Fr.: profil moyen
The shape of a pulsar's pulse as determined by averaging several pulses.
mean sidereal day
ruz-e axtari-ye miyângin
Fr.: jour sidéral moyen
mean sidereal time
zamân-e axtari-ye miyângin (#)
Fr.: temps sidéral moyen
The hour angle of the mean equinox for a given observer.
mean solar day
ruz-e xoršidi-ye miyângin (#)
Fr.: jour solaire moyen
The average length of the apparent solar day. In other words, the interval between successive transits of the mean Sun for a given observer.
mean solar time
zamân-e xoršidi-ye miyângin (#)
Fr.: temps solaire moyen
The time since the mean Sun crossed the meridian with 12 hours added to make the day begin at midnight.
Fr.: spectre moyen
A plot of the mass-to-charge ratio of elementary particles, sorted by their isotopic mass.
xoršid-e miyângin (#)
Fr.: Soleil moyen
A hypothetical Sun that moves along the ecliptic at a uniform rate equal to the average motion of the real Sun.
Fr.: terme moyen
mean value theorem
farbin-e arzeš-e miyângin
Fr.: théorème des accroissements finis
1) If f(x) is a continuous function on the interval from a to b, then:
Fr.: sens, signification
M.E., from mean; O.E. mænan "to mean, intend, signify" (cf. O.Fris. mena "to signify," O.S. menian "to intend, signify," M.Du. menen, Du. meenen, Ger. meinen "think, suppose"), related to Pers. maneš "disposition, temperament," mênidan "to think, consider," → idea; + → -ing.
Cemâr, from cem or cim "meaning, signification;" Mid.Pers. cim "meaning, reason, cause;" ultimately from Proto-Ir. *cahmāt "wherefore?" cf. Skt. kasmāt "why, where from? whence?," kim "what? how? why?" + âr short form of âvar present stem of âvardan "to cause or produce; to bring," → production, as in bonâr, → cause, used also as a nuance suffix; see also the verb → mean.
period-mean density relation
bâzâneš-e dowré-cagâli-ye miyângin
Fr.: relation période-densité moyenne
A relation that gives a rough estimate of the oscillation period of a → pulsating star as a function of its mean density. This relation is obtained by considering how long it would take a sound wave to travel across the diameter of a model star: Π ≅ (3π/2γGρ)1/2, where ρ is the mean density, γ the ratio of → specific heats (Cp/Cv), and G the → gravitational constant. This relation shows that the pulsation period of a star is inversely proportional to the square root of its mean density. And this is the reason why the pulsation periods decrease along the → instability strip from the luminous, very tenuous → supergiants to the faint, very dense → white dwarfs.
root mean square (rms)
riše-ye câruši-ye miyângin, ~ dovom-e ~
Fr.: valeur quadratique moyenne
The square root of the arithmetic mean of the squares of the numbers in a given set.
irang-e riše-ye câruši-ye miyângin, ~ ~ dovom-e ~
The square root of the second moment corresponding to the frequency function of a random variable.
arzeš-e riše-ye câruši-ye miyângin
Fr.: écart quadratique moyen, écart type
Statistics: The square root of the arithmetic mean of the squares of the deviation of observed values from their arithmetic mean.
Rosseland mean opacity
kederi-ye miyângin-e Rosseland
Fr.: opacité moyenne de Rosseland
The → opacity of a gas of given composition, temperature, and density averaged over the various wavelengths of the radiation being absorbed and scattered. The radiation is assumed to be in → thermal equilibrium with the gas, and hence have a → blackbody spectrum. Since → monochromatic opacity in stellar plasma has a complex frequency dependence, the Rosseland mean opacity facilitates the analysis. Denoted κR, it is defined by: 1/κR = (π/4σT3) ∫(1/kν) (∂B/∂T)νdν, summed from 0 to ∞, where σ is the → Stefan-Boltzmann constant, T temperature, B(T,ν) the → Planck function, and kν monochromatic opacity (See Rogers, F.J., Iglesias, C. A. Radiative atomic Rosseland mean opacity tables, 1992, ApJS 79, 507).
miyângin-e vazni (#)
Fr.: moyenne pondérée
An mean which is obtained by combining different numbers according to the relative importance of each.