An Etymological Dictionary of Astronomy and Astrophysics
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فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 13176 Search : in
kilo-
  کیلو-   
kilo- (#)

Fr.: kilo-   

A prefix meaning 103.

Introduced in France in 1795, when the → metric system was officially adopted, from Gk. khilioi "thousand," of unknown origin.

kilogram (kg)
  کیلوگرم   
kilogram (#)

Fr.: kilogramme   

The basic unit of mass in the → International System of Units (SI) and → MKS versions of the → metric system, equal to 1,000 → grams. The kilogram was until 2019 defined as the mass of the standard (international prototype) kilogram, a platinum-iridium cylinder kept at the International Bureau of Weights and Measures (BIPM), at Sèvre, near Paris, France. Copies of this prototype are kept by the standards agencies of all the major industrial nations. A kilogram is equal to the mass of 1,000 cubic cm of water at 4°C (→ maximum density). According to the new (2019) definition, the kilogram is defined by taking the fixed numerical value of the → Planck constant (h) to be 6.62607015 × 10-34 when expressed in the unit J.s, which is equal to kg m2 s-1, where the meter and the second are defined in terms of c and Δν Cs.

kilo-; → gram.

kilogram-force (kgf)
  کیلوگرم-نیرو   
kilogram-niru (#)

Fr.: kilogramme-force   

A metric unit of force which is equal to a mass of one kilogram multiplied by the standard acceleration due to gravity on Earth (9.80665 m sec-2). Therefore one (1) kilogram-force is equal to 1 kg × 9.80665 m sec-2 = 9.80665 → newtons.

kilogram; → force.

kilohertz (kHz)
  کیلوهرتز   
kilohertz (#)

Fr.: kilohertz   

A unit of → frequency, equal to 103 Hz.

kilo-; → hertz.

kilometer (km)
  کیلومتر   
kilometr (#)

Fr.: kilomètre   

A unit of length, equal to 1000 meters.,

kilo-; → meter.

kilonova
  کیلو-نووا   
kilonovâ

Fr.: kilonova   

A fast-evolving → supernova-like phenomenon resulting from the → merger of compact, binary objects such as two → neutron stars or a neutron star and a → black hole. A kilonova represents an → electromagnetic counterpart to → gravitational waves. Also called → macronova. A simple model of the phenomenon was put forward by Li and Paczynski (1998, ApJL 507, L59). The kilonova phenomenon can last between days and weeks following the merger. Within the small volume of space where a merger occurs, the combination of a huge amount of energy, and a large number of neutrons, is the instigator for the → r-process. The high density favors this rapid → neutron capture by nuclei, leading to the formation of new → chemical elements with high → atomic numbers and high → atomic weights. Many elements heavier than → iron form in these environments, including many rare elements, most notably → platinum (atomic number 78) and → gold (atomic number 79). The decay of heavy atomic nuclei leads to the radioactive heating and a release of electromagnetic radiation. The heat cannot easily escape as radiation, because of the high opacity of the ejected material. The heat is radiated thermally, heating up the nearby matter, which can be then seen in the → near-infrared. It was long thought that the r-process could also occur during core-collapse supernovae, but the density of neutrons within supernovae appears to be too low. The first indication of a kilonova following a short GRB came from the extensive follow-up of GRB 130603B, which was one of the nearest and brightest short GRBs ever detected, and also the first short GRB with an optical afterglow spectrum. The first kilonova found to be associated with a gravitational waves was detected in the study of → GW170817.

The term kilonova was introduced by Metzger et al. (2010, MNRAS 406, 2650), who argued that the peak luminosities of neutron star merger transients are typically ~ few × 1041 erg s-1, or a factor of ~ 103 larger than the → Eddington luminosity for a solar mass object. They therefore dubbed these events kilonovae; from → kilo-; → nova.

kiloparsec (kpc)
  کیلوپارسک   
kilopârsek (#)

Fr.: kiloparsec   

A unit of distance equal to 1,000 → parsec (pc)s, or 3,260 → light-years.

kilo-; → parsec.

kilowatt-hour (kWh)
  کیلووات-ساعت   
kilowatt-sâ'at (#)

Fr.: kilowatt-heure   

A unit of energy equivalent to one kilowatt (1 kW) of power expended for one hour (1 h) of time. The kilowatt-hour is not a standard unit in any formal system, but it is commonly used to measure the consumption of electrical energy. To convert to → joules, use: 1 kWh = 3.6 × 106 J = 3.6 × 1013ergs.

kilo-; → watt-hour.

kinematic
  جنبشی، جنبشیک   
jonbeši, jonbešk

Fr.: cinématique   

Of or relating to → kinematics. Same as kinematical.

kinematics.

kinematic bias
  ورک ِ جنبشی   
varak-e jonbeši

Fr.: biais cinématique   

A systematic error introduced in a sample of stellar → proper motion data by higher velocity stars that are easier to measure.

kinematic; → bias.

kinematic viscosity
  وشکسانی ِ جنبشیک   
vošksâni-ye jonbešik

Fr.: viscosité cinématique   

The ratio of the → dynamic viscosity (η) to the density (ρ) of a fluid: ν = η/ρ. The unit of kinematic viscosity in the → SI system is m2s-1. In the → cgs system, cm2s-1, equal to 10-4 m2s-1, is called the → stokes (st).

kinematic; → viscosity.

kinematical
  جنبشی، جنبشیک   
jonbeši, jonbešik

Fr.: cinématique   

Of or relating to → kinematics. → kinematic.

kinematic; → -al.

kinematically decoupled core (KDC)
  مغزه‌ی ِ جنبشیکانه واجفسریده   
maqze-ye jonbešikâné vâjafsaridé

Fr.: cœur cinématiquement découplé   

A central, tightly bound stellar subsystem observed in some elliptical galaxies which rotates in the opposite direction with respect to the main body of the → elliptical galaxy. Elliptical galaxies are thought to be the result of the → merger of two or more sizable galaxies. A plausible scenario for how counter-rotating cores could form in such a merger is as follows. If at least one of the galaxies has a core region that is fairly tightly bound by the galaxy's gravity, and the direction in which the two galaxies orbit each other before merging is opposite to the direction of rotation of stars in that tightly bound core, it is likely that, after the merger, the tightly bound core will end up as the core of the new, larger galaxy, while retaining its original sense of rotation. The surrounding stars, on the other hand, will rotate in a different way dictated by the orbital motion of the galaxies around each other, before the merger. While this is a plausible scenario, it can only explain some of the counter-rotating cores. Recently A. Tsatsi et al. (2015, ApJ 802, L3) have shown that although the two → progenitor galaxies are initially following a → prograde orbit, strong reactive forces during the merger can cause a short-lived change of their orbital spin; the two progenitors follow a → retrograde orbit right before their final coalescence. This results in a central kinematic decoupling and the formation of a large-scale (~2 kpc radius) counter-rotating core at the center of the final elliptical-like merger remnant, while its outer parts keep the rotation direction of the initial orbital spin.

kinematical; → decouple; → core.

kinematics
  جنبشیک   
jonbešik

Fr.: cinématique   

The branch of mechanics dealing with the description of the motion of bodies or fluids without reference to the forces producing the motion.

From Gk. kinetikos "moving, putting in motion," from kinetos "moved," verbal adj. of kinein "to move;" PIE base *kei- "to move to and fro" (cf. Mod.Pers. šodan, šow- "to go; to become;" Av. šiyav-, š(ii)auu- "to move, go," šiyavati "goes," šyaoθna- "activity; action; doing, working;" O.Pers. šiyav- "to go forth, set," ašiyavam "I set forth;" Skt. cyu- "to move to and fro, shake about; to stir," cyávate "stirs himself, goes;" Goth. haitan "call, be called;" O.E. hatan "command, call").

Jonbešik, from jonbeš "motion" + -ik-ics. The first element from Mid.Pers. jumbidan, jumb- "to move," Lori, Laki jem "motion," related to gâm "step, pace;" O.Pers. gam- "to come; to go," Av. gam- "to come; to go," jamaiti "goes," gāman- "step, pace" (Mod.Pers. âmadan "to come"); Skt. gamati "goes;" Gk. bainein "to go, walk, step," L. venire "to come;" Tocharian A käm- "to come;" O.H.G. queman "to come;" E. come; PIE root *gwem- "to go, come."

kinetic
  جنبشی   
jonbeši (#)

Fr.: cinétique   

Of or relating to motion; caused by motion; characterized by movement.

From Gk. kinetikos "moving, putting in motion," from kinein "to move," → kinematics.

Jonbeši, adj. of jonbeš, verbal noun of jonbidan, → move.

kinetic energy
  کاروژ ِ جنبشی   
kâruž-e jonbeši

Fr.: énergie cinétique   

The energy which a body possesses as a consequence of its motion, defined as one-half the product of its mass m and the square of its speed v, i.e. 1/2 mv2.

kinetic; → energy.

kinetic helicity
  پیچاری ِ جنبشی   
picari-ye jonbeši

Fr.: hélicité cinétique   

In fluid mechanics, a quantity that describes helical flow. It is defined by the integrated scalar product of the velocity field and the → vorticity: KK = ∫ dVu . ( x u). In the absence of magnetic field, this quantity is conserved by the → Euler equation. See also → magnetic helicity.

kinetic; → helicity.

kinetic potential
  توند ِ جنبشیک   
tavand-e jonbešik

Fr.: potentiel cinétique   

Same as → Lagrangian function.

kinetic; → potential.

kinetic temperature
  دمای ِ جنبشی   
damâ-ye jonbeši (#)

Fr.: température cinétique   

The temperature of a gas defined in terms of the average kinetic energy of its atoms or molecules.

kinetic; → temperature.

kinetic theory of gases
  نگره‌ی ِ جنبشی ِ گاز‌ها   
negare-ye jonbeši-ye gâzhâ (#)

Fr.: théorie cinétique des gaz   

A theory that explains macroscopic properties of gases, such as pressure, temperature, or volume, by considering their molecular composition and motion.

kinetic; → theory; → gas.

<< < -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 > >>