Yes, with the help of infrared telescope to decode mysteries into the space that uses infrared light to detect the celestial bodies. The world’s largest optical and infrared telescope, that will help scientists to understand and explore the universe. Universe is currently being built in chile by the European southern observatory. The telescope has a main mirror which is 39 meters in diameter. Unique in features, the extra large telescope (ELT) is modeled as an adaptive telescope with the ability of checking and correcting atmospheric turbulence's. The giant telescope is all set for completion and launch n 2024. Scientists from oxford university are playing a major role in the ambitious project, the team is responsible for the construction and design of the telescope’s spectrograph, called ‘harmoni’, a specially developed equipment to simultaneously take almost 4,000 images, each in slightly different color tones. The near infrared instrument will provide extremely vivid images that will more magnify and that will more explore the universe. 

Any location on earth is described by two numbers – its latitude and its longitude.

On a globe of the earth, lines of latitude are circles of different size. The longest is the equator, whose latitude is zero, while at the poles – at latitude 90 degree north and 90 degree south (or -90 degree) the circles shrink to a point.

On the globe, lines of constant longitudes (‘meridians’) extend from pole to pole.

Every meridian must cross the equator. Since the equator is a circle, we can divide it like any circle into 360 degrees, and the longitude of a point is then the marked value of that division where its meridian meet s the equator.

For the historical reasons, the longitude (meridian) passing the old royal astronomical observatory in Greenwich, England is the one chosen as zero longitude. Located at the eastern edge of London, the British capital, the observatory is now a public museum and a brass band stretching across its yard mark the “prime meridian”.

A line of longitude is also called a meridian, derived from the latin, from meri, a variation of “medius” which denotes “middle”, and diem, meaning “day”. The word once meant “noon”, and times of the day before noon were known as “ante meridian”, while times after it were “post meridian”. Today’s observations a.m. and p.m. come from these terms, and the sun at noon was said to be “passing meridian”. All points on the same line of longitude experienced noon (and any other hour) at the same time and were therefore said to be on the same “meridian line”.

Named after the physicist who discovered them, these are two bands of the outermost layer of the atmosphere (magnetosphere), at heights of 3000 km and 16000 km above the earth’s surface. Here the ionized particles trapped by the earth’s magnetic field from the solar radiation, concentrate.

All the planet move around the sun in elliptical orbits, with the sun being at rest at one focus of the orbit.

The position vector of the planet with the sun at the region sweeps out equal area in equal time i.e. the areal velocity of planet around the sun always remains constant.

A consequences of this law is that the speed of planet increases when the planet is closer to the sun and decreases when the planet is far away from the sun.

Speed of a planet is maximum when it is at perigee and minimum when it is apogee.

The square of the period of revolution of a planet around the sun is directly proportional to the cube of mean distance of planet from the sun.

If T is period of revolution and r is the mean distance of planet from sun then T^2 proportional r^3.

Clearly distant planets have larger period of revolution. The time period of nearest planet mercury is 88 days where as time period of farthest planet Pluto is 247.7 years.

Satellites are natural or artificial bodies revolving around a planet under its gravitational attraction. Moon is a natural satellite while INSAT-IB is an artificial satellite of earth.

Orbital speed of a satellite is independent of its mass. Hence satellites of different masses revolving in the orbit of same radius have same orbital speed.

Orbital speed of a satellite depends upon the radius of orbit (height of satellite from the surface of earth ). Greater the radius of orbit, lesser will be the orbital speed.

The orbital speed of a satellite revolving near the surface of earth is 7.9 km/sec.

Time taken by a satellite to complete one revolution in its orbit is called its period of revolution.

i.e. period of revolution = circumference of orbit/orbital speed

period of revolution of a satellite depends upon the height of satellite from the surface of the earth.

Greater the height, more will be the period of revolution.

Period of revolution of a satellite is independent of its mass.

The period of revolution of satellite revolving near the surface of earth is 1 hour 24 minute (84 minute).

If a satellite revolves in equatorial plane in the direction of earth’s rotation i.e. from west to east with a period of revolution equal to time period of rotation of earth on its own axis i.e. 24 hours, then the satellite will appear stationary relative to earth. Such a satellite is called geo-stationary satellite. Such a satellite revolves around the earth at a height of 36000 km. the orbit of geo-stationary satellite is called parking orbit. Arthur c. clarck was first to predict that a communication satellite can be stationed in the geosynchronous orbit.

Escape velocity is that minimum velocity with which a body should be projected from the surface of earth so as it goes out of gravitational field of earth and never return to earth.

Escape velocity is independent of the mass, shape and size of the body and its direction of projection.

Escape velocity is also called second cosmic velocity.

For earth escape velocity = 11.2 km/s.

For moon escape velocity =2.4 km/s.

Orbital velocity of a satellite V0 =√g R and escape velocity Ve = √2gR

Where R = radius of earth i.e. Ve = √2V0 i.e. escape velocity is √2 times the orbital velocity.

Therefore if the orbital velocity of a satellite is increased to √2 times (increased by 41%), the satellite will leave the orbit and escape.

Weather is the description of the atmospheric conditions of a particular place at a particular time for a short period of time.

Climate is the composite or integrated picture of the weather conditions over a long period of time.

Climatic data is based on calculated averages of the data recorded over a period of 35 years. The classical period is 30 years, as defined by WMO.

Atmospheric pressure is the pressure at any point on the surface of the earth due to the weight of the column of air above that point.

Hydrogen and the helium are the predominant gases that constitute the sun. the proportion of hydrogen to helium is 3:1.

The core of the sun acts like a gigantic nuclear reactor and converts huge quantity of hydrogen into helium. In this process of nuclear fusion, the sun releases tremendous amount of energy in all directions.

The sun radiates energy (both heat and light) in all directions.

Because of its small size in relation to the sun, the earth intercepts only a small part of the sun’s radiant energy.

Solar radiations are the primary source of heat and light to the earth.

The incoming solar radiation (energy intercepted by the earth) is known as insolation and it is received in the form of short waves.

The sun’s energy absorbed by the earth’s surface when radiated out into space is called terrestrial radiation.

Troposphere

Stratosphere

Mesosphere

Thermosphere

Exosphere

This is the first layer of the atmosphere. It extends to a height of 18 km at the equator and 8 km at the poles.

In this layer temperature decreases with the height. This is due to the fact that the density of air decreases with height and so the heat absorbed is less. It contains more than 90% of gases in the atmosphere.

Since most of the water vapour form clouds in this layer, all weather changes occur in the troposphere (‘tropo’ means ‘change’).

The height at which the temperature stops decreasing is called tropopause. Here the temperature may be as low as -58 degree Celsius.

This is the second layer of the atmosphere. It extends from the tropopause to about 50 km.

Temperature increases due to the absorption of the ultraviolet radiation of the sun by ozone present in this layer. The temperature slowly increases to 4 degree Celsius.

This layer is free from clouds and associate weather phenomena. Hence it provides ideal flying conditions for large jet planes.

At about 50 km the temperature begins to fall again. This marks the end of the stratosphere. The end of the stratosphere is called the stratopause.

Above the stratosphere lies the mesosphere.

The mesosphere extends to a height of 80 km.

Here the temperature decreases again, falling as low as -90 degree Celsius.

The end of this layer is known as the mesopause.

The thermosphere lies above the mesosphere.

This layer extends to a height of about 640 km.

In this layer temperature rises dramatically reaching upto 1480 degree Celsius.

This increase in temperature is due to the fact that the gas molecules in this layer absorb the x-rays and ultraviolet radiation of the sun.

This results in the break up of the gas molecules into positively and negatively charged particles or ions. Thus, this layer is also known as the ionosphere.

The electricity charged gas molecules of the thermosphere reflect radio waves from the earth back into space. Thus this layer also helps in long distance communications.

The thermosphere also protects us from meteors and obsolete satellites, because its high temperature burns up nearly all the debris coming towards the earth.

This layer lies above the thermosphere.

The exosphere extends beyond the thermosphere upto 960 km.

It gradually merges with interplanetary space.

The temperature in this layer range from about 300 degree Celsius to 1650 degree Celsius.

This layer contains only traces of gases like oxygen, nitrogen, argon and helium because the lack of gravity allows the gas molecules to escape easily into space.

The envelope of air that completely surrounds the earth is known as atmosphere.

The atmosphere extends to about 1000 km from the surface of the earth. But 99% of the total mass of the atmosphere is found within 32 km.

This is because the atmosphere is held by the gravitational pull of the earth.

Nitrogen – 78%

Oxygen – 21%

Argon – 0.93%

Carbon dioxide – 0.03%

Neon – 0.0018%

Helium – 0.00005%

Ozone – 0.0006%

Hydrogen – 0.00005%

Carbon dioxide:  it is present in small quantity in the atmosphere. It is an important constituent of air because it has the ability to absorb heat and thus keep the atmosphere warm, thereby, balancing the heat of the earth.

Water vapour:  it is the most significant component of the atmosphere as far as its effect on weather is concerned although its quantity varies considerably from practically none (0) to upto about 4% by volume. Water vapour is the source of all clouds and precipitation (rain, hail storm etc.). water vapour , like carbon dioxide, has the ability to absorb heat energy. It also regulates the hydrological cycle.

Dust :  intercepts and reflect incoming insolation.

The polluted particles present in the air not only absorb larger amount of insolation but also greatly absorb the terrestrial radiation. Dust in the atmosphere contributes to the red and orange color of sunrise and sunset.

Torrid zone

This is also referred to as Tropical zone. The tropics is a region on the earth surrounding equator by the tropic of cancer in the northern hemisphere at 23 degree 26’16” s (approx). the tropics include all the areas on the earth where the sun reaches a point directly overhead at least once in a year.

This area receives maximum heat and is called the torrid zone.

Frigid zone

Near the polar regions, the rays of the sun are very slanting and so it is very cold.

The region//area between the arctic circle and the north pole in the northern hemisphere is called the frigid zone.

There are similar regions in the southern hemisphere between the Antarctic circle and the south pole, also called the frigid zone (here frigid means cold).

The earth spins (rotates), west to east on its axis once in 24 hours approximately.

The earth’s axis not vertical. It makes an angle of 23 degree 30’ (minutes), with the vertical or 66 degree 30’ (minutes), with the plane of earth’s orbit.

The earth’s axis always remains pointed in the same direction (towards the pole star) as the earth moves around the sun. the tilt of the earth’s axis is known as the inclination of the earth’s axis.

Rotation of the earth on its tilted axis causes  days and nights to be of different length in different parts of the earth.

Since the earth’s axis is tilted in the same direction, the orientation of the earth’s axis to the sun’s rays is constantly changing as the erth moves around the sun. this results in a continuous change in the length of days and nights throughout the year.

The position of the earth or any other planet in its orbit when it is at its nearest point to the sun.

The earth reaches its perihelion about 3^rd January at a distance of about 147 million kilometer near one extremity  of the major axis of the earth’s elliptical orbit, the axis being called apsides line.

The position of the earth or any other planet in its orbit when it is at its distant point from the sun.

The earth reaches its aphelion on 4^th july when the earth is at a distance of 152 million kilometer near the other extremity of the major axis.

Solstice is one of the two dates in the year on which the sun reaches greatest altitude north or south of the equator and is directly overhead along one of the lines of the tropics.

On june 21, the earth is so located in its orbit that the sun is overhead on the tropic of cancer ( 23 ½ degree north ).

On this date the northern hemisphere is tipped towards the sun having the longest day, while the southern hemisphere is tipped away from the sun having the shortest day.

On December 22, the earth is in an equivalent position on the opposite points in its orbit, so the southern hemisphere is tipped towards the sun and the northern hemisphere away from it.

The sun is overhead on the tropic of Capricorn ( 23 ½  degree south), resulting in the shortest day in the northern hemisphere.

Two days in a year when day and night are equal throughout the world are equinoxes.

Falling midway between the dates of solstices, on these dates, the earth’s axis lies at 90 degree to the line joining the centres of the earth and the sun and neither the northern nor the southern hemisphere is inclined towards the sun.

The ‘vernal equinox’ occurs on march 21 and it is also called the spring equinox in the northern hemisphere.

The ‘autumnal equinox’ occurs on September 23.

This phenomenon is observed in the arctic and Antarctic zones around mid-summer, when the sun does not sink below the horizon throughout 24 hours of the day and therefore, may be seen at midnight.

This is the direct consequence of the inclination of the axis of the earth to the plane of the orbit.

Norway is the place of midnight sun where the sun is continuously visible between may and july.

In the southern hemisphere, the phenomenon is seen in the Antarctica continent.

An eclipse occurs when the sun, moon and the earth are in a straight line.

A ‘solar eclipse’ occurs between sunrise and sunset on new moon when the moon passes directly in front of the sun so that its shadow lies on the earth. In other words, the moon lies between the sun and the earth.

The ‘lunar eclipse’ takes place when the earth comes in between the sun and the moon so that the shadow of the earth is cast on the moon.

A lunar eclipse takes place on a full moon.

Generally a total of seven eclipses, including solar and lunar eclipses, takes place every year.

There are two important concepts, related to latitude and longitude (especially) are local time (LT) and universal time (UT).

Longitudes are measured from zero to 180 degree east and 180 degree west (or -180), and both 180 degree longitudes share the same line, in the middle of the pacific ocean.

As the earth rotates around its axis, at any moment one line of the longitude ‘the noon meridian’ faces the sun, and at that moment, it will be noon everywhere on it. After 24 hours the earth has undergone a full rotation with respect to the sun, and the same meridian again faces noon. Thus each hour the earth rotates by 360/24 = 15 degree.

Longitude determines only the hour of the day, i.e. not the date, which is determined separately. The international date line has been established most of it following the 180^th meridian where by common agreement, whenever we cross it the date advances one day (going west) or goes back one day (going east).

That line passes the bering strait between Alaska and Siberia, which thus have different dates, but for most of its course it runs in mid ocean and does not inconvenience any local time keeping.

Astronomers, astronauts and people dealing with satellite data may need a time schedule which is the same everywhere, not tied to a locality or time zone. The Greenwich mean time, the astronomical time at Greenwich (average over the year) is generally used here. It is sometimes called universal time (UT). 

Hydrosphere (or sea) covers five-sevenths or more accurately 70.78% (36,10,59,226 sq. km) of the total surface area of the earth.

Water is freely available in the gaseous, liquid and solid state.

It is necessary for carrying out chemical reactions within the bodies of the living organism.

Water also dissolves and transports nutrients from the soil to the pants.

It is used by plants for making food.