Fr.: en rotation
Capable of or having rotation.
rotating black hole
Fr.: trou noir en rotation
A black hole that possesses angular momentum, as first postulated by Roy C. Kerr in 1963. Opposite of a stationary black hole. → ergosphere.
setâre-ye carxân, ~ carxandé
Fr.: étoile en rotation
A star that has a non-zero → angular velocity. In a rotating star, the → centrifugal forces reduce the → effective gravity according to the latitude and also introduce deviations from sphericity. In a rotating star, the equations of stellar structure need to be modified. The usual spherical coordinates must be replaced by new coordinates characterizing the → equipotentials. See also → von Zeipel theorem.
The motion of a body about its axis.
Verbal noun of → rotate.
Fr.: axe de rotation
Fr.: courbe de rotation
A plot of the variation in → orbital velocity of stars and → interstellar matter with distance from the center of a → galaxy. A "flat" rotation curve indicates that the mass of the galaxy increases linearly with distance from its center. See also: farsi→ Keplerian rotation curve
Rotation; → curve.
Fr.: énergie de rotation
Fr.: fréquence de rotation
The number of rotations per unit time of a rotating object.
dowre-ye carxeš (#)
Fr.: période de rotation
The interval of time during which an object turns once about its axis.
âšubnâki-ye zâyide-ye carxeš, darhâzidé az ~
Fr.: turbulence induite par turbulence
rotation-powered pulsar (RPP)
tapâr-e carxeš-tavân, pulsâr-e ~ ~
A → neutron star that is spinning down as a result of → torques from → magnetic dipole radiation and particle emission. RPPs derive their energy primarily from the → rotation of the neutron star. The energy from their → spin-down appears as broad-band pulsations from → radio to → gamma-ray wavelengths and as a → wind of energetic particles flowing into their surrounding → pulsar wind nebulae. Since the discovery of RPPs through their radio → pulsations in 1967, more than 2000 → radio pulsars are now known with periods ranging from a few milliseconds to several seconds (A. K. Harding, 2013, Front. Phys. 8, 679).
Fr.: spectre rotation-vibration
The spectrum of a molecule resulting from the simultaneous rotation and vibration of its constituent atoms.
Of or pertaining to → rotation.
rotational angular momentum
jonbâk-e zâviyeyi-ye carxeši
Fr.: moment angulaire rotationnel, moment cinétique ~
The → angular momentum of a body rotating about an axis. The rotational angular momentum of a solid homogeneous sphere of mass M and radius R rotating about an axis passing through its center with a period of T is given by: L = 4πMR2/5T.
Fr.: axe de rotation
Fr.: élargissement rotationnel
The spectral line broadening caused by stellar rotation. Light from two rims of the star will be Doppler shifted in opposite directions, resulting in a line broadening effect. The line broadening depends on the inclination of the star's pole to the line of sight. The derived value is a function of ve. sini, where ve is the rotational velocity at the equator and i is the inclination, which is not always known. The fractional width (Δλ/λ) is of the order of 10-3 for B stars.
rotational Eddington limit
hadd-e Eddington-e carxeši
Fr.: limite d'Eddington avec rotation
The → Eddington limit of luminosity for a → rotating star in which both the effects of → radiative acceleration and rotation are important. Such objects mainly include → OB stars, → LBV, → supergiants, and → Wolf-Rayet stars. It turns out that the maximum permitted luminosity of a star is reduced by rotation, with respect to the usual Eddington limit (Maeder & Meynet, 2000, A&A, 361, 159).
Fr.: énergie rotationnelle
The → kinetic energy due to the → rotation of and object. Rotational energy is part of the total kinetic energy of the body. It is given by: (1/2)Iω2, where I is the → moment of inertia and ω is the → angular velocity. Same as → angular kinetic energy.
Fr.: mélange rotationnel
A consequence of → stellar rotation that deforms the star, triggers instabilities (→ shear turbulence and → meridional currents) leading to → transport of chemical species in the star. The efficiency of rotational mixing (measured for instance by the degree of surface → enrichments at a given → evolutionary stage) increases when the initial mass and rotation increase. This efficiency increases also when the initial → metallicity decreases. This is due to the fact that when the metallicity is lower, the stars are more compact. This makes the → gradients of the → angular velocity steeper in the stellar interiors. Steeper gradients produce stronger shear turbulence and thus more mixing. Rotational mixing can bring to the surface heavy elements newly synthesized in the stellar core. Rotation thus produces an increase of the → opacity of the outer layers and activates strong → mass loss through → radiatively driven winds. This effect may be responsible for the loss of large fractions of the initial mass of the star (Meynet et al. 2007, arXiv:0709.2275).
Fr.: mouvement de rotation
Of a → rigid body, a motion in which there are always two points of the body which remain motionless.