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IZOHLI LUG’AT

GALAKTIKA- GALAXY

A galaxy is a massive, gravitationally bound system that consists

of stars and stellar remnants, an interstellar medium of gas dust, and an

important but poorly understood component tentatively dubbed dark

matter.The name is from the Greek word galaxias, literally meaning

"milky", a reference to the Milky Way galaxy. Typical galaxies range

from dwarfs with as few as ten million (107) stars, up to giants with a

hundred trillion (1014) stars,[4] all orbiting the galaxy's center of mass.

Galaxies may contain many star systems, star clusters, and various

interstellar clouds. The Sun is one of the stars in the Milky Way galaxy;

the Solar System includes the Earth and all the other objects that orbit

the Sun.

SPIRAL GALAKTIKA- SPIRAL GALAXY

An example of a spiral galaxy, the Pinwheel Galaxy (also known

as Messier 101 or NGC 5457)

A spiral galaxy is a certain kind of galaxy originally described by

Edwin Hubble in his 1936 work The Realm of the Nebulae and, as such,

forms part of the Hubble sequence. Spiral galaxies consist of a flat,

rotating disk containing stars, gas and dust, and a central concentration

of stars known as the bulge. These are surrounded by a much fainter

halo of stars, many of which reside in globular clusters.

Spiral galaxies are named for the spiral structures that extend from

the center into the disk. The spiral arms are sites of ongoing star

formation and are brighter than the surrounding disk because of the

young, hot OB stars that inhabit them.

GALO- HALO

The galactic disk is surrounded by a spheroid halo of old stars and

globular clusters, of which 90% lie within 100,000 light-years (30

kpc),[50] suggesting a stellar halo diameter of 200,000 light-years.

However, a few globular clusters have been found farther, such as PAL

4 and AM1 at more than 200,000 light-years away from the galactic

center. About 40% of these clusters are on retrograde orbits, which

means they move in the opposite direction from the Milky Way rotation.

The globular clusters can follow rosette orbits about the galaxy, in

contrast to the elliptical orbit of a planet.

While the disk contains gas and dust which obscure the view in

some wavelengths, the spheroid component does not. Active star

formation takes place in the disk (especially in the spiral arms, which

represent areas of high density), but not in the halo. Open clusters also

occur primarily in the disk.

Discoveries in the early 21st century have added dimension to the

knowledge of the Milky Way's structure. With the discovery that the

disk of the Andromeda Galaxy (M31) extends much further than

previously thought, the possibility of the disk of the Milky Way galaxy

extending further is apparent, and this is supported by evidence from the

discovery of the Outer Arm extension of the Cygnus Arm. With the

discovery of the Sagittarius Dwarf Elliptical Galaxy came the discovery

of a ribbon of galactic debris as the polar orbit of the dwarf and its

interaction with the Milky Way tears it apart. Similarly, with the

discovery of the Canis Major Dwarf Galaxy, it was found that a ring of

galactic debris from its interaction with the Milky Way encircles the

galactic disk.

GALAKTIKA MARKAZI- GALACTIC CENTER

Main article: Galactic Center

Observed structure of the Milky Way's spiral arms. The Sun is in

the Local Spur.

The galactic disc, which bulges outward at the galactic center, has

a diameter of 70,000–100,000 light-years (20–30 kpc). The exact

distance from the Sun to the galactic center is actively debated. The

latest estimates from geometric-based methods and standard candles

yield distances to the Galactic center of 7.6–8.7 kpc (25,000–28,000 ly).

The fact that the estimates span over 1 kpc only underscores the true

uncertainty associated with the distance to the Galactic center.

The galactic center harbors a compact object of very large mass as

determined by the motion of material around the center. The intense

radio source named Sagittarius A*, thought to mark the center of the

Milky Way, is newly confirmed to be a supermassive black hole. Most

galaxies are believed to have supermassive black holes at their centers.

SPIRAL TARMOQLAR- SPIRAL ARMS

Observed and extrapolated structure of the spiral arms.

Artist's conception of the spiral structure of the Milky Way with

two major stellar arms and a bar.

Maps of the Milky Way's spiral structure are notoriously uncertain

and exhibit striking differences. Some 150 years after Alexander (1852)

first suggested that the Milky Way was a spiral, there is currently no

consensus on the number or nature of the Galaxy's spiral arms. Perfect

grand design logarithmic spiral patterns ineptly describe features near

the Sun, namely since galaxies commonly exhibit arms that branch,

merge, twist unexpectedly, and feature a degree of irregularity. The

possible scenario of the Sun within a spur / Local arm emphasizes that

point and indicates that such features are likely not unique, and exist

elsewhere in the galaxy.

GALAKTIKALARNI

SINFLASHTIRISH-

THE

HUBBLE

SEQUENCE IS A MORPHOLOGICAL CLASSIFICATION SCHEME FOR

The Hubble sequence is a morphological classification scheme for

galaxies invented by Edwin Hubble in 1926. It is often known

colloquially as the Hubble tuning-fork diagram because of the shape in

which it is traditionally represented.

Tuning-fork style diagram of the Hubble sequence

Hubble’s scheme divides regular galaxies into 3 broad classes -

ellipticals, lenticulars and spirals - based on their visual appearance

(originally on photographic plates). A fourth class contains galaxies

with an irregular appearance. To this day, the Hubble sequence is the

most commonly used system for classifying galaxies, both in

professional astronomical research and in amateur astronomy.

ELLIPTIK GALAKTIKA- ELLIPTICAL GALAXY

An elliptical galaxy is a galaxy having an approximately

ellipsoidal shape and a smooth, nearly featureless brightness profile.

They range in shape from nearly spherical to highly flat and in size from

hundreds of millions to over one trillion stars. They can be the result of

two galaxies colliding.

Elliptical galaxies are one of the three main classes of galaxy

originally described by American astronomer Edwin Hubble in his 1936

work The Realm of the Nebulae, along with spiral and lenticular

galaxies. Elliptical galaxies are (together with lenticular galaxies) also

called "early-type" galaxies (ETG), due to their location in the Hubble

sequence.

NOTO’G’RI GALAKTIKA- IRREGULARS

Galaxies that do not fit into the Hubble sequence, because they

have no regular structure (either disk-like or ellipsoidal), are termed

irregular galaxies. Hubble defined two classes of irregular galaxy:

Irr I galaxies have asymmetric profiles and lack a central bulge or

obvious spiral structure; instead they contain many individual clusters of

young stars

Irr II galaxies have smoother, asymmetric appearances and are not

clearly resolved into individual stars or stellar clusters

In his extension to the Hubble sequence, de Vaucouleurs called the

Irr I galaxies 'Magellanic irregulars', after the Magellanic Clouds - two

satellites of the Milky Way which Hubble classified as Irr I. The

discovery of a faint spiral structure[10] in the Large Magellanic Cloud

led de Vaucouleurs to further divide the irregular galaxies into those

that, like the LMC, show some evidence for spiral structure (these are

given the symbol Sm) and those that have no obvious structure, such as

the Small Magellanic Cloud (denoted Im). In the extended Hubble

sequence, the Magellanic irregulars are usually placed at the end of the

spiral branch of the Hubble tuning fork.

GALAKTIKA DISKI- DISC (GALAXY)

A disc is a component of disc galaxies, such as spiral galaxies, or

lenticular galaxies.

The galactic disc is the plane in which the spirals, bars and discs of

disc galaxies exist. Galaxy discs tend to have more gas and dust, and

younger stars than galactic bulges, or galactic haloes.

The galactic disc is mainly composed of gas, dust and stars. The

gas and dust component of the galactic disk is called the gaseous disk.

The star component of the galactic disk is called the stellar disk

10.

ASTRONOMIYA-ASTRONOMY

Astronomy is a natural science that deals with the study of celestial

objects (such as stars, planets, comets, nebulae, star clusters and

galaxies) and phenomena that originate outside the Earth's atmosphere

(such as the cosmic background radiation). It is concerned with the

evolution, physics, chemistry, meteorology, and motion of celestial

objects, as well as the formation and development of the universe.

11.

YULDUZ-STAR

A star is a massive, luminous ball of plasma held together by

gravity. At the end of its lifetime, a star can also contain a proportion of

degenerate matter. The nearest star to Earth is the Sun, which is the

source of most of the energy on Earth. Other stars are visible from Earth

during the night when they are not outshone by the Sun or blocked by

atmospheric phenomena. Historically, the most prominent stars on the

celestial sphere were grouped together into constellations and asterisms,

and the brightest stars gained proper names. Extensive catalogues of

stars have been assembled by astronomers, which provide standardized

star designations.

12.

QO‘SHALOQ YULDUZ - DOUBLE STAR

A binary star is a star system consisting of two stars orbiting

around their common center of mass. The brighter star is called the

primary and the other is its companion star, comes, or secondary.

Research between the early 19th century and today suggests that many

stars are part of either binary star systems or star systems with more

than two stars, called multiple star systems. The term double star may

be used synonymously with binary star, but more generally, a double

star may be either a binary star or an optical double star which consists

of two stars with no physical connection but which appear close

together in the sky as seen from the Earth. A double star may be

determined to be optical if its components have sufficiently different

proper motions or radial velocities, or if parallax measurements reveal

its two components to be at sufficiently different distances from the

Earth. Most known double stars have not yet been determined to be

either bound binary star systems or optical doubles.

13.

MASSIV YULDUZ - MASSIVE STARS

During their helium-burning phase, very high mass stars with more

than nine solar masses expand to form red supergiants. Once this fuel is

exhausted at the core, they can continue to fuse elements heavier than

helium.

The core contracts until the temperature and pressure are sufficient

to fuse carbon (see carbon burning process). This process continues,

with the successive stages being fueled by neon (see neon burning

process), oxygen (see oxygen burning process), and silicon (see silicon

burning process). Near the end of the star's life, fusion can occur along a

series of onion-layer shells within the star. Each shell fuses a different

element, with the outermost shell fusing hydrogen; the next shell fusing

helium, and so forth.

The final stage is reached when the star begins producing iron.

Since iron nuclei are more tightly bound than any heavier nuclei, if they

are fused they do not release energy—the process would, on the

contrary, consume energy. Likewise, since they are more tightly bound

than all lighter nuclei, energy cannot be released by fission. In relatively

old, very massive stars, a large core of inert iron will accumulate in the

center of the star. The heavier elements in these stars can work their

way up to the surface, forming evolved objects known as Wolf-Rayet

stars that have a dense stellar wind which sheds the outer atmosphere.

14.

CHANG – COLLAPSE

An evolved, average-size star will now shed its outer layers as a

planetary nebula. If what remains after the outer atmosphere has been

shed is less than 1.4 solar masses, it shrinks to a relatively tiny object

(about the size of Earth) that is not massive enough for further

compression to take place, known as a white dwarf. The electron-

degenerate matter inside a white dwarf is no longer a plasma, even

though stars are generally referred to as being spheres of plasma. White

dwarfs will eventually fade into black dwarfs over a very long stretch of

time.

The Crab Nebula, remnants of a supernova that was first observed

around 1050 AD

In larger stars, fusion continues until the iron core has grown so

large (more than 1.4 solar masses) that it can no longer support its own

mass. This core will suddenly collapse as its electrons are driven into its

protons, forming neutrons and neutrinos in a burst of inverse beta decay,

or electron capture. The shockwave formed by this sudden collapse

causes the rest of the star to explode in a supernova. Supernovae are so

bright that they may briefly outshine the star's entire home galaxy.

When they occur within the Milky Way, supernovae have historically

been observed by naked-eye observers as "new stars" where none

existed before.

15.

SPEKTR-SPECTR

Astronomical spectroscopy is the technique of spectroscopy used

in astronomy. The object of study is the spectrum of electromagnetic

radiation, including visible light, which radiates from stars and other

celestial objects. Spectroscopy can be used to derive many properties of

distant stars and galaxies, such as their chemical composition, but also

their motion by Doppler shift measurements.

16.

SPEKTRASKOP – SPECTROSCOPY

Spectroscopy is the study of the interaction between matter and

radiated energy. Historically, spectroscopy originated through the study

of visible light dispersed according to its wavelength, e.g., by a prism.

Later the concept was expanded greatly to comprise any interaction with

radiative energy as a function of its wavelength or frequency.

Spectroscopic data is often represented by a spectrum, a plot of the

response of interest as a function of wavelength or frequency.

Spectrometry and spectrography are terms used to refer to the

measurement of radiation intensity as a function of wavelength and are

often used to describe experimental spectroscopic methods. Spectral

measurement

devices

are

referred

spectrometers,

spectrophotometers, spectrographs or spectral analyzers.

17.

OSMON-THE SKY

he sky is the part of the atmosphere or outer space visible from the

surface of any astronomical object. It is difficult to define precisely for

several reasons. During daylight, the sky of Earth has the appearance of

a pale blue surface because the air scatters the sunlight. The sky is

sometimes defined as the denser gaseous zone of a planet's atmosphere.

At night the sky has the appearance of a black surface or region

scattered with stars.

18.

QUYOSH- SUN

The Sun is the star at the center of the Solar System. It is almost

perfectly spherical and consists of hot plasma interwoven with magnetic

fields. It has a diameter of about 1,392,000 km, about 109 times that of

Earth, and its mass (about 2×1030 kilograms, 330,000 times that of

Earth) accounts for about 99.86% of the total mass of the Solar System.

Chemically, about three quarters of the Sun's mass consists of hydrogen,

while the rest is mostly helium. Less than 2% consists of heavier

elements, including oxygen, carbon, neon, iron, and others.

19.

ATOM- ATOMS

Atomic spectroscopy was the first application of spectroscopy

developed. Atomic absorption spectroscopy (AAS) and atomic emission

spectroscopy (AES) involve visible and ultraviolet light. These

absorptions and emissions, often referred to as atomic spectral lines, are

due to electronic transitions of an outer shell electron to an excited state.

Atoms also have distinct x-ray spectra that are attributable to the

excitation of inner shell electrons to excited states.

Atoms of different elements have distinct spectra and therefore

atomic spectroscopy allows for the identification and quantitation of a

sample's elemental composition. Robert Bunsen, developer of the

Bunsen burner, and Gustav Kirchhoff discovered new elements by

observing their emission spectra. Atomic absorption lines are observed

in the solar spectrum and referred to as Fraunhofer lines after their

discoverer. A comprehensive explanation of the hydrogen spectrum was

an early success of quantum mechanics and explaining the Lamb shift

observed in the hydrogen spectrum led to the development of quantum

electrodynamics.

20.

YER- THE EARTH

Earth (or the Earth) is the third planet from the Sun and the densest

and fifth-largest of the eight planets in the Solar System. It is also the

largest of the Solar System's four terrestrial planets. It is sometimes

referred to as the World, the Blue Planet,[ or by its Latin name, Terra.

Home to millions of species including humans, Earth is currently

the only astronomical body where life is known to exist. The planet

formed 4.54 billion years ago, and life appeared on its surface within

one billion years.Earth's biosphere has significantly altered the

atmosphere and other abiotic conditions on the planet, enabling the

proliferation of aerobic organisms as well as the formation of the ozone

layer which, together with Earth's magnetic field, blocks harmful solar

radiation, permitting life on land. The physical properties of the Earth,

as well as its geological history and orbit, have allowed life to persist

during this period. The planet is expected to continue supporting life for

at least another 500 million years.

21.

KOINOT- THE UNIVERSE

everything that exists, including all physical matter and energy, the

planets, stars, galaxies, and the contents of intergalactic space, although

this usage may differ with the context (see definitions, below). The term

universe may be used in slightly different contextual senses, denoting

such concepts as the cosmos, the world, or nature. Observations of

earlier stages in the development of the universe, which can be seen at

great distances, suggest that the universe has been governed by the same

physical laws and constants throughout most of its extent and history.

22.

TEMPERATURA- TEMPERATURE

Temperature is a physical property of matter that quantitatively

expresses the common notions of hot and cold. Objects of low

temperature are cold, while various degrees of higher temperatures are

referred to as warm or hot. Quantitatively, temperature is measured with

thermometers, which may be calibrated to a variety of temperature

scales.

Much of the world uses the Celsius scale (°C) for most

temperature measurements. It has the same incremental scaling as the

Kelvin scale used by scientists, but fixes its null point, at 0°C =

273.15K, the freezing point of water.[note 1] A few countries, most

notably the United States, use the Fahrenheit scale for common

purposes, a historical scale on which water freezes at 32 °F and boils at

212 °F.

For practical purposes of scientific temperature measurement, the

International System of Units (SI) defines a scale and unit for the

thermodynamic temperature by using the easily reproducible

temperature of the triple point of water as a second reference point. For

historical reasons, the triple point is fixed at 273.16 units of the

measurement increment, which has been named the kelvin in honor of

the Scottish physicist who first defined the scale. The unit symbol of the

kelvin is K.

23.

QORA JISM- A BLACK BODY

A black body is an idealized physical body that absorbs all

incident electromagnetic radiation. Because of this perfect absorptivity

at all wavelengths, a black body is also the best possible emitter of

thermal radiation, which it radiates incandescently in a characteristic,

continuous spectrum that depends on the body's temperature. At Earth-

ambient temperatures this emission is in the infrared region of the

electromagnetic spectrum and is not visible. The object appears black,

since it does not reflect or emit any visible light.

24.

MASSA- WEIGHT

In most physics textbooks, weight is the name given to the force

on an object due to gravity. However, some books use an operational

definition, defining the weight of an object as the force measured by the

operation of weighing it (that is, the force required to support it). Both

definitions imply that weight is a force and that its value depends on the

local gravitational field. For example, an object with a mass of one

kilogram will have a weight of 9.8 newtons on the surface of the Earth,

about one-sixth as much on the Moon, and zero when floating freely far

out in space away from all gravitational influence. The differences

between the two definitions are discussed below. For example, they

differ over the weight of an object in free fall, such as a falling apple or

an astronaut in an orbiting spacecraft. In these cases, the operational

definition implies the weight is zero, whereas the gravitational

definition does not.

25.

MAGNIT MAYDON - MAGNETIC FIELD

Magnetic field of a star is generated within regions of the interior

where convective circulation occurs. This movement of conductive

plasma functions like a dynamo, generating magnetic fields that extend

throughout the star. The strength of the magnetic field varies with the

mass and composition of the star, and the amount of magnetic surface

activity depends upon the star's rate of rotation. This surface activity

produces starspots, which are regions of strong magnetic fields and

lower than normal surface temperatures. Coronal loops are arching

magnetic fields that reach out into the corona from active regions.

Stellar flares are bursts of high-energy particles that are emitted due to

the same magnetic activity.

26.

TELESKOP- TELESCOPE

A telescope is an instrument that aids in the observation of remote

objects by collecting electromagnetic radiation (such as visible light).

The first known practical telescopes were invented in the Netherlands at

the beginning of the 17th century. The word telescope can refer to a

wide range of instruments detecting different regions of the

electromagnetic spectrum.

The word "telescope" (from the Greek τῆλε, tele "far" and

σκοπεῖν, skopein "to look or see"; τηλεσκόπος, teleskopos "far-seeing")

was coined in 1611 by the Greek mathematician Giovanni Demisiani for

one of Galileo Galilei's instruments presented at a banquet at the

Accademia dei Lincei. In the Starry Messenger Galileo had used the

term "perspicillum".

27.

ORBITA- ORBIT

In physics, an orbit is the gravitationally curved path of an object

around a point in space, for example the orbit of a planet around the

center of a star system, such as the solar system. Orbits of planets are

typically elliptical.

Current understanding of the mechanics of orbital motion is based

on Albert Einstein's general theory of relativity, which accounts for

gravity as due to curvature of space-time, with orbits following

geodesics; though in common practice an approximate force-based

theory of universal gravitation based on Kepler's laws of planetary mot

28.

RADIUS- RADIUS

Remote Authentication Dial In User Service (RADIUS) is a

networking protocol that provides centralized Authentication,

Authorization, and Accounting (AAA) management for computers to

connect and use a network service. RADIUS was developed by

Livingston Enterprises, Inc., in 1991 as an access server authentication

and accounting protocol and later brought into the Internet Engineering

Task Force (IETF) standards.

Because of the broad support and the ubiquitous nature of the

RADIUS protocol, it is often used by ISPs and enterprises to manage

access to the Internet or internal networks, wireless networks, and

integrated e-mail services. These networks may incorporate modems,

DSL, access points, VPNs, network ports, web servers, etc.

29.

TORTISHISH-GRAVITATION

Gravitation is a natural phenomenon by which physical bodies

attract with a force proportional to their mass. In everyday life,

gravitation is most familiar as the agent that gives weight to objects with

mass and causes them to fall to the ground when dropped. Gravitation

causes dispersed matter to coalesce, and coalesced matter to remain

intact, thus accounting for the existence of the Earth, the Sun, and most

of the macroscopic objects in the universe. Gravitation is responsible for

keeping the Earth and the other planets in their orbits around the Sun;

for keeping the Moon in its orbit around the Earth; for the formation of

tides; for natural convection, by which fluid flow occurs under the

influence of a density gradient and gravity; for heating the interiors of

forming stars and planets to very high temperatures; and for various

other phenomena observed on Earth.

30.

AERODINAMIK KUCH-AERODYNAMIC FORCE

Aerodynamic force is the resultant force exerted on a body by the air

(or some other gas) in which the body is immersed, and is due to the

relative motion between the body and the fluid. An aerodynamic force

arises from two causes:

the force due to the pressure on the surface of the body

the force due to viscosity, also known as skin friction

When a body is exposed to the wind it experiences a force in the

direction in which the wind is moving. This is an aerodynamic force.

When a body is moving in air or some other gas the aerodynamic force

is usually called drag.

31.

BOSIM KUCHI-PRESSURE-GRADIENT FORCE

The pressure gradient force is not actually a 'force' but the

acceleration of air due to pressure difference (a force per unit mass). It

is usually responsible for accelerating a parcel of air from a high

atmospheric pressure region to a low pressure region, resulting in wind.

In meteorology, pressure gradient force refers to the horizontal

movement of air according to the equation

The term F / m is equal to the acceleration dv / dt because this is an

expression of Newton's law F = ma. dp / dx is the component of the

pressure gradient along the x-axis. ρ is the mass density and (1 / ρ)

shows that as the mass density increases, the acceleration due to the

pressure gradient becomes smaller.

32.

MAGNIT KUCHLARI-FORCE BETWEEN MAGNETS

Magnets exert forces and torques on each other due to the complex

rules of electromagnetism. The magnetic field of magnets are due to

microscopic currents of electrically charged electrons orbiting nuclei

and the intrinsic magnetism of fundamental particles (such as electrons)

that make up the material. Both of these are modeled quite well as tiny

loops of current called magnetic dipoles that produce their own

magnetic field and are affected by external magnetic fields. The most

elementary force between magnets, therefore, is the magnetic dipole-

dipole interaction. If all of the magnetic dipoles that make up two

magnets are known then the net force on both magnets can be

determined by summing up all these interaction between the dipoles of

the first magnet and that of the second.

It is often more convenient to model the force between two magnets

as being due to forces between magnetic poles having magnetic charges

'smeared' over them. Such a model fails to account for many important

properties of magnetism such as the relationship between angular

momentum and magnetic dipoles. Further, magnetic charge does not

exist. This model works quite well, though, in predicting the forces

between simple magnets where good models of how the 'magnetic

charge' is distributed is available.

33.

KOSMIK FAZO-SPACE PHASE

n mathematics and physics, a phase space, introduced by Willard

Gibbs in 1901,[1] is a space in which all possible states of a system are

represented, with each possible state of the system corresponding to one

unique point in the phase space. For mechanical systems, the phase

space usually consists of all possible values of position and momentum

variables.

A plot of position and momentum variables as a function of time is

sometimes called a phase plot or a phase diagram. Phase diagram,

however, is more usually reserved in the physical sciences for a diagram

showing the various regions of stability of the thermodynamic phases of

a chemical system, which consists of pressure, temperature, and

composition.

34.

ENERGIYA INTEGRALI- INTEGRAL OF ENERGY

Integral Energy is the second largest state-owned energy corporation

in New South Wales, incorporated under the Energy Services

Corporations Act 1995 from a merger between Prospect Electricity and

Illawarra Electricity. Integral Energy is involved in electricity retail in

addition to owning an electricity distribution network and currently

holds licences to retail electricity in the contestable markets covered by

the NEM (National Electricity Market).

Integral Energy distributes and retails electricity and services to

807,000 customers, or 2.1 million people. The company is increasingly

operating outside of New South Wales, with the introduction of full

retail contestability in other states. In addition to electricity retailing,

Integral Energy also owns an electricity distribution network spanning

24,500 square kilometres in Greater Western Sydney, the Illawarra, and

the Southern Highlands.

35.

IKKI JISM MASALASI- TWO-BODY PROBLEM

determine the motion of two point particles that interact only with

each other. Common examples include a satellite orbiting a planet, a

planet orbiting a star, two stars orbiting each other (a binary star), and a

classical electron orbiting an atomic nucleus (although to solve this

system correctly a quantum mechanical approach must be used).

The two-body problem can be re-formulated as two independent

one-body problems, a trivial one and one that involves solving for the

motion of one particle in an external potential. Since many one-body

problems can be solved exactly, the corresponding two-body problem

can also be solved. By contrast, the three-body problem (and, more

generally, the n-body problem for n ≥ 3) cannot be solved, except in

special cases.

36.

AYLANISH DAVRI- THE ROTATION PERIOD of an

astronomical object is the time it takes to complete one revolution

around its axis of rotation relative to the background stars. It differs

from the planet's solar day, which includes an extra fractional rotation

needed to accommodate the portion of the planet's orbital period during

one day.

37.

GIPERBOLIK TROEKTORIYA- HYPERBOLIC TRAJECTORY

In astrodynamics or celestial mechanics a hyperbolic trajectory is a

Kepler orbit with the eccentricity greater than 1. Under standard

assumptions a body traveling along this trajectory will coast to infinity,

arriving there with hyperbolic excess velocity relative to the central

body. Similarly to parabolic trajectory all hyperbolic trajectories are

also escape trajectories. The specific energy of a hyperbolic trajectory

orbit is positive.

38.

ORBITA ELEMENTLARI- ORBITAL ELEMENTS

A Kepler orbit is specified by six orbital elements, normally the

following (assuming an elliptical orbit; parabolas and hyperbolas are

also possible if eccentricity >= 1).

Two define the shape and size of the ellipse:

Eccentricity ( )

Semimajor axis ( )

Two define the orientation of the orbital plane:

Inclination ( )

Longitude of the ascending node ( )

And finally:

Argument of periapsis ( ) defines the orientation of the ellipse in

the orbital plane.

Mean anomaly at epoch (

) defines the position of the orbiting

body along the ellipse. (True anomaly ( ) is shown on the diagram,

since mean anomaly does not represent a real geometric angle.)

39.

HARAKAT-ROTATION

A three-dimensional object rotates always around an imaginary line

called a rotation axis.If the axis is within the body, and passes through

its center of mass the body is said to rotate upon itself, or spin. A

rotation about an external point, e.g. the Earth about the Sun, is called a

revolution or orbital revolution, typically when it is produced by

gravity.

40.

HARAKAT DINAMIKASI-FLIGHT DYNAMICS

Flight dynamics is the science of air vehicle orientation and control

in three dimensions. The three critical flight dynamics parameters are

the angles of rotation in three dimensions about the vehicle's center of

mass, known as pitch, roll and yaw (quite different from their use as

Tait-Bryan angles).

41.

ENERGIYA-ENERGY

In physics, energy (Ancient Greek: ένέργεια energeia "activity,

operation"[1]) is an indirectly observed quantity. It is often understood

as the ability a physical system has to do work on other physical

systems.[2][3] Since work is defined as a force acting through a distance

(a length of space), energy is always equivalent to the ability to exert

pulls or pushes against the basic forces of nature, along a path of a

certain length.

42. ZARRA OQIMI- PARTICLE BEAMS

Electron beams are used in welding, which allows energy densities up to

107 W·cm−2 across a narrow focus diameter of 0.1–1.3 mm and usually

does not require a filler material. This welding technique must be

performed in a vacuum, so that the electron beam does not interact with

the gas prior to reaching the target, and it can be used to join conductive

materials that would otherwise be considered unsuitable for welding.

Electron beam lithography (EBL) is a method of etching

semiconductors at resolutions smaller than a micron. This technique is

limited by high costs, slow performance, the need to operate the beam in

the vacuum and the tendency of the electrons to scatter in solids. The

last problem limits the resolution to about 10 nm. For this reason, EBL

is primarily used for the production of small numbers of specialized

integrated circuits

43.

MAGNIT MAYDON - MAGNETIC FIELD

magnetic field of a star is generated within regions of the interior