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
magic square
  چاروش ِ جادو   
câruš-e jâdu

Fr.: carré magique   

An n × n matrix in which every row, column, and diagonal add up to the same number.

magic; → square.

magistrate
  دادیار   
dâdyâr (#)

Fr.: magistrat   

1) A civil officer charged with the administration of the law.
2) A minor judicial officer, as a justice of the peace or the judge of a police court, having jurisdiction to try minor criminal cases and to conduct preliminary examinations of persons charged with serious crimes (Dictionary.com).

M.E., from O.Fr. magistrat, from L. magistratus "a magistrate, public functionary," from magistrare "to serve as a magistrate," from magister, "chief, director," → master.

Dâdyâr, from dâd, → justice, + yâr, "assistant, helper," → gravity assist.

magma
  ماگما   
mâgmâ (#)

Fr.: magma   

1) Molten → rock material that occurs below Earth's surface.
2) Molten material both below and on top of the surface of a → planet.

From L. magma "dregs of an ointment," from Gk. magma "an ointment," from root of massein "to knead, mold."

Mâgma, loanword from Fr.

magma chamber
  اتاقک ِ ماگما   
otâqak-e mâgmâ (#)

Fr.: chambre magmatique   

A large cavity within the Earth's → crust containing → magma. When a → vent is opened to the surface, magma is extruded onto the surface as → lava.

magma; → chamber.

magnesium
  منیزیوم   
manyeziom (#)

Fr.: magnésium   

A metallic chemical element; symbol Mg. Atomic number 12; atomic weight 24.305; melting point about 648.8°C; boiling point about 1,090°C. The Scottish chemist Joseph Black recognized it as a separate element in 1755. In 1808, the English chemist Humphrey Davy obtained the impure metal and in 1831 the French pharmacist and chemist Antoine-Alexandre Brutus Bussy isolated the metal in the pure state.

The name originally used was magnium and was later changed to magnesium, which is derived from Magnesia, a district in the northeastern region of Greece called Thessalia.

magnet
  آهنربا، مغناتیس   
âhanrobâ (#), meqnâtis (#)

Fr.: aimant   

An object that produces a magnetic field around itself.

From L. magnetum (nom. magnes) "lodestone," from Gk. ho Magnes lithos "the Magnesian stone," from Magnesia region in Thessaly where magnetized ore was obtained.

Âhanrobâ, literally "iron attracting, iron robbing," from âhaniron + robâ agent noun of robudan, robâyidan "to attract, to grab, rob;" Av. urūpaiieinti "to cause racking pain(?);" cf. Skt. rop- "to suffer from abdominal pain," rurupas "to cause violent pain," ropaná- "causing racking pain," rópi- "racking pain;" L. rumpere "to break;" O.E. reofan "to break, tear."
Meqnâtis, from Ar., from Gk., as above.

magnetar
  مگنتار   
magnetâr (#)

Fr.: magnétar   

A highly magnetized → neutron star with fields a thousand times stronger than those of → radio pulsars. There are two sub-classes of magnetars, → anomalous X-Ray pulsar (AXP)s and → soft gamma repeater (SGR)s, that were thought for many years to be separate and unrelated objects. In fact SGRs and AXPs are both neutron stars possessing → magnetic fields of unprecedented strength of 1014 - 1016 G, and that show both steady X-ray pulsations as well as soft gamma-ray bursts. Their inferred steady X-ray luminosities are about one hundred times higher than their → spin-down luminosities, requiring a source of power well beyond the magnetic dipole spin-down that powers → rotation-powered pulsar (RPP)s. New high-energy components discovered in the spectra of a number of AXPs and SGRs require non-thermal particle acceleration and look very similar to high-energy spectral components of young rotation-powered pulsars (A. K. Harding, 2013, Front. Phys. 8, 679).

From magnet, contraction of → magnetic + -(s)tar, from → star.

magnetic
  مغناتیسی، مغناتی، آهنرباییک   
meqnâtisi (#), meqnâti, âhanrobâyik

Fr.: magnétique   

Of or pertaining to a magnet or magnetism.

From → magnet + → -ic.

Meqnâtisi, meqnâti, from meqnâtis, → magnet; âhanrobâyik, from âhanrobâ, → magnet, + → -ik, → -ic.

magnetic advection
  پهنبز ِ مغناتیسی   
pahnbaz-e meqnâtisi

Fr.: advection magnétique   

The transport of the magnetic field by a fluid. It is given by the term ∇ x (v x B) in the → induction equation.

magnetic; → advection.

magnetic axis
  آسه‌ی ِ مغناتیسی   
âse-ye meqnâtisi

Fr.: axe magnétique   

The imaginary straight line joining the two → poles of a → magnet.

magnetic; → meridian.

magnetic bottle
  بطری ِ مغناتیسی   
botri-ye meqnâtisi (#)

Fr.: bouteille magnétique   

Any configuration of → magnetic fields used in the containment of a → plasma during controlled → thermonuclear reaction experiments.

magnetic; → bottle.

magnetic braking
  لگامش ِ مغناتیسی   
legâmeš-e meqnâtisi

Fr.: freinage magnétique   

The process whereby a star which loses mass slows down under the action of its → magnetic field. The stellar material follows the → magnetic field lines extending well beyond the stellar surface. The material gain → angular momentum and the underlying object is slowed down. Magnetic braking is an efficient mechanism for removing angular momentum from the the rotating object. See also → disk locking.

magnetic; → braking.

magnetic braking catastrophe
  نگونزار ِ لگامش ِ مغناتیسی   
negunzâr-e legâmeš-e meqnâtisi

Fr.: catastrophe du freinage magnétique   

The failure of numerical star formation calculations to produce rotationally supported → Keplerian disks because of the → magnetic braking effect, when → magnetic fields of strengths comparable to those observed in → molecular clouds are accounted for. The formation and early evolution of disks is a long-standing fundamental problem in → star formation models. Early work in the field had concentrated on the simpler problem of disk formation from the → collapse of a rotating dense core in the absence of a magnetic field. However, dense star-forming cores are observed to be significantly magnetized. There is increasing theoretical evidence that disk formation is greatly modified, perhaps even suppressed, by a dynamically important magnetic field. This has been found in analytic studies, axisymmetric numerical models and in 3D calculations using → ideal magnetohydrodynamics. By contrast, recent observations suggest the presence of massive, 50-100 AU disks and evidence for associated → outflows in the earliest (→ class 0) stages of star formation around both low and high mass stars. Two primary solutions have been proposed: → turbulence and → non-ideal magnetohydrodynamics. Calculations of the collapse of a massive 100 Msun core have shown that 100 AU scale disk formation in the presence of strong magnetic fields was indeed possible, with some argument over whether this is caused by turbulent reconnection or another mechanism. Studies, using simulations of collapsing 5 Msun cores, have found that turbulence diffuses the strong magnetic field out of the inner regions of the core, and that the non-zero → angular momentum of the turbulence causes a misalignment between the rotation axis and the magnetic field. Both of these effects reduce the magnetic braking, and allow a massive disk to form (Wurster et al. 2016, arxiv/1512.01597 and references therein).

magnetic; → braking; → catastrophe.

magnetic bremsstrahlung
  لگام-تابش ِ مغناتیسی   
legâm-tâbeš-e meqâtisi

Fr.: rayonnement de freinage magnétique   

Same as → synchrotron radiation.

magnetic; → bremsstrahlung.

magnetic buoyancy
  بالارانی ِ مغناتیسی   
bâlârâni-ye meqnâtisi

Fr.: flottabilité magnétique   

The phenomenon whereby the presence of a → magnetic field can make a portion of → compressible fluid less dense than its surroundings, so that it floats upward under the influence of gravity. This magnetic buoyancy is thought, in fact, to be the mechanism by which magnetic flux tubes rise through the Sun's → convection zone and break at the surface in the form of → sunspots. The Sun's rotation would have a major effect on the rate at which these magnetic flux tubes rise. The rotation substantially lengthen the time taken for the flux tubes to reach the surface (D. J. Acheson, 1979, Nature 277, 41).

magnetic; → buoyancy.

magnetic cataclysmic binary
  دورین ِ گتلوری ِ مغناتیسی   
dorin-e gatluri-ye meqnâtisi

Fr.: binaire cataclysmique magnétique   

A cataclysmic binary in which the white dwarf primary has a strong magnetic field that radically affects the accretion flow in the system. → polar

magnetic; → cataclysmic; → binary.

magnetic cloud
  ابر ِ مغناتیسی   
abr-e meqnâtisi

Fr.: nuage magnétique   

A transient ejection in the → solar wind having an enhanced field, a large and smooth change in field direction, and a low → proton temperature compared to the ambient proton temperature (L. F. Burlaga, 1995, Interplanetary Magnetohydrodynamics, Oxford Univ. Press, 89-114).

magnetic; → cloud.

magnetic compass
  قطبنما   
qotbnemâ (#)

Fr.: compas magnétique   

compass.

magnetic; → compass.

magnetic connectivity
  هابندندگی ِ مغناتیسی   
hâbandandegi-ye meqnâtisi

Fr.: connectivité magnétique   

Of magnetic field lines, the condition for them to be connected or the process whereby they become connected or connective.

magnetic;→ connectivity.

magnetic constant
  پایای ِ مغناتیسی   
pâyâ-ye meqnâtisi (#)

Fr.: constante magnétique   

A physical constant relating mechanical and electromagnetic units of measurement. It has the value of 4π × 10-7 henry per meter. Also called the permeability of free space, or → absolute permeability.

magnetic; → constant.

<< < -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 > >>