient Sumerians around 2000 B.C., was transmitted to the Babylonians, and is still used in modified form for measuring time, angles, and geographic coordinates.

sexagesimal; → system.

Sextans
  ششکان   
Šešakân

Fr.: Sextant   

The Sextant. An inconspicuous constellation located on the celestial equator at 10h 20m, 0° declination. Its brightest star, Alpha Sextantis is of 4th magnitude. It was introduced in the 17th century by Johannes Hevelius (1611-1687). Abbreviation: Sex; genitive: Sextantis.

The name is L. for → sextant, an instrument that Hevelius made frequent use of in his observations.

sextant
  ششکان   
šešakân

Fr.: sextant   

An instrument used mainly in nautical astronomy to determine the angular distances of celestial bodies above the horizon. The sextant consists of a 60° graduated arc, or limb, a small telescope, and two mirrors. Only half of one of the mirrors, the horizon glass, is silvered and, like the telescope, it is fastened to the frame supporting the limb. The other mirror, the index mirror, moves with an index arm pivoted at the center of the arc. The index arm is equipped with a → vernier which moves along the limb. An object in direction S can be observed in the telescope through the un-silvered portion of the horizon glass. By moving the index arm, the second object S' is made to coincide with S in the telescope. According to the law of reflection, the angle between S and S' is double the angle between the mirrors. The angular distance between the objects can therefore be obtained from the measurement of angles between the planes of the mirrors.

From Mod.L. sextans, from L. sextans "a sixth," from sexsix.

Šešakân, from šešak "a sixth," from šeš, → six + -ak, contraction of yak "one," (Mid.Pers. êwak; Proto-Iranian *aiua-ka-; O.Pers. aiva- "one, alone;" Av. aēuua- "one, alone" (cf. Skt. éka- "one, alone, single;" Gk. oios "alone, lonely;" L. unus "one;" E. one) + -ân nuance suffix.

sextet
  شش‌تایه   
šeštâyé

Fr.: sextet   

Any group or set of six. → Seyfert's sextet.

From Latinized sestet, from It. sestetto, diminutive of sesto "sixth," from L. sextus "sixth," from sex, → six.

Šeštâyé, from šeš, → six, + "fold, plait, ply; piece, part" (Mid.Pers. tâg "piece, part") + -(y)é nuance suffix.

sextuplet
  ششتایی   
šeštâyi

Fr.: sextuplet   

A group or combination of six objects, such as the → Mizar and the → Castor star systems.

From sextuple, from L. sext(us) "sixth," → six, + et

Seyfert galaxy
  کهکشان ِ سیفرت   
kahkešân-e Seyfert

Fr.: galaxie de Seyfert   

A member of an important class of → active galaxies which are characterized by the presence of an intensely bright nucleus in the optical wavelengths (109-1012Lsun) displaying emission spectral lines. The presence of these emission features, which are not seen in the spectra of normal galaxies, indicates a very high degree of ionization. Moreover, the nucleus radiates → non-thermal  → continuum emission extending over the whole electromagnetic spectrum. It is thought that a → massive black hole in the nucleus of a galaxy accretes gas (→ accretion) from its surrounding environment to power Seyfert galaxies. These galaxies are divided into two types according to the width of their spectral lines. Type 1 Seyfert (Sy 1) galaxies have very broad emission lines (103- 104 km s-1), while Type 2 Seyferts (Sy 2) show relatively narrow lines (several hundred km s-1). These spectral differences may be the result of viewing the nucleus from different angles. A Type 2 Seyfert galaxy may be a mostly edge-on view of matter spiraling in toward the supermassive black hole, whereas a Type 1 Seyfert provides a more pole-on view, allowing us to see the more turbulent region around the black hole.

Named after Carl Keenan Seyfert (1911-1960), the American astronomer who first identified this type of galaxies in 1943; → galaxy.

Seyfert's sextet
  شش‌تایه‌ی ِ سیفرت   
Šeštâye-ye Seyfert

Fr.: Sextette de Seyfert   

A group of galaxies about 190 million → light-years away in the head portion of the constellation → Serpens. The group appears to contain six members, but actually contains only four → interacting galaxies. A face-on → spiral galaxy lies in the distant background and appears only by chance aligned with the main group. Also, a prominent condensation is likely not a separate galaxy, but a → tidal tail of stars flung out by the galaxies' gravitational interactions. The interacting galaxies are tightly packed into a region around 100,000 light-years across, comparable to the size of our own Milky Way galaxy, making this one of the densest known galaxy groups.

Discovered by the American astronomer Carl Keenan Seyfert (1911-1960) using photographic plates made at the Barnard Observatory of Vanderbilt University. → sextet.

Sgr A*
     
Sgr A*

Fr.: Sgr A*   

The object identified as the Galactic → supermassive black hole.

Sagittarius A (Sgr A).

Sgr A* cluster
  خوشه‌ی ِ *Sgr A   
xuše-ye Sgr A*

Fr.: amas Sgr A*   

Same as → S cluster.

Sgr A*; → cluster.

Sh2-279
     
Sh2-279

Fr.: Sh2-279   

A large → H II region in the north part of → Orion's Sword composed of reflection and emission components ( → reflection nebula, → emission nebula). It includes NGC 1977, NGC 1975, and NGC 1973, separated from each other by a → dark nebula which resembles a running man, as well as the → open cluster NGC 1981. NGC 1977, the designation some sources use to describe the entire complex, is the largest and brightest nebulous component first described by Herschel in 1786. The nebula is approximately 40 arcmin in apparent diameter, and 1,500 → light-years distant.

Nebula number 279 in the second edition of the → Sharpless catalog.

Shack-Hartmann wavefront sensor
  حسگر ِ پیشان ِ موج ِ شک-هارتمان   
hessgar-e pišân-e mowj-e Shack-Hartmann

Fr.: analyseur de front d'onde   

An optical device, a modern version of the → Hartmann test, used for analyzing the wavefront of light. Theses sensors can be used to characterize the performance of optical systems. Moreover, they are increasingly used in real-time applications, such as → adaptive optics to remove the wavefront distortion before creating an image. It consists of a microlens array placed in front of a CCD array. A planar wavefront that is transmitted through a microlens array and imaged on the CCD array will form a regular pattern of bright spots. If, however, the wavefront is distorted, the light imaged on the CCD will consist of some regularly spaced spots mixed with displaced spots and missing spots. This information is used to calculate the shape of the wavefront that was incident on the microlens array.

Named after the German astronomer Johannes Hartmann (1865-1936), who first developed the method, and R. V. Shack, who in the late 1960s replaced the screen by a microlens array; → wavefront; → sensor.

shade
  سیوان   
sivân

Fr.: ombre   

1) The comparative darkness caused by the interception or screening of rays of light from an object, place, or area.
2) A place or an area of comparative darkness, as one sheltered from the sun (Dictionary.com). See also → shadow.

M.E. schade; O.E. scead "partial darkness; shelter," → shadow.

Sivân, from Kurd. sayvân "shadow, shade," variants si, sâ, sâyé, → shadow.

shadow
  سایه   
sâyé (#)

Fr.: ombre   

A dark patch formed by a body which obstructs rays of light.

M.E. sch(e)adew(e), schadow, shadw(e), O.E. sceadwe, sceaduwe, sceadu "shade, shadow, darkness;" cf. O.S. skado, M.Du. scade, Du. schaduw, O.H.G. scato, Ger. Schatten, Goth. skadus; from PIE base *skot- "dark, shade."

Sâyé "shadow," from Mid.Pers. sâyak "shadow;" Av. a-saya- "throwing no shadow;" Skt. chāya- "shadow;" Gk. skia "shade;" Rus. sijat' "to shine;" M.H.G. schinen, O.H.G. skinan, Ger. Schein "glow, shine;" PIE base *skai- "bright."

shadow bands
  نوارهای ِ سایه، باندهای ِ ~   
navârhâ-ye sâyé, bândhâ-ye ~

Fr.: ombres volantes   

Faint wavy lines of alternating light and dark that sometimes can be seen on flat, light-colored surfaces just before and just after a total solar eclipse. The phenomenon results from sunlight distortion by irregularities in the Earth's atmosphere.

shadow; → band.

shadow cone
  مخروط سایه   
maxrut-e sâyé

Fr.: cône d'ombre   

A cone-shaped shadow cast by Earth or the Moon pointing away from the Sun. The dark inner portion of the shadow cone is called the → umbra. The lighter outer portion of the shadow is called the → penumbra. Its extension is called the → antumbra.

shadow; → cone.

shale
  اردوال   
ardavâl (#)

Fr.: schiste, schiste argileux   

A fissile rock composed mostly of layers of clay-like, fine-grained → sediments. Shale is the most frequently occurring → sedimentary rock.

Probably from obsolete or dialect shale "scale, shell," from M.E., from O.E. scealu, → rock.

Ardavâl "shale," in the dialectal Mod.Pers. of Golpâyegân, Arâk, Xonsâr, etc.

shallow
  نژل   
nažal

Fr.: peu profond   

Of little depth; not deep.

M.E. schalowe, akin to O.E. sceald "shallow."

Nažal, from negation prefix na-, → non-, + žal "deep," variant of jal, jol, jul, → deep.

<< < -es -it -sc 201 951 abe abs abs aca acc acc aco act ada adh ado aer aft air Alf alg alk alp Alt alt amb ana And ang ani ann ant ant ant apo app app Apu arc arg Arn art ass ast ast ast atm ato att aur aut avo azi bac bal bar bar bat Bea Bel bet bia big bin bio Bir bla bla blo Blu bol Boo bou box bre Bri bro bur cal cal Can cap car Car cat cau cel cen cen cha Cha cha che Chi chr cir cir civ cla clo clo CMB coa coe coh col col col com com com com com com com com Com con con con con con con con con con con con con coo cor cor cor Cos cos cos cou cou cra cri cro cry cul cur cyc D l dar dat day dea dec dec dec def def deg Del Den dep der det deu dew dic dif dif dil dip dir dis dis dis dis dis diu dog Dop dou Dra Dsc dus dwa dyn Dys Ear ecc eco edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ eru eth Eur eve exa exc exe exi exo exp ext ext ext fab fai Fan fea fem fer fie fil fir fir fla fli flu foc for for for fra fre fre fri fun fuz gal gal gal Gam gau Gau gen geo geo geo geo Gib glo gov gra gra gra gra gre gro Gui H-a hal Ham har Hay hea hei hel Hel her het hie hig hoa hom hor hot Hub Hug hur hyd hyd hyl hyp ice ide ima ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv inv ion iro Isl iso iso Jab jet Jov Jup Kar Kep kil Kip Kra Lag Lam Lan Lar las law lea Leg Leo lev lig lim lin lin lin lit loc loc log Lor low lum lun lun Lym Mac mag mag mag mag mag mai Mal map mas mas mat Mau mea mea med Men mer Mes Met met mic mic Mie mil min Mir mix mod mol mom Moo mor mov mul mur n-b nan nat nea neg Ner neu new New NGC noc nom non non nor nor nuc nuc nul nut obj obl obs occ oct off old one ope opp opt opt orb ord org Ori osc oth ove Owl P-s Pal par par par par Pas pat pec pen per per per per per Pha pha pho pho pho phy pie pix Pla pla pla pla Pli Poi pol pol pol pol por pos pos pow pre pre pre pre pri pri pri pro pro pro pro pro pro pro pub pul pyc qua qua qua qua qui rad rad rad rad rad rad rai ran rar Ray rea Rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot rur S5- Sal sat sca sca Sch sci Scu sec sec sed sel sel sem seq set sha she sho sid sie sil sim sin sit sky slo sno sod sol sol sol sol son sou spa spa spe spe spe spe sph spi spo squ sta sta sta sta ste ste ste Sti sto str str sub sub sub sul sup sup sup sup sur sur syl syn sys tal Tay tel ten ter tex the the the the Tho thr tid tim Tit too Tor tra tra Tra tra Tra tri Tri tru tub tur two Typ ult ult unc uni uni uni upl ura uti val var vec vel ver Ver vie vir vis vis vol W-R war wav wav wea Wei wha wid win WN3 Wol wri xen yok zen zij > >>