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Sunday, September 25, 2011

Sir.C.V.Raman, we feel proud of him.



Sir C.V.Raman and Raman Spectroscopy (1888-1970)

Sir C.V.Raman won the Nobel Prize in 1930 for discovering a new type of radiation when a material is excited by an external light source. This radiation was nothing but a signature of the molecular bonds holding the molecules together which was unique for every material. A look into the background of Sir C.V.Ramans life and a little description about the famous Raman Effect.
Chandrashekhar Venkata Raman was born on November 7th 1888 in the small village of Thiruvanaikkava near Trichinopoly, Madras Presidency (now Tiruchirapalli, state of Tamil Nadu, India) in Southern India, the son of Chandrashekara Aiyar, who became the Professor of Mathematics and Physics at the Mrs. A.V.N.College in Vishakapatnam when his son was three years old, and Parvati Ammal, who belonged to a family famous for Sanskrit Scholarship. Young Raman received an early interest in science and music from his father and a strong personality and sense of self-reliance from his mother. He attended the A.V.N. College and then the Presidency College of the University of Madras, from which he received his BA degree in 1904 at the age of 15, ranking first in his class and winning the gold medals for Physics and English. While still an undergraduate, he began research on acoustics and optics and published his first article (in the Philosophical magazine) in 1906 at the age of 18. He received his MA degree with highest honors in January 1907.

Because of ill health Raman was unable to pursue further studies at any of the universities in Great Britain (He was disqualified medically by the Civil Surgeons of Madras, who said that the rigors of English Climate would kill him) and because at that time there were no opportunities or incentives in India for a scientific career, he entered the Indian Civil Service, attaining first place on the competitive examination for a position in the Indian finance Department (The Indian Audit and Account Service was the only Government department that did not require a training period in Great Britain) . In June 1907 he was posted at Calcutta as Assistant Accountant General, and that same year he married 13-year old Lokasundari Ammal, an artist who shared his interest in musical instruments, by whom he had two sons, Chandrasekhara and Radhakrishnan. He served the Indian Finance Department in posts of increasing responsibility for a decade, much as Einstein worked as an examiner in the Swiss Patent Office. Like Einstein, he continued to carry out independent research working nights and weekends, mostly at the laboratory of the Indian Association for the Cultivation of Science at Calcutta. He worked primarily on vibrations and sound (Theoretical and experimental investigations of the oscillations of strings) and on the theory of musical instruments, especially that of violins and Indian drums.
During this period Raman published 30 papers in Nature, the Philosophical magazine, and the Physical review, which led to his being offered in 1917 the newly endowed Palit professorship of Physics at the University of Calcutta. Despite a considerable financial sacrifice, he resigned his better paying government post to accept this chair, which he held for 16 years, during which time he continued his work on acoustics and optics and made Calcutta a center for scientific research.
In the summer of 1921 Raman represented his University at the British Empire Universities Congress at Oxford and lectured on the theory of stringed instruments before the Royal Society of London. Returning home by the way of the Mediterranean Sea, he was fascinated by its opalescent, deep blue color and attempted to discover the cause. Rejecting Lord Rayleigh’s explanation that it was caused by the reflection from the sky, in 1922 Raman showed that the scattering of light by water molecules could account for the color of the sea exactly as the scattering of light by air molecules accounted for the color of the sky.

Despite his increasing preoccupation with optics, Raman also continued his research on acoustics, which resulted in his election to fellowship in the Royal Society in 1924. He worked on the excitation of strings vibrations; motion of the bowed point; the effect of the bridge in coupling the motion of the string to the body of the violin; vibration phenomena of the piano, veena and sitar; and the harmonic overtones of Indian drums. He also traveled extensively, visiting and representing India in Canada, the United States (At Nobel laureate Robert A.Millikan’s invitation he spent five months at the California Institute of technology in 1924), the USSR, Germany, Switzerland and Italy. In India he was active in organizing learned societies and journals, e.g. the Indian Science Congress (1924), The Indian Academy of Sciences (1934) and its Proceedings (In which much of his work was published) and the Indian Journal of Physics (which he founded and of which he became editor in 1926).

In the field of optics his primary concern, Raman studied light scattering by various substances, especially liquids. In April 1923 his associate K.R.Ramanathan observed a weak secondary radiation, shifted in wavelength along with normally scattered light, which was attributed to ‘fluorescence’. In January 1928, S.Venkateswaran next noticed that highly purified glycerin does not appear blue under sunlight but instead radiates a strongly polarized, brilliant, green light, they reported in Nature (March 31,1928) ‘ a new type of secondary radiation’ from the scattering of focused beams of sunlight in both carefully purified liquid and dust free air.

Raman further refined his experiment by using a mercury arc as the light source on February 28, 1928, and on March 16 he reported his results to the Indian Science Association at Bangalore in the Southern Indian state of Karnataka (‘A New Radiation’, Indian Journal of Physics, 2,387 (1928)). This secondary radiation showed several lines shifted toward longer wavelengths (The Shifts were characteristics of the substances used) and indicated the absorption of energy by the scattering molecule, an effect predicted in 1923 by the Austrian Physicist Adolf Smekal (1895-1959) and observed independently, but in less detail, several months after Raman and Krishnan’s discovery by the Soviet Physicists Grigorii Samuilovich Landsberg (1890-1957) and Leonid Isaakovich Mandelshtam (1879-1944). For his discovery, known as the Raman Effect, which Ernest Rutherford described as ‘among the best three or four discoveries in experimental physics of the decade’, Raman was awarded the Hughes Medal of the Royal Society of London (1930), the Matteucci Medal of the Societa Italiana delle Scienze (1928) was knighted by King George V of great Britain (1929) and received honorary degrees from numerous universities. In 1930 he received that ne plus ultra of science, the Nobel prize (in Physics) ‘ for his work on the scattering of light and for the discovery of the effect named after him’. He was the first Asian to receive a Nobel Prize in science. Raman continued his work on the Raman effect through the 1930’s, as did many others; almost 2,000 articles on it were published during the dozen years following its discovery.

Beginning at 1930, Raman divided his time between training future leaders of science and crystallographic studies that he thought ‘will ultimately have repercussions in the whole scientific world’. Believing that two and possibly four types of diamonds based on tetrahedral and octahedral symmetry must exist; he used a large portion of his $40,000 Nobel Prize to but diamonds. He studied their Raman spectra, fluorescence, absorption spectra, magnetic susceptibility, specific heat, X-ray diffraction patterns, and infra red spectra, and he demonstrated that the luminescence of a diamond excited by ultraviolet light is a characteristic of the diamond itself and is not due to impurities or defects, as was previously believed. He also investigated optical effects in minerals (labradorite, pearly felspar, and agate) and gems such as opal and pearls.

In 1933, Raman moved to Bangalore to become Director (1933-1937) of the Indian Institute of Science and Head of its Department of Physics (1933-1948). Here he pursued experimental and theoretical work on the diffraction of light by acoustic waves of ultrasonic and hypersonic frequencies, Brillouin scattering in liquids, light scattering in colloids, and the effects produced by X-rays on Infrared vibrations in crystals exposed to ordinary light. In 1948 Raman became the first Director of the Raman Research Institute built on land in Hebbal, a suburb of Bangalore, give by the Mysore government to the Indian Academy of Sciences. That same year he was appointed the first National Professor by the Government of a newly independent India.


Among topics investigated by Raman during his later years were colors and their perception, the spectroscopic study of flowers (the first to do this), the physiology of human color vision (he developed a new theory.), and electrical and magnetic anisotropy. A proud man of great authority, Raman was often arrogant and contemptuous of others, yet he was generous in encouraging his students. He often represented India at international meetings, was fluent in English slang, and considered himself a humorist. Educated entirely in India, he carried out pioneering scientific research when few Indians made science a career and when the Indian scientific community was small and relatively isolated. For his championing of Indian science, he was regarded, along with Rabindranath Tagore, Mahatma Gandhi, and Jawaharlal Nehru, as one of the heroes of the Indian political and cultural renaissance. He died on November 21, 1970 in Bangalore and was cremated in his beloved rose garden.

Raman Effect:-

The Raman effects, a scattering of a portion of monochromatic light when it is passed through a transparent substance, is the counterpart for visible light of the Compton effect for the X-rays. The American experimental physicist Robert Williams Wood considered it ‘one of the most convincing proofs of the quantum theory of light’. In addition to the light of the original frequency, the spectrum of the scattered light contains weaker lines (Raman lines) differing from the original frequency by constant amounts and due to the grain or loss of their energy experienced by the photons because of their interaction with the vibrating molecules of the substance through which they pass.

Since no two compounds have the same Raman Spectrum and since the intensity of a Raman line of a substance is proportional to its concentration, Raman spectroscopy can be used in qualitative and quantitative analysis. It is also employed in the elucidation of the structures of molecules, the study of the interactions between molecules and the calculation of thermodynamic properties.

Much information about a molecule can be deduced from its Raman spectrum. For example, for a diatomic molecule the effective moment of inertia in the lowest vibrational energy state and from this the effective inter-nuclear distance for this state can be obtained. Because homo-nuclear molecules such as H2 and N2 have no permanent dipole moment, they yield no pure rotational or vibrational infrared spectrum and therefore can be studied only by their Raman effect (although electronic spectra can yield rotational spectra). From an analysis of the vibrational-rotational bands there can be obtained the classical vibrational frequency of the diatomic molecule, the moments of inertia and inter-nuclear distances for higher vibrational states, the force constant, the dissociation energies, the zero point energy, the potential energy curve as a function of the inter-nuclear distance, and the rotational and vibrational energies needed for thermodynamic calculations.

Raman spectral data can also be used to detect interactions between molecules. For example, if hydrogen bonding is present, Raman displacements corresponding to C single bond H and C double bond O vibrations appear at values much lower than their normal values. The weakness of the scattered radiation have been the greatest deterrent to the widespread adoption of Raman spectroscopy as an analytical technique. Since the more intense the primary radiation source, the greater the intensity of the Raman spectra, the advent of lasers transformed this method of largely academic interest into a highly practical, powerful tool with a number of commercially available instruments and installations in many industrial laboratories. If Raman were alive today, he would undoubtedly be amazed - and –pleased by the multifaceted uses now made of his ‘new’ radiation.

Saturday, September 24, 2011

HOMI JEHANGIR BHABHA...MAKES US FEEL PROUD TO BE AN INDIAN


Homi Jehangir Bhabha

Homi J. Bhabha, considered the father of India's atomic energy program.
Born
30 October 1909
Mumbai
Died24 January 1966
ResidenceIndia 
NationalityIndian 
FieldPhysics
InstitutionsCavendish Laboratories
Tata Institute of Fundamental Research
Atomic Energy Commission of India
Alma materCambridge
Academic advisor Paul Dirac 

Friday, September 23, 2011

NEVER THINK YOU ARE OLD!


Well, here's 20 reasons, why you're never too old to accomplish your dreams...
At age 40, Hank Aaron hit his 715th home run, more than anyone had ever hit.


At age 41, Christopher Columbus landed in the New World.

At age 44, Marie Curie won the Nobel Prize in chemistry.

At age 49, Mario Puzo published, The Godfather.

At age 52, Ludwig Van Beethovan composed the Ninth Symphony.

At age 53, Margaret Thatcher was elected Prime Minister of Britain--the first woman to hold that office. Yeah, Margaret!

At age 55, Alex Haley published Roots.

At age 57, Annie Peck climbed Mount Huascaran in the Andes. She was the first person to reach the top.

At age 59, Clara Barton founded the Red Cross.

At age 63, Francis Galton revealed to the world that no two people have the same fingerprints and revolutionized crime fighting in the process.

At age 64, John Pierpont Morgan formed U.S. Steel, the world's first billion dollar corporation.

At age 65, Laura Ingalls published Little House In the Big Woods, the first story in the popular "Little House on the Prairie," series.





At age 68, Clifford Batt swam the English Channel.



At age 69, Mother Teresa won the Nobel Peace Prize.


At age 78, Grandma Moses began taking painting seriously. Soon afterward, her career took off.



At age 79, Benjamin Franklin invented the bifocals.

At age 92, George Burns starred in the movie, Eighteen Again.

At age 94, Leopold Stokowski signed a six-year contract to conduct music.

At age 95, Mother Jones, Union Organizer, wrote her famed biography.



At age 100, Ichijirou Araya climbed Mount Fuji.



KEEP THE CLOCK GOING... ITS NEVER TOO LATE FOR DOING ANYTHIe
.
__,_._,___

Thursday, September 22, 2011

10 Amazing Child Prodigies Across Time

10 Amazing Child Prodigies Across Time (Famous and Not)


A child prodigy is defined as someone under the age of 13 who is capable of excelling in at least one area of skill at a level that is considered to be an adult level in that field. There are child prodigies in all different skills areas including music, math, chess, the arts and even humanities. As long as the child shows demonstrable adult-level skill in one of these areas prior to that age 13 mark, he or she is considered a prodigy in that area. The most famous child prodigies include Mozart for music and Picasso for art. Let’s take a closer look at those two prodigies as well as eight other amazing child prodigies in different skills areas at different times throughout history.

1. Wolfgang Amadeus Mozart.

Mozart is widely considered to be one of the world’s greatest child prodigies in music because of the amazing musical feats that he mastered at an early age. It is unclear whether he had an eidetic memory or simply was trained so extensively that he was able to become so skilled at music so early on but whatever the case may be, he certainly excelled in this area. Born in 1756, Mozart began playing the harpsichord at age 3 and could read and play music by age 5. He debuted onto the classical music scene one year later and went on to be one of the most prolific composers of all time.


2. Pablo Picasso.

You know this Spanish artist because he is a famous artist but did you know that he was also a child prodigy in the arts. One of his most well-known pieces of artwork, The Picador, was created in the late nineteenth century when he was only eight years old. He began exhibiting his art by the age of 15. Picasso went on to not only create great works of art but to get deeply involved in the science and math of art, inventing numerous creations that did and did not come to fruition.

3. Sergey Karjakin.

This Ukranian boy achieved the title of Grandmaster in Chess at the tender age of 12, a record-breaking feat that happened in 2002. Chess is considered one of the few games in which child prodigies can truly exist and actually compete with adults on an equal playing field. As the youngest person to hold the title of Grandmaster, Karjakin is considered to be among the top chess prodigies of all times.

4. Cho Hunhyun.

Another game that sometimes finds itself played by child prodigies but which doesn’t get nearly as much attention as chess is the Chinese game of Go. This is a tough game to learn but there are people out there like this kid who managed to become a professional Go player in 1962 when he was only nine years old. This child prodigy is considered by many to be the best Go player of all time.

5. William James Sidis.

You know those people that you hear about primarily in fiction (or TV shows like Numb3rs) who are so smart that they go to college when they are still kids? That’s the real life story of this boy who was born at the turn of the twentieth century and who was such a prodigy in both math and linguistics that he was accepted to attend Harvard University when he was only eleven years old. Interestingly, he strayed away from math entirely in his later years but is still considered to be one of the most intelligent people ever born.

6. March Tian Boedihardjo.

 If you thought that the age of eleven was young for starting to attend college then you’ll be even more surprised by this child who got into a Hong Kong University at the age of 9, the youngest student ever accepted to college in Hong Kong. It will be interesting to see what this child prodigy opts to do with his life now that he’s getting closer to college graduation as well as to his teenage years!

7.Sufiah Yusof.

Ten years before March Tian Boedihardjo was acceted to that Hong Kong University, Sufiah Yusof was accepted to Oxford University to study mathematics there. She was only twelve years old. This particular child prodigy interests me because it is rare to see female child prodigies and it is still rare to see women in advanced math careers so her experience as a modern-day child prodigy female in math was truly unique. But there’s more to this story. The pressure of the life was too much for her and it is rumored that she has spent the past ten years bouncing from waitressing jobs to prostitution to back to school. Imagine that! Being smart isn’t always easy at all.

8. Lucretia Maria Davidson.

Here is a more positive example of a female child prodigy although one that does have a somewhat sad ending. This woman born in the early nineteenth century was a child prodigy of words who made her mark as an astounding poet of her time before the age of 11. Sadly, her work as a poet lasted only five years because her life was cut short due to death by tuberculosis but she did manage to make her mark on history as a child prodigy in the art of poetry.

9. William Cullen Bryant.

This man is another poet who gained adult-level praise for his work before the age of 13 and so is considered a child prodigy of poetry. Also born in the early nineteenth century, Bryant published his first book at the age of ten. By the age of 13, he had completed a book of satire poems that were widely recognized for their advanced quality. 

10. Jean-François Champollion.

I am totally fascinated by the life of this man who was born at the end of the eighteenth century. His work was in deciphering Egyptian hieroglyphics which just sounds so interesting but he was considered a child prodigy before that due to the fact that he could speak several dead languages before the age of ten. By 16, he could speak more than one dozen languages in spite of the fact that his only teacher was a brother who himself was largely self-taught. Wow!

ANOTHER INDIAN TO MAKE US PROUD.


আচার্য জগদীশ চন্দ্র বসু
Acharyo-Jogodiish-Chondro-Boshū
Acharya Sir Jagadish Chandra Bose, CSI, CIE, FRS

Jagadish Chandra Bose in Royal Institution, London
Born30 November 1858
BikrampurBengal PresidencyBritish India
Died23 November 1937 (aged 78)
GiridihBengalBritish India
ResidenceKolkataBengalBritish India
NationalityBritish Indian
FieldsPhysicsBiophysicsBiologyBotany,ArchaeologyBengali LiteratureBangla Science Fiction
InstitutionsUniversity of Calcutta
University of Cambridge
University of London
Alma materSt. Xavier's College, Calcutta
University of Cambridge
Doctoral advisorJohn Strutt (Lord Rayleigh)
Notable studentsSatyendra Nath Bose
Known forMillimetre waves
Radio
Crescograph Plant science
Notable awardsCompanion of the Order of the Indian Empire (CIE) (1903)
Companion of the Order of the Star of India (CSI) (1911)
Knight Bachelor (1917)

Tuesday, September 20, 2011

Invention of the Telescope////Sorce 'The net'



Johannes Hevelius observing with one of his telescopes [click for larger image]
The Telescope
The telescope was one of the central instruments of what has been called the Scientific Revolution of the seventeenth century. It revealed hitherto unsuspected phenomena in the heavens and had a profound influence on the controversy between followers of the traditional geocentric astronomy and cosmology and those who favored the heliocentric system of Copernicus. It was the first extension of one of man's senses, and demonstrated that ordinary observers could see things that the great Aristotle had not dreamed of. It therefore helped shift authority in the observation of nature from men to instruments. In short, it was the prototype of modern scientific instruments. But the telescope was not the invention of scientists; rather, it was the product of craftsmen. For that reason, much of its origin is inaccessible to us since craftsmen were by and large illiterate and therefore historically often invisible.
Although the magnifying and diminishing properties of convex and concave transparent objects was known in Antiquity, lenses as we know them were introduced in the West [1] at the end of the thirteenth century. Glass of reasonable quality had become relatively cheap and in the major glass-making centers of Venice and Florence techniques for grinding and polishing glass had reached a high state of development. Now one of the perennial problems faced by aging scholars could be solved. With age, the eye progressively loses its power to accommodate, that is to change its focus from faraway objects to nearby ones. This condition, known aspresbyopia, becomes noticeable for most people in their forties, when they can no longer focus on letters held at a comfortable distance from the eye. Magnifying glasses became common in the thirteenth century, but these are cumbersome, especially when one is writing. Craftsmen in Venice began making small disks of glass, convex on both sides, that could be worn in a frame--spectacles. Because these little disks were shaped like lentils, they became known as "lentils of glass," or (from the Latin) lenses. The earliest illustrations of spectacles date from about 1350, and spectacles soon came to be symbols of learning.
The Spectacle Vendor by Johannes Stradanus, engraved by Johannes Collaert, 1582 [click for larger image]


These spectacles were, then, reading glasses. When one had trouble reading, one went to a spectacle-maker's shop or a peddler of spectacles (see figs. 2 and 3) and found a suitable pair by trial and error. They were, by and large, glasses for the old. spectacles for the young, concave lenses[2] that correct the refractive error known as myopia, were first made (again in Italy) in the middle of the fifteenth century. So by about 1450 the ingredients for making a telescope were there. The telescopic effect can be achieved by several combinations of concave and convex mirrors and lenses. Why was the telescope not invented in the fifteenth century? There is no good answer to this question, except perhaps that lenses and mirrors of the appropriate strengths were not available until later.
In the literature of white magic, so popular in the sixteenth century, there are several tantalizing references to devices that would allow one to see one's enemies or count coins from a great distance. But these allusions were cast in obscure language and were accompanied by fantastic claims; the telescope, when it came, was a very humble and simple device. It is possible that in the 1570s Leonard and Thomas Digges in England actually made an instrument consisting of a convex lens and a mirror, but if this proves to be the case, it was an experimental setup that was never translated into a mass-produced device.[3]
The earliest known illlustration of a telescope. Giovanpattista della Porta included this sketch in a letter written in August 1609
[click for larger image]
The telescope was unveiled in the Netherlands. In October 1608, the States General (the national government) in The Hague discussed the patent applications first of Hans Lipperhey of Middelburg, and then of Jacob Metius of Alkmaar, on a device for "seeing faraway things as though nearby." It consisted of a convex and concave lens in a tube, and the combination magnified three or four times.[4] The gentlemen found the device too easy to copy to award the patent, but it voted a small award to Metius and employed Lipperhey to make several binocular versions, for which he was paid handsomely. It appears that another citizen of Middelburg, Sacharias Janssen had a telescope at about the same time but was at the Frankfurt Fair where he tried to sell it.

Galileo's telescopes
[click here for larger image]


The news of this new invention spread rapidly through Europe, and the device itself quickly followed. By April 1609 three-powered spyglasses could be bought in spectacle-maker's shops on the Pont Neuf in Paris, and four months later there were several in Italy. (fig. 4) We know that Thomas Harriot observed the Moon with a six-powered instrument early in August 1609. But it was Galileo who made the instrument famous. He constructed his first three-powered spyglass in June or July 1609, presented an eight-powered instrument to the Venetian Senate in August, and turned a twenty-powered instrument to the heavens in October or November. With this instrument (fig. 5) he observed the Moon, discovered four satellites of Jupiter, and resolved nebular patches into stars. He published Sidereus Nuncius in March 1610.
Verifying Galileo's discoveries was initially difficult. In the spring of 1610 no one had telescopes of sufficient quality and power to see the satellites of Jupiter, although many had weaker instruments with which they could see some of the lunar detail Galileo had described in Sidereus Nuncius. Galileo's lead was one of practice, not theory, and it took about six months before others could make or obtain instruments good enough to see Jupiter's moons. With the verification of the phases of Venus by others, in the first half of 1611, Galileo's lead in telescope-making had more or less evaporated. The next discovery, that of sunspots, was made by several observers, including Galileo, independently.
???


A typical Galilean telescope with which Jupiter's moons could be observed was configured as follows. It had a plano-convex objective (the lens toward the object) with a focal length of about 30-40 inches., and a plano-concave ocular with a focal length of about 2 inches. The ocular was in a little tube that could be adjusted for focusing. The objective lens was stopped down to an aperture of 0.5 to 1 inch. , and the field of view was about 15 arc-minutes (about 15 inches in 100 yards). The instrument's magnification was 15-20. The glass was full of little bubbles and had a greenish tinge (caused by the iron content of the glass); the shape of the lenses was reasonable good near their centers but poor near the periphery (hence the restricted aperture); the polish was rather poor. The limiting factor of this type of instrument was its small field of view--about 15 arc-minutes--which meant that only a quarter of the full Moon could be accommodated in the field. Over the next several decades, lens-grinding and polishing techniques improved gradually, as a specialized craft of telescope makers slowly developed. But although Galilean telescopes of higher magnifications were certainly made, they were almost useless because of the concomitant shrinking of the field.
As mentioned above, a the telescopic effect can be achieved with different combinations of lenses and mirrors. As early as 1611, in his Dioptrice,Johannes Kepler had shown that a telescope could also be made by combining a convex objective and a convex ocular. He pointed out that such a combination would produce an inverted image but showed that the addition of yet a third convex lens would make the image erect again. This suggestion was not immediately taken up by astronomers, however, and it was not until Christoph Scheiner published his Rosa Ursina in 1630 that this form of telescope began to spread. In his study of sunspots, Scheiner had experimented with telescopes with convex oculars in order to make the image of the Sun projected through the telescope erect.[5] But when he happened to view an object directly through such an instrument, he found that, although the image was inverted, it was much brighter and the field of view much larger than in a Galilean telescope. Since for astronomical observations an inverted image is no problem, the advantages of what became known as the astronomical telescope led to its general acceptance in the astronomical community by the middle of the century.
The Galilean telescope could be used for terrestrial and celestial purposes interchangeably. This was not true for the astronomical telescope with its inverted image. Astronomers eschewed the third convex lens (the erector lens) necessary for re-inverting the image because the more lenses the more optical defects multiplied. In the second half of the seventeenth century, therefore, the Galilean telescope was replaced for terrestrial purposes by the "terrestrial telescope," which had four convex lenses: objective, ocular, erector lens, and a field lens (which enlarged the field of view even further).
Hevelius's 60- and 140-foot telescopes (Machina Coelestis, 1673) [click for larger image]


With the acceptance of the astronomical telescope, the limit on magnification caused by the small field of view of the Galilean telescope was temporarily lifted, and a "telescope race" developed. Because of optical defects, the curvature of lenses had to be minimized, and therefore (since the magnification of a simple telescope is given roughly by the ratio of the focal lengths of the objective and ocular) increased magnification had to be achieved by increasing the focal length of the objective. Beginning in the 1640s, the length of telescopes began to increase. From the typical Galilean telescope of 5 or 6 feet in length, astronomical telescopes rose to lengths of 15 or 20 feet by the middle of the century. A typical astronomical telescope is the one made by Christiaan Huygens, in 1656. It was 23 feet long; its objective had an aperture of several inches, it magnified about 100 times, and its field of view was 17 arc-minutes.
Aerial telescope (Christiaan Huygensm Astroscopium Compendiaria,1684) [click for larger image]


Telescopes had now again reached the point where further increases in magnification would restrict the field of view of the instrument too much. This time another optical device, the field lens came to the rescue. Adding a third convex lens--of appropriate focal length, and in the right place--increased the field significantly, thus allowing higher magnifications. The telescope race therefore continued unabated and lengths increased exponentially. By the early 1670s, Johannes Hevelius had built a 140-foot telescope.
But such long telescopes were useless for observation: it was almost impossible to keep the lenses aligned and any wind would make the instrument flutter. After about 1675, therefore, astronomers did away with the telescope tube. The objective was mounted on a building or pole by means of a ball-joint and aimed by means of a string; the image was found by trial and error; and the compound eyepiece (field lens and ocular), on a little stand, was then positioned to receive the image cast by the objective. Such instruments were called "aerial telescopes."
Although some discoveries were made with these very long instruments, this form of telescope had reached its limits. By the beginning of the eighteenth century very long telescopes were rarely mounted any more, and further increases of power came, beginning in the 1730s, from a new form of telescope, the reflecting telescope.
Since it was known that the telescopic effect could be achieved using a variety of combinations of lenses and mirrors, a number of scientists speculated on combinations involving mirrors. Much of this speculation was fueled by the increasingly refined theoretical study of the telescope. In his Dioptrique, appended to his Discourse on Method of 1637, René Descartes addressed the problem of spherical aberration, already pointed out by others. In a thin spherical lens, not all rays from infinity--incident parallel to the optical axis--are united at one point. Those farther from the optical axis come to a focus closer to the back of the lens than those nearer the optical axis. Descartes had either learned the sine law of refraction from Willebrord Snell (Snell's Law)[6] or had discovered it independently, and this allowed him to quantify spherical aberration. In order to eliminate it, he showed, lens curvature had to be either plano-hyperboloidal or spherico-ellipsoidal. His demonstration led many to attempt to make plano-hyperboloidal objectives, an effort which was doomed to failure by the state of the art of lens-grinding. Others began considering the virtues of a concave paraboloidal mirror as primary receptor: it had been known since Antiquity that such a mirror would bring parallel incident rays to a focus at one point.
Newton's reflecting telescope (1671)
[click for larger image]


A second theoretical development came in 1672, when Isaac Newton published his celebrated paper on light and colors. Newton showed that white light is a mixture of colored light of different refrangibility: every color had its own degree of refraction. The result was that any curved lens would decompose white light into the colors of the spectrum, each of which comes to a focus at a different point on the optical axis. This effect, which became known as chromatic aberration, resulted in a central image of, e.g., a planet, being surrounded by circles of different colors. Newton had developed his theory of light several years before publishing his paper, when he had turned his mind to the improvement of the telescope, and he had despaired of ever ridding the objective of this defect. He therefore decided to try a mirror, but unlike his predecessors he was able to put his idea into practice. He cast a two-inch mirror blank of speculum metal (basically copper with some tin) and ground it into spherical curvature. He placed it in the bottom of a tube and caught the reflected rays on a 45� secondary mirror which reflected the image into a convex ocular lens outside the tube (see fig. 12). He sent this little instrument to the Royal Society, where it caused a sensation; it was the first working reflecting telescope. But the effort ended there. Others were unable to grind mirrors of regular curvature, and to add to the problem, the mirror tarnished and had to be repolished every few months, with the attending danger of damage to the curvature.
Hevelius's rooftop observatory, (Machina Coelestis, 1673)
[click for larger image]


The reflecting telescope therefore remained a curiosity for decades. In second and third decades of the eighteenth century, however, the reflecting telescope became a reality in the hands of first James Hadley and then others. By the middle of the century, reflecting telescopes with primary mirrors up to six inches in diameter had been made. It was found that for large aperture ratios (the ratio of focal length of the primary to its aperture, as the f-ratio in modern cameras for instance), f/10 or more, the difference between spherical and paraboloidal mirrors was negligible in the performance of the telescope. In the second half of the eighteenth century, in the hands of James Short and then William Herschel, the reflecting telescope with parabolically ground mirrors came into its own.


 Galileo disproved that the earth is the center of the universe

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