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

Of a gas, the ratio of its → specific heat at constant pressure to its specific heat at constant volume: γ = C_P/ C_V.

→ adiabatic; → index.

A parameter indicating the rate at which a → pulsar slows down. Neutron stars are powered by → rotational energy and lose energy by accelerating particle → winds and by emitting → electromagnetic radiation. The → rotation frequency, Ω, thus decreases with time and this slowdown is usually described by the relation Ω^. = - kΩn, where k is a positive constant which depends on the → moment of inertia and the → magnetic dipole moment of the → neutron star and n is the braking index. Conventionally, the braking index is derived by differentiation of the above equation, yielding n = ΩΩ^.. / Ω^.2. In a highly simplified model in which the spin-down torque arises from dipole radiation at the rotation frequency, one expects n = 3 (Johnston, S., Galloway, D., 1999, arXiv:astro-ph/9905058).

→ braking; → index.

The strength of the → calcium break, as measured from the fluxes in the intervals 3750-3950 Å and 4050-4250 Å. It is given by the expression Ca-break[%] = 100 · (f_upper - f_lower)/f_upper, where f_upper and f_lower are the mean fluxes measured in the 3750-3950 Å and 4050-4250 Å bands, respectively, in the rest frame (Dressler & Shectman 1987, AJ 94, 899).

→ calcium; → break; → index.

A manuscript text in book form which was common before the invention of printing. The codex is the earliest known form of a bound book which replaced the scroll. It was a Roman invention. → Dresden codex.

From L. codex "book," → code.

Nebigân, from nebi / nepi / nevi "book, scripture," from Mid.Pers. nibêg "writing, scripture, book," related to neveštan, → write, + -gân suffix denoting collective nature.

The difference between the → apparent magnitude of a star measured at one standard wavelength and the apparent magnitude at another longer, standard wavelength, allowing the quantitative measure of a star's color.

→ color; → index.

A conventional notation for decimal exponent, which converts the number after it into its common antilogarithm; for example, dex (2.35) = 10^2.35.

From decimal + exponent.

A combining form meaning "right" and "turning clockwise," used in the formation of compound words, e.g. → dextrorotatory, dextrocardia, dextrocular, etc. The variant dextr- occurs before vowels. Compare → levo-.

From L. dextr-, from dexter "right, right-hand;" cf. Gk. dexios "right," dexiteros "located on the right side;" Av. dašina- "right; south" ( Mid.Pers. dašn "right hand; " Ossetic dæsni "skillful, dexterous"); Skt. dáksina- "right; southern;" Goth. taihswo "right hand;" O.Ir. dess "on the right hand, southern;" PIE base *deks- "right;" + epenthetic vowel -o-; see also → south.

Râst- from râst, → right.

The clockwise rotation of the → plane of polarization of light (as viewed by an observer looking straight in the incoming light) by certain substances. See also → levorotation.

→ dextro-; → rotation.

Relating to an → optically active substance that causes → dextrorotation.

Adj. related to → dextrorotation.

The reciprocal of the → dispersive power.

→ dispersive; → index.

A pre-Colombian Maya manuscript consisting of numerous calendar and astronomical data, probably dating from the 12th century. It seems that it is an updated copy of a document from the period of the old Maya Empire (4th-9th centuries). It contains a table which covers over 32 years, grouping 45 successive → lunations, divided into 69 groups of 5 or 6 lunations. The data are calculated in days and correspond remarkably to the intervals in an eclipse table: each group ends at the probable date of a solar eclipse (M.S.: SDE).

Dresden refers to the Dresden Library where the original document is preserved. It was bought in 1739 by the library director, Johann Christian Götze, who found it in a private library in Vienna. Its earlier history is unknown; codex, from L. codex earlier caudex "book, book of laws," literally "tree-trunk, book (formed originally from wooden tablets);" → codex.

1) Math.: A number or symbol, often written as a → subscript or → superscript to a mathematical expression, that indicates an operation to be performed, an ordering relation, or a use of the associated expression.
2) Physics: A measure of a particular property; e.g. → adiabatic index; → color index; → index of refraction.
3) In some → astrolabes, the → rule.
4) A sequential arrangement of items, especially in alphabetical or numerical order. → Index Catalogue.

Index, from L. index "forefinger, pointer, sign," literally "anything which points out," from indicare "point out, show," from in- "in" + dicare "to proclaim," from stem of dicere "to speak, to say;" PIE base *deik- "to point out" (cf. Av. daēs- " to show;" Skt. dic- "to point out, show;" Gk. deiknynai "to prove;" O.H.G. zeigon; Ger. zeigen "to show;" O.E. teon "to accuse," tæcan "to teach").

1) Dišan, from diš-, simple aorist of Av. daēs- "to show," as above, + suffix -an.
2) Fehrest, from Mid.Pers. payrâstag "arranged," from payrâstan "to arrange; to adorn" (Mod.Pers. pirâstan); Proto-Ir. *pati-rāsta-, from *pati "to, at, for, in" (cf. Mid.Pers. pad "to, at, for, in;" Mod.Pers. be, beh; Old.Pers. paity; Av. paiti "to, toward, in, at;" Skt. práti; Gk. poti) + *rād- "to direct, arrange" (cf. Mod.Pers. raj "line, row," variants raž, rak, râk, rezg (Lori), ris, risé, radé, rasté, râsté, related to râst "right, true; just, upright, straight;" Mid.Pers. râst "true, straight, direct;" Sogdian rəšt "right;" O.Pers. rāsta- "straight, true," rās- "to be right, straight, true;" Av. rāz- "to direct, put in line, set," razan- "order;" cf. Skt. raj- "to direct, stretch," rjuyant- "walking straight;" Gk. orektos "stretched out;" L. regere "to lead straight, guide, rule," p.p. rectus "right, straight;" PIE base *reg- "move in a straight line," hence, "to direct, rule").

Either of two catalogues of non-stellar objects, which serve as supplements to the → New General Catalogue.

→ index; → catalog

Same as → refractive index.

→ index; → refraction.

A variable used in → spherical harmonic expansions. Each spherical harmonic is characterized by its multipole index l: l = 0 for a → monopole, l = 1 for a → dipole, and so on. It is used in particular to describe the → cosmic microwave background anisotropy: ΔT/T₀ (θ,φ) = Σ a_lmY_lm(θ,φ), where θ and φ are the → spherical polar coordinates, Y_lm is the → spherical harmonic functions, and the sum runs over l = 1, 2, ..., ∞ and m = -l, ..., l, where the multipole index l corresponds to angular scales ≅ 180°/l.

→ multipole; → index.

A number appearing in the equation describing a → polytropic process.

→ polytropic; → index.

In the Johnson → UBV system, a reddening-free parameter which is related to the → effective temperature of stars and thus provides a useful, but rough, discriminant for → spectral types. It is expressed as: Q = (U - B) - 0.72 (B - V).

→ index.

Of any optical medium, the ratio of the → speed of light in vacuum (c) to that in the medium (v): n = c/v. The refractive index for vacuum, by definition, is 1. The refractive index of air is 1.00029 at standard temperature (25 °C) and pressure (1 atm). The refractive index of a medium depends on the wavelength of refracted wave. With light waves, n increases as the wavelength decreases. → Snell's law can be used to derive n. Same as → index of refraction.

Refractive, pertaining to → refraction; → index.

The ratio of the sine of the angle of incidence to the sine of the angle of refraction for a ray passing out of one of the media into the other.

→ relative; → refractive; → index.

1) The → exponent of the → frequency on which depends the intensity of the → continuum emission, that is: F_ν∝ ν^α. The exponent (α) typically takes positive values from 0 to 2 for → thermal emission, while → non-thermal emission, such as → synchrotron radiation, leads to negative values of the spectral index ranging from about -0.5 to -1.5.
2) The ratio α_IR = dlog(λF_λ)/dlogλ, where F represents the flux and λ the wavelength, in the range 2.2 μm ≤ λ ≤ 25 μm, particularly used in the classification of → protostars (→ Class I, → Class II, and → Class III).

→ spectral; → index.