An Etymological Dictionary of Astronomy and Astrophysics

فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory



Number of Results: 7 Search : owl

Fr.: reconnaître   

1) To admit to be real or true; recognize the existence, truth, or fact of.
2) To recognize the authority, validity, or claims of.
3) To show or express appreciation or gratitude for (

A blend of M.E aknow "admit or show one's knowledge" (from O.E. oncnawan "understand") and M.E. knowlechen "to admit."

Âdânidan, from âdân, from prefix â- + dân present stem of dânestan, → know; cf. Sogd. âzân, azân "to acknowledge, to confess," from prefixed zân, variant of dân.

  ۱، ۲) آدانش؛ ۲) سپاسگزاری   
1, 2) âdâneš 2) sepâsgozâri

Fr.: 1) reconnaissance, aveu; 2) remerciement   

1) Recognition of the existence or truth of something.
2) An expression of appreciation (

acknowledge; → -ment.

Cowling model
  مدل ِ کاؤلینگ   
model-e Cowling

Fr.: modèle de Cowling   

A model of the internal structure of → massive stars in which a → convective core is surrounded by a large → radiative envelope. However, recent studies point to the presence of a thin → convection zone in the outer envelope of hot massive stars, beneath the → photosphere, which is caused by opacity peaks associated with iron and helium ionization. See also → iron convection zone.

After Thomas Cowling (1906-1990), a British astronomer, who put forward the model; → model.

  ۱،۲) شناخت؛ ۲) دانستگان   
1, 2) šenâxt (#); 2) dânestgân

Fr.: connaissance   

1) Acquaintance with facts, truths, or principles, as from study or investigation.
2) All the information, facts, truths, and principles learned throughout time.

M.E. cnawlece, from O.E. cnawan, cf. O.H.G. bi-chnaan, ir-chnaan "to know;" cognate with Pers. šenâxt, as below.

1) Šenâxt, past stem of šenâxtan, šenâsidan "to know, discern, distinguish, be acquainted with;" Mid.Pers. šnâxtan, šnâs- "to know, recognize," dânestan "to know;" O.Pers./Av. xšnā- "to know, learn, come to know, recognize;" cf. Skt. jñā- "to recognize, know," jānāti "he knows;" Gk. gignoskein "to know, think, judge;" L. gnoscere, noscere "to come to know" (Fr. connaître; Sp. conocer); O.E. cnawan; E. know; Rus. znat "to know;" PIE base *gno- "to know."
2) Dânestgân, literally "body of (what is) known," from dânest, short for dâneste "known," p.p. of dânestan variant of šenâxtan, as above, + -gân suffix forming plural entities.

  جغد، بوف   
joqd (#), buf (#)

Fr.: hibou, chouette   

Any of an order (Strigiformes) of chiefly nocturnal birds of prey with a large head and eyes, short hooked bill, strong talons, and soft fluffy often brown-mottled plumage (

Owl, from O.E. ule, from P.Gmc. *uwwalon (cf. Du. uil, O.H.G. uwila, Ger. Eule), a diminutive of root *uwwa, which is imitative of an owl's hoot (cf. L. ulula "owl;" Gk. ololyzein "to cry aloud," Skt. uluka- "owl."

Buf "owl;" Mid.Pers. bûf "owl," related to Av. bucahin- "he who is prone to howling," buxti- "howling, hissing" (Pokorny); cf. Skt. bukk- "to bark, yelp;" Gk. buas "owl;" L. bubo "owl" (Fr. hibou); Arm. bou "owl."
Joqd "owl," probably related to jiq "shreak, clamour, cry."

Owl Nebula
  میغِ بوف، ~ِ جغد   
miq-e buf, ~ joqd

Fr.: Nébuleuse de la Chouette   

A → planetary nebula in the constellation → Ursa Major, one of the four planetary nebulae in → Messier catalog. It is one of the more complex planetary nebulae known. Its appearance has been interpreted as that of a cylindrical torus shell viewed obliquely, so that the projected matter-poor ends of the cylinder correspond with the Owl's eyes. Also known as M97 or NGC 3587.

Discovered by Pierre Méchain in 1781, the name goes back to Lord Rosse, who first used it in 1848. → owl; → nebula.

Slowly Pulsating B star (SPB)
  ستاره‌ی ِ آهسته تپنده‌ی ِ گونه‌ی ِ B   
setâre-ye âhesté tapande-ye gune-ye B

Fr.: étoile B pulsante à longue période   

A member of a class of → B stars that are situated along the → main sequence with → spectral types ranging from B2 to B9 and masses from 3 to 7 → solar masses. In the → H-R diagram the SPB group lies below → beta Cephei variables, which are more massive. SPBs show light and line-profile variations that are multi-periodic with periods of the order of days. This variability is understood in terms of non-radial → stellar pulsations, and their → oscillation modes are high-order → g modes. Theoretical models attribute the pulsational nature of SPBs to the → kappa mechanism, acting in the metal → opacity bump at 2 x 105 K. Their g-mode pulsations penetrate deep into the stellar interior, making these objects very promising for → asteroseismology. Several oscillation modes are excited simultaneously, resulting in periodicities on time scales of the order of months or even years. The prototype of this group is 53 Per. First introduced as a distinct class by Waelkens (1991, A&A 246, 453).

slow; → pulsating; → B star.