TET MATERIALS | TET QUESTION PAPERS

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TNPSC MATERIALS | TNPSC QUESTION PAPERS

PLUS TWO MATERIALS | PLUS TWO QUESTION PAPERS

KALVISOLAI - TN FLASH NEWS

  1. TRB - PHYSICS - PG - PGTRB - POLYTECHNIC TRB- LATEST STUDY MATERIALS DOWNLOAD | மாநில அளவில் முதலிடம் பெற _ PG TRB PHYSICS _ QUESTION BANK _ BY V . KARIKALAN
  2. TRB - EDUCATION METHODOLOGY - BT - PG - PGTRB - POLYTECHNIC - LATEST STUDY MATERIALS DOWNLOAD BY V. KARIKALAN – 8807432425
  3. DGE - SSLC JUN/JULY 2017 - PRIVATE CANDIDATE HALL TICKET DOWNLOAD | எஸ்எஸ்எல்சி துணை தேர்வுக்கு அனுமதிச்சீட்டை 21-ம் தேதி (புதன்கிழமை) முதல் அரசு தேர்வுத் துறையின் இணையதளத்தில் (www.dge.tn.gov.in) இருந்து பதிவிறக்கம் செய்துகொள்ளலாம்.
  4. TNEA 2017 Random Number and Rank Publication |பொறியியல் படிப்புக்கு 1.40 லட்சம் பேர் விண்ணப்பம் கணினி மூலம் ரேண்டம் எண் ஒதுக்கீடு.
  5. முதுகலை பட்டதாரிகள் பிஎட் சேர குறைந்தபட்ச மதிப்பெண் தகுதி தேவையில்லை இந்த ஆண்டு புதிய நடைமுறை அமல்
  6. 660 உதவிப் பேராசிரியர் பணியிடங்கள் உருவாக்கப்படும் முதல்-அமைச்சர் எடப்பாடி பழனிசாமி அறிவிப்பு
  7. சென்னை டி.பி.ஐ. வளாகத்தில் செயல்படும் பள்ளி கல்வி இயக்ககத்திற்கு ரூ.33 கோடியில் புதிய கட்டிடம் எடப்பாடி பழனிசாமி அறிவிப்பு
  8. பிஎட் படிப்புக்கான அரசு ஒதுக்கீட்டில் உள்ள இடங்களுக்கு ஜூன் 21 முதல் விண்ணப்பம் வழங்கப்படும் என்று கல்லூரி கல்வி இயக்குநர் ஜெ.மஞ்சுளா அறிவித்துள்ளார்.
  9. TRB GOVT POLYTECHNIC LECTURER NOTIFICATION | VACANCIES:1058 | EXAM DATE:13.08.17 | ONLINE APPLY LAST DATE: 07.07.17
  10. PG TRB HALL TICKET PUBLISHED | DIRECT RECRUITMENT OF POST GRADUATE ASSISTANTS FOR THE YEAR 2015 - 16 AND 2016 - 17 - PLEASE CLICK HERE FOR HALL TICKET DOWNLOAD
  11. எஸ்எஸ்எல்சி சிறப்பு துணை பொதுத்தேர்வுக்கான அறிவியல் செய்முறைத்தேர்வு வரும் ஜூன் 22, 23 ஆகிய தேதிகளில் நடைபெறும் என்று அரசு தேர்வுத்துறை அறிவித்துள்ளது.
  12. பிளஸ்-2 சிறப்பு துணைத்தேர்வுக்கு ஹால் டிக்கெட் இன்று (16.06.2017) முதல் பதிவிறக்கம் செய்து கொள்ளலாம்
  13. NEET 2017 தேர்வுக்கான விடைகள் இணையதளத்தில் வெளியீடு
  14. TNSCHOOLS 2017-2018 SCHOOL CALENDAR DOWNLOAD | மேல்நிலை,உயர்நிலை,நடுநிலை மற்றும் தொடக்கப்பள்ளிகளுக்கான வேலை நாள் காட்டியை பள்ளிக்கல்வித்துறை மற்றும் தொடக்கக்கல்வித்துறை இணைந்து வெளியிட்டுள்ளது. அதில் 2017-18ம் கல்வியாண்டுக்கான மாதவாரியாக பள்ளி வேலைநாட்கள் மற்றும் செயல்பாடுகள் விவரங்கள் குறிப்பிடப்பட்டுள்ளன.
  15. பள்ளிக்கல்வித் துறையில் 43 புதிய அறிவிப்புக்களை வெளியிட்டார் பள்ளிக்கல்வித்துறை அமைச்சர் கே.ஏ. செங்கோட்டையன்...விரிவான விவரங்கள்...
  16. TAMIL NADU HOUSING BOARD | RECRUITMENT NOTIFICATION | TNHB அறிவித்துள்ள வேலைவாய்ப்பு அறிவிப்பு . விண்ணப்பிக்க கடைசி தேதி 30.06.2017
  17. CSIR UGC NET ADMIT CARD 2017 DOWNLOAD | நெட் தேர்வுக்கு வி்ண்ணப்பித்த தகுதியான நபர்களுக்கு www.csirhrdg.res.in என்ற இணையதளத்தில் ஹால்டிக்கெட் பதிவேற்றம் செய்யப்பட்டுள்ளது.
  18. பள்ளி மாணவர்களுக்கான புதிய பாடத்திட்டத்தை உருவாக்கும் பணியில் கல்வியாளர்கள் பங்கு பெறலாம் என SCERT இயக்குனர் அறிவிப்பு.ஆர்வமுள்ளவர்கள் www.tnscert.org என்ற இணையதள முகவரியில் தங்களது விவரங்களை வருகிற 23-ந் தேதிக்குள் பதிவு செய்ய வேண்டும்.
  19. TEACHERS GENERAL COUNSELLING 2017-2018 HELP CENTRE | FORMS | SCHEDULE | NORMS | MUTUAL TRANSFER FORM
  20. TRB PGT EXAM NOTIFICATION 2017 DOWNLOAD
    Date of Notification : 09.05.2017 | Commencement of submission of application through online mode : 10.05.2017 | Last date for submission of application through online mode : 30.05.2017 | Date of Written Examination : 02.07.2017
  21. TNPSC GROUP-2A 1953 POST NOTIFICATION | விண்ணப்பிக்க கடைசி நாள் 26.05.2017 தேர்வு நாள் 06.08.2017
  22. TN TEACHERS PROMOTION PANEL 2017-2018 DOWNLOAD
  23. SSLC (10TH) EXAMINATION RESULTS - MARCH 2017 LINK-1 (AVAILABLE)
  24. SSLC (10TH) EXAMINATION RESULTS - MARCH 2017 LINK-2 (AVAILABLE)
  25. SSLC (10TH) EXAMINATION RESULTS - MARCH 2017 LINK-3 (AVAILABLE)
  26. SSLC (10TH) EXAMINATION RESULTS - MARCH 2017 LINK-4 (AVAILABLE)
  27. MBBS IN CHINA | நீங்கள் சீனாவில் எம்.பி.பி.எஸ் படிக்க விருப்பமா ?
  28. DSE JD TRANSFER, CEO TRANSFER AND DEO PROMOTION LIST 2017 DOWNLOAD
  29. NEET (UG) 2017 PHYSICS-CHEMISTRY-BIOLOGY PAPER WITH ANSWER DOWNLOAD
  30. TNTET PAPER 1 AND PAPER 2 QP ANSWER KEY DOWNLOAD
  31. PG REGULARAISATION ORDER - BATCH 2013-14, 2014-15 DOWNLOAD
  32. TRB ANNUAL PLANNER 2017 DOWNLOAD
  33. TNPSC ANNUAL PLANNER 2017 DOWNLOAD
  34. AKASH IAS ACADEMY TNTET COACHING CENTRE STUDY MATERIALS DOWNLOAD | CONTACT CELL : 99 42 511 522
  35. TNTET 2017 HALL TICKET DOWNLOAD
  36. KALVISOLAI MUTUAL TRANSFER ENTRY | VIEW
  37. TRB | TNTET | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD.
  38. TRB - TAMIL - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  39. TRB - ENGLISH - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  40. TRB - MATHEMATICS - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  41. TRB - PHYSICS - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  42. TRB - CHEMISTRY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  43. TRB - BOTANY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  44. TRB - ZOOLOGY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  45. TRB - HISTORY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  46. TRB - ECONOMICS - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  47. TRB - COMPUTER SCIENCE - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  48. TRB - COMMERCE - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  49. TRB - PHYSICAL EDUCATION DIRECTOR GRADE I - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  50. TRB - EDUCATION METHODOLOGY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  51. TRB - GEOGRAPHY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  52. TRB - POLITICAL SCIENCE - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  53. TRB - TELUGU - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  54. TRB - GENERAL KNOWLEDGE - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  55. TRB - MICRO BIOLOGY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  56. TRB - BIOCHEMISTRY - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  57. TRB - HOME SCIENCE - PGTRB - BTTRB - SYLLABUS - ORIGINAL GOVT QUESTION PAPERS - ANSWER KEYS - LATEST STUDY MATERIALS DOWNLOAD
  58. NEET (UG) 2017 PHYSICS-CHEMISTRY-BIOLOGY PAPER WITH ANSWER DOWNLOAD
  59. SSLC | TAMIL | TENTH | CLASS 10 | TAMIL | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  60. SSLC | OTHER LANGUAGE | TENTH | CLASS 10 | OTHER LANGUAGE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  61. SSLC | ENGLISH | TENTH | CLASS 10 | ENGLISH | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  62. SSLC | MATHS | TENTH | CLASS 10 | MATHS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  63. SSLC | SCIENCE | TENTH | CLASS 10 | SCIENCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  64. SSLC | SOCIAL SCIENCE | TENTH | CLASS 10 | SOCIAL SCIENCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD

  65. PLUS TWO | TAMIL | +2 | CLASS 12 | TAMIL | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  66. PLUS TWO | OTHER LANGUAGE | +2 | CLASS 12 | OTHER LANGUAGE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  67. PLUS TWO | ENGLISH | +2 | CLASS 12 | ENGLISH | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  68. PLUS TWO | +2 | CLASS 12 | MATHS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  69. PLUS TWO | +2 | CLASS 12 | PHYSICS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  70. PLUS TWO | CHEMISTRY | +2 | CLASS 12 | CHEMISTRY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  71. PLUS TWO | BIOLOGY | +2 | CLASS 12 | BIOLOGY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  72. PLUS TWO | BOTANY | +2 | CLASS 12 | BOTANY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  73. PLUS TWO | ZOOLOGY | +2 | CLASS 12 | ZOOLOGY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  74. PLUS TWO | HISTORY | +2 | CLASS 12 | HISTORY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  75. PLUS TWO | ECONOMICS | +2 | CLASS 12 | ECONOMICS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  76. PLUS TWO | COMMERCE | +2 | CLASS 12 | COMMERCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  77. PLUS TWO | ACCOUNTANCY | +2 | CLASS 12 | ACCOUNTANCY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  78. PLUS TWO | COMPUTER SCIENCE | +2 | CLASS 12 | COMPUTER SCIENCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  79. PLUS TWO | NURSING | +2 | CLASS 12 | NURSING | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  80. PLUS TWO | VOCATIONAL SUBJECTS | +2 | CLASS 12 | VOCATIONAL SUBJECTS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  81. PLUS TWO | GEOGRAPHY | +2 | CLASS 12 | GEOGRAPHY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  82. PLUS TWO | HOME SCIENCE | +2 | CLASS 12 | HOME SCIENCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  83. PLUS TWO | COMMUNICATIVE ENGLISH | +2 | CLASS 12 | COMMUNICATIVE ENGLISH | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  84. PLUS TWO | INDIAN CULTURE | +2 | CLASS 12 | INDIAN CULTURE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  85. PLUS TWO | STATISTICS | +2 | CLASS 12 | STATISTICS | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  86. PLUS TWO | BIO-CHEMISTRY | +2 | CLASS 12 | BIO-CHEMISTRY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  87. PLUS TWO | ADVANCED TAMIL | +2 | CLASS 12 | ADVANCED TAMIL | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  88. PLUS TWO | POLITICAL SCIENCE | +2 | CLASS 12 | POLITICAL SCIENCE | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  89. PLUS TWO | MICRO BIOLOGY | +2 | CLASS 12 | MICRO BIOLOGY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  90. PLUS TWO | NUTRITION AND DIETETICS | +2 | CLASS 12 | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  91. PLUS TWO | BUSINESS MATHS| +2 | CLASS 12 | BUSINESS MATHS| ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  92. MARCH-2017-SSLC(10TH)- HSC (12TH)-QP-ANSWER KEY DOWNLOAD
  93. SSLC | TENTH | CLASS 10 | PLUS TWO | +2 | CLASS 12 | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  94. PLUS TWO | +2 | CLASS 12 | BIOLOGY | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  95. SSLC | TENTH | 10TH | CLASS 10 | ENGLISH | ORIGINAL GOVT QUESTION PAPERS, ANSWER KEYS AND STUDY MATERIALS DOWNLOAD
  96. TNTET EXAM - 2017 | ஆசிரியர் தகுதித்தேர்வு 2017
  97. LAB ASST SELECTION LIST FOR COUNSELLING | ஆய்வக உதவியாளர் கலந்தாய்வு பட்டியல்
  98. KALVISOLAI R.H-2017 | கல்விச்சோலை RH 2017
  99. கல்விச்சோலை செய்தித் துளிகள்!
  100. விறு விறு செய்திகளுடன்...புதிய செய்தி
  101. SET EXAM - 2017 ANNOUNCED
  102. NEET EXAM - 2017 NEWS
  103. IT FORM VERSION 2017.3 DOWNLOAD
  104. Police Recruitment - 2017 | Common Recruitment for the posts of Gr II Police Constables, Gr II Jail Warders and Firemen Common Recruitment - 2017
  105. SSLC - PLUS TWO PUBLIC EXAM - MARCH 2017 - TIME TABLE DOWNLOAD.
  106. TNPSC GROUP 4 QP AND ANSWER KEY DOWNLOAD
  107. CLASS 10 | SSLC QUESTION PAPERS DOWNLOAD UPTO SEPTEMBER 2016
  108. CLASS 12 | +2 QUESTION PAPERS DOWNLOAD UPTO SEPTEMBER 2016
  109. TNPSC-TRB-ONLINE TEST MATERIALS
  110. ALL LATEST STUDY MATERIALS DOWMLOAD 2016-2017
  111. tnpsc group 4 model study materials,question paper with answers
  112. DSE | DGE | DEE | G.O | OTHER DOWNLOADS
  113. KALVISOLAI CONTACT 2016 -ENTER UR MOBILE & EMAIL ID
  114. Kalvisolai.Com - Today's Headlines!
  115. LATEST STUDY MATERIALS DOWNLOAD ...CLICK HERE...
  116. # CLASS 12 | SEPTEMBER 2016 | GOVT QUESTION PAPER DOWNLOAD | CLASS 12 | SEPTEMBER 2016 | 12TH | HSC | PLUS TWO | +2 | GOVT QUESTION PAPER DOWNLOAD.
  117. # CLASS 10 | SEPTEMBER 2016 | SSLC | GOVT QUESTION PAPER DOWNLOAD.
  118. # TNPSC GK - அரசுப் பணி தேர்வுகளுக்கான மாதிரி வினா-விடை
  119. # PLUS TWO SPECIAL GUIDE 2016-2017 | AMMA GUIDE 2017 | ENGLISH MEDIUM | பள்ளிக்கல்வித்துறை சார்பில் SCERT வெளியிட்டுள்ள பிளஸ் டூ மாணவர்களுக்கான குறைந்த பட்ச கற்றல் கையேடுகளை பதிவிறக்கம் செய்யுங்கள்...
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Sunday, December 5, 2010

Stephen W. Hawking - My Life in Physics

I did my first degree in Oxford. In my final examination, I was asked about my future plans. I replied, if you give me a first class degree, I will go to Cambridge. If I only get a second, I will stay in Oxford. They gave me a first. I arrived in Cambridge as a graduate student in October 1962. I had applied to work with Fred Hoyle, the principal defender of the steady state theory and the most famous British astronomer of the time. I say astronomer because cosmology was at that time, hardly recognized as a legitimate field, yet that was where I wanted to do my research, inspired by having been on a summer course with Hoyle's student, Jayant Narlikar. However, Hoyle had enough students already, so to my great disappointment, I was assigned to Dennis Sharma, of whom I had not heard. But it was probably for the best. Hoyle was away a lot, seldom in the department, and I wouldn't have had much of his attention. Sharma, on the other hand, was usually around and ready to talk. I didn't agree with many of his ideas, particularly on Mach's principle, but that stimulated me to develop my own picture.

When I began research, the two areas that seemed exciting were cosmology and elementary particle physics. Elementary particles was the active, rapidly changing field that attracted most of the best minds, while cosmology and general relativity were stuck where they had been in the 1930s. Feynman has given an amusing account of attending the conference on general relativity and gravitation in Warsaw in 1962. In a letter to his wife, he said, “I am not getting anything out of the meeting. I am learning nothing. Because there are no experiments, this field is not an active one, so few of the best men are doing work in it. The result is that there are hosts of dopes here (126) and it is not good for my blood pressure. Remind me not to come to any more gravity conferences!”

Of course, I wasn't aware of all this when I began my research. But I felt that elementary particles at that time, was too like botany. Quantum electro dynamics, the theory of light and electrons that governs chemistry and the structure of atoms, had been worked out completely in the 40s and 50s. Attention had now shifted to the weak and strong nuclear forces between particles in the nucleus of an atom, but similar field theories didn't seem to work. Indeed, the Cambridge school, in particular, held that there was no underlying field theory. Instead, everything would be determined by unitarity, that is, probability conservation, and certain characteristic patterns in the scattering. With hind sight, it now seems amazing that it was thought this approach would work, but I remember the scorn that was poured on the first attempts at unified field theories of the weak nuclear forces. Yet it is these field theories that are remembered and the analytic S matrix work is forgotten. I'm very glad I didn't start my research in elementary particles. None of my work from that period would have survived.

Cosmology and gravitation, on the other hand, were neglected fields that were ripe for development at that time. Unlike elementary particles, there was a well defined theory, the general theory of relativity, but this was thought to be impossibly difficult. People were so pleased to find any solution of the field equations, they didn't ask what physical significance, if any, it had. This was the old school of general relativity that Feynman encountered in Warsaw. But the Warsaw conference also marked the beginning of the renaissance of general relativity, though Feynman could be forgiven for not recognizing it at the time.

A new generation entered the field and new centers of general relativity appeared. Two of these were of particular importance to me. One was in Hamburg under Pascal Jordan. I never visited it, but I admired their elegant papers which were such a contrast to the previous messy work on general relativity. The other center was at Kings College, London, under Hermann Bondi, another proponent of the steady state theory but not ideologically committed to it, like Hoyle.

I hadn't done much mathematics at school or in the very easy physics course at Oxford, so Sharma suggested I work on astrophysics. But having been cheated out of working with Hoyle, I wasn't going to do something boring like Faraday rotation. I had come to Cambridge to do cosmology, and cosmology I was determined to do. So I read old text books on general relativity and traveled up to lectures at Kings College, London each week with three other students of Sharma. I followed the words and equations, but I didn't really get a feel for the subject. Also, I had been diagnosed with motor neurone disease, or ALS, and given to expect I didn't have long enough to finish my PhD. Then suddenly, towards the end of my second year of research, things picked up. My disease wasn't progressing much and my work all fell into place, and I began to get somewhere.

Sharma was very keen on Mach's principle, the idea that objects owe their inertia to the influence of all the other matter in the universe. He tried to get me to work on this, but I felt his formulations of Mach's principle were not well defined. However, he introduced me to something a bit similar with regard to light, the so called Wheeler Feynman electro dynamics. This said that electricity and magnetism were time symmetric. However, when one switched on a lamp, it was the influence of all the other matter in the universe that caused light waves to travel outward from the lamp, rather than come in from infinity and end on the lamp. For Wheeler Feynman electro dynamics to work, it was necessary that all the light traveling out from the lamp should be absorbed by other matter in the universe. This would happen in a steady state universe in which the density of matter would remain constant, but not in a big bang universe where the density would go down as the universe expanded. It was claimed that this was another proof, if proof were needed, that we live in a steady state universe. There was a conference on Wheeler Feynman electro dynamics and the arrow of time in Cornell in 1963. Feynman was so disgusted by the nonsense that was talked about the arrow of time that he refused to let his name appear in the proceedings. He was referred to as Mr. X, but everyone knew who X was.
I found that Hoyle and Narlikar had already worked out Wheeler Feynman electro dynamics in expanding universes and had then gone on to formulate a time symmetric new theory of gravity. Hoyle unveiled the theory at a meeting of the royal society in 1964. I was at the lecture, and in the question period, I said that the influence of all the matter in a steady state universe would make his masses infinite. Hoyle asked why I said that, and I replied that I had calculated it. Everyone thought I had done it in my head during the lecture, but in fact, I was sharing an office with Narlikar and had seen a draft of the paper. Hoyle was furious. He was trying to set up his own institute, and threatening to join the brain drain to America if he didn't get the money. He thought I had been put up to it, to sabotage his plans. However, he got his institute and later gave me a job, so he didn't harbor a grudge against me.

The big question in cosmology in the early 60s, was did the universe have a beginning? Many scientists were instinctively opposed to the idea, because they felt that a point of creation would be a place where science broke down. One would have to appeal to religion and the hand of God to determine how the universe would start off. Two alternative scenarios were therefore put forward. One was the steady state theory, in which as the universe expanded, new matter was continually created to keep the density constant on average. The steady state theory was never on a very strong theoretical basis because it required a negative energy field to create the matter. This would have made it unstable, to run away production of matter and negative energy. But it had the great merit as a scientific theory of making definite predictions that could be tested by observations. By 1963, the steady state theory was already in trouble. Martin Ryle's radio astronomy group at the Cavendish did a survey of faint radio sources. They found the sources were distributed fairly uniformly across the sky. This indicated that they were probably outside our galaxy because otherwise, they would be concentrated along the Milky Way. But the graph of the number of sources against source strength did not agree with the prediction of the steady state theory. There were too many faint sources indicating that the density of sources was higher in the distant past. Hoyle and his supporters put forward increasingly contrived explanations of the observations, but the final nail in the coffin of the steady state theory came in 1965 with the discovery of a faint background of microwave radiation. This could not be accounted for in the steady state theory, though Hoyle and Narlikar tried desperately. It was just as well I hadn't been a student of Hoyle, because I would have had to have defended the steady state.

The microwave background indicated that the universe had had a hot dense stage in the past. But it didn't prove that was the beginning of the universe. One might imagine that the universe had had a previous contracting phase, and that it had bounced from contraction to expansion at a high, but finite density. This was clearly a fundamental question, and it was just what I needed to complete my PhD thesis.

Gravity pulls matter together, but rotation throws it apart. So my first question was, could rotation cause the universe to bounce? Together with George Ellis, I was able to show that the answer was no, if the universe was spatially homogeneous, that is, if it was the same at each point of space. However, two Russians, Lifshitz and Khalatnikov, had claimed to have proved that a general contraction without exact symmetry would always lead to a bounce, with the density remaining finite. This result was very convenient for Marxist Leninist dialectical materialism, because it avoided awkward questions about the creation of the universe. It therefore became an article of faith for Soviet scientists.

Lifshitz and Khalatnikov were members of the old school in general relativity. That is, they wrote down a massive system of equations and tried to guess a solution. But it wasn't clear that the solution they found was the most general one. However, Roger Penrose introduced a new approach which didn't require solving the field equations explicitly, just certain general properties such as that energy is positive and gravity is attractive. Penrose gave a seminar in Kings College, London, in January 1965. I wasn't at the seminar, but I heard about it from Brandon Carter, with whom I shared an office in the then new DAMTP premises in Silver Street. At first, I couldn't understand what the point was. Penrose had showed that once a dying star had contracted to a certain radius, there would inevitably be a singularity, a point where space and time came to an end. Surely, I thought, we already knew that nothing could prevent a massive cold star collapsing under its own gravity until it reached a singularity of infinite density. But in fact, the equations had been solved, only for the collapse of a perfectly spherical star. Of course, a real star won't be exactly spherical. If Lifshitz and Kalatnikov were right, the departures from spherical symmetry would grow as the star collapsed and would cause different parts of the star to miss each other and avoid a singularity of infinite density. But Penrose showed they were wrong. Small departures from spherical symmetry will not prevent a singularity.

I realized that similar arguments could be applied to the expansion of the universe. In this case, I could prove there were singularities where spacetime had a beginning. So again, Lifshitz and Khalatnikov were wrong. General relativity predicted that the universe should have a beginning, a result that did not pass unnoticed by the Church.

The original singularity theorems of both Penrose and myself, required the assumption that the universe had a Cauchy surface, that is, a surface that intersects every time like curve once, and only once. It was therefore possible that our first singularity theorems just proved that the universe didn't have a Cauchy surface. While interesting, this didn't compare in importance with time having a beginning or end. I therefore set about proving singularity theorems that didn't require the assumption of a Cauchy surface. In the next five years, Roger Penrose, Bob Geroch and I developed the theory of causal structure in general relativity. It was a glorious feeling, having a whole field virtually to ourselves. How unlike particle physics, where people were falling over themselves to latch onto the latest idea. They still are.
Up to 1970, my main interest was in the big bang singularity of cosmology, rather than the singularities that Penrose had shown would occur in collapsing stars. However, in 1967, Werner Israel produced an important result. He showed that unless the remnant from a collapsing star was exactly spherical, the singularity it contained would be naked, that is, it would be visible to outside observers. This would have meant that the break down of general relativity at the singularity of a collapsing star would destroy our ability to predict the future of the rest of the universe.

At first, most people, including Israel himself, thought that this implied that because real stars aren't spherical, their collapse would give rise to naked singularities and break down of predictability. However, a different interpretation was put forward by Roger Penrose and John Wheeler. It was that there is Cosmic Censorship. This says that Nature is a prude and hides singularities in black holes where they can't be seen. I used to have a bumper sticker, black holes are out of sight, on the door of my office in DAMTP. This so irritated the head of department, that he engineered my election to the Lucasian professorship, moved me to a better office on the strength of it, and personally tore off the offending notice from the old office.

My work on black holes began with a Eureka moment in 1970, a few days after the birth of my daughter, Lucy. While getting into bed, I realized that I could apply to black holes, the causal structure theory I had developed for singularity theorems. In particular, the area of the horizon, the boundary of the black hole, would always increase. When two black holes collide and merge, the area of the final black hole is greater than the sum of the areas of the original holes. This and other properties that Jim Bardeen, Brandon Carter and I discovered, suggested that the area was like the entropy of a black hole. This would be a measure of how many states a black hole could have on the inside, for the same appearance on the outside. But the area couldn't actually be the entropy, because as everyone knew, black holes were completely black and couldn't be in equilibrium with thermal radiation.

There was an exciting period culminating in the Les Houches summer school in 1972, in which we solved most of the major problems in black hole theory. This was before there was any observational evidence for black holes, which shows Feynman was wrong when he said an active field has to be experimentally driven. Just as well for M theory. The one problem that was never solved was to prove the Cosmic Censorship hypothesis, though a number of attempts to disprove it, failed. It is fundamental to all work on black holes, so I have a strong vested interest in it being true. I therefore have a bet with Kip Thorne and John Preskill. It is difficult for me to win this bet, but quite possible to lose, by finding a counter example with a naked singularity. In fact, I have already lost an earlier version of the bet by not being careful enough about the wording. They were not amused by the t-shirt I offered in settlement.

We were so successful with the classical general theory of relativity that I was at a bit of a loose end in 1973 after the publication with George Ellis, of The Large Scale Structure of Spacetime. My work with Penrose had shown that general relativity broke down at singularities. So the obvious next step would be to combine general relativity, the theory of the very large, with quantum theory, the theory of the very small. I had no background in quantum theory, and the singularity problem seemed too difficult for a frontal assault at that time. So as a warm up exercise, I considered how particles and fields governed by quantum theory would behave near a black hole. In particular, I wondered, can one have atoms in which the nucleus is a tiny primordial black hole, formed in the early universe?

To answer this, I studied how quantum fields would scatter off a black hole. I was expecting that part of an incident wave would be absorbed, and the remainder, scattered. But to my great surprise, I found there seemed to be emission from the black hole. At first, I thought this must be a mistake in my calculation. But what persuaded me that it was real, was that the emission was exactly what was required to identify the area of the horizon with the entropy of a black hole. I would like this simple formula to be on my tomb stone.

Work with Jim Hartle, Gary Gibbons, and Malcolm Perry uncovered the deep reason for this formula. General relativity can be combined with quantum theory in an elegant manner, if one replaces ordinary time, by imaginary time. I have tried to explain imaginary time on other occasion with varying degrees of success. I think it is the name, imaginary, that makes it so confusing. It is easier if you accept the positivist view that a theory is just a mathematical model. In this case, the mathematical model has a minus sign whenever time appears twice. The Euclidean approach to quantum gravity, based on imaginary time, was pioneered in Cambridge. It met a lot of resistance, but is now generally accepted.

The Radiation from a black hole will carry away energy, so the black hole will lose mass, and shrink. Eventually, it seems the black hole will evaporate completely and disappear. This raised a problem that struck at the heart of physics. My calculation showed that the radiation was exactly thermal and random, as it has to be, if the area of the horizon is to be the entropy of the black hole. So how could the radiation left over carry all the information about what made the black hole? But if information is lost, this is incompatible with quantum mechanics. This paradox had been argued for thirty years without much progress, until I found what I think is its resolution. Information is not lost, but it is not returned in a useful way. It is like burning an encyclopedia. Information is not lost, but it is very hard to read. In fact, Kip Thorne and I had a bet with John Preskill on the information paradox. I gave John a baseball encyclopedia. Maybe I should have just given him the ashes.

Between 1970 and 1980, I worked mainly on black holes and the Euclidean approach to quantum gravity. But the suggestions that the early universe had gone through a period of inflationary expansion, renewed my interest in cosmology. Euclidean methods were the obvious way to describe fluctuations and phase transitions in an inflationary universe. We held a Nuffield work shop in Cambridge in 1982, attended by all the major players in the field. At this meeting, we established most of our present picture of inflation, including the all important density fluctuations which give rise to galaxy formation and so to our existence. This was ten years before fluctuations in the microwave were observed, so again in gravity, theory was ahead of experiment.

The scenario for inflation in 1982 was that the universe began with a big bang singularity. As the universe expanded, it was supposed somehow to get into an inflationary state. I thought this was unsatisfactory because all equations would break down at a singularity. But unless one knew what came out of the initial singularity, one could not calculate how the universe would develop. Cosmology would not have any predictive power.

After the work shop in Cambridge, I spent the summer at the Institute of Theoretical Physics, Santa Barbara, which had just been set up. We stayed in student houses and I drove in to the institute in a rented electric wheel chair. I remember my younger son, Tim aged three, watching the Sun set on the mountains, and saying, it's a big country.

While in Santa Barbara, I talked to Jim Hartle about how to apply the Euclidean approach to cosmology. According to Dewitt and others, the universe should be described by a wave function that obeyed the Wheeler Dewitt equation. But what picked out the particular solution of the equation that represents our universe. According to the Euclidean approach, the wave function of the universe is given by a Feynman sum over a certain class of histories in imaginary time. Because imaginary time behaves like another direction in space, histories in imaginary time can be closed surfaces, like the surface of the Earth, with no beginning or end. Jim and I decided that this was the most natural choice of class, indeed the only natural choice. We had side stepped the scientific and philosophical difficulty of time beginning by turning it into a direction in space.

Most people in theoretical physics have been trained in particle physics rather than general relativity. They have therefore been more interested in calculations of what they observe in particle accelerators than in questions about the beginning and end of time. The feeling was that if they could find a theory that in principle, allowed them to calculate particle scattering to arbitrary accuracy, everything else would somehow follow. In 1985, it was claimed that string theory was this ultimate theory. But in the years that followed, it emerged that the situation was more complicated and more interesting. It seems that there's a network called M theory. All the theories in the M theory network can be regarded as approximations to the same underlying theory, in different limits. None of the theories allow calculation of scattering to arbitrary accuracy, and none can be regarded as the fundamental theory of which others are reflections. Instead, they should all be regarded as effective theories, valid in different limits. String theorists have long used the term, effective theory, as a pejorative description of general relativity. However, string theory is equally an effective theory, valid in the limit that the M theory membrane is rolled into a cylinder of small radius. Saying that string theory is only an effective theory isn't very popular, but it's true.

Because they had the dream of a theory that would allow calculation of scattering to arbitrary accuracy, people rejected quantum general relativity and supergravity on the grounds that they were non renormalizable. This means that one needs undetermined subtractions at each order to get finite answers. In fact, it is not surprising that naïve perturbation theory breaks down in quantum gravity. One can not regard a black hole as a perturbation of flat space.

I have done some work recently on making supergravity renormalizable, by adding higher derivative terms to the action. This apparently introduces ghosts, states with negative probability. However, I have found this is an illusion. One can never prepare a system in a state of negative probability. But the presence of ghosts means that one can not predict with arbitrary accuracy. If one can accept that, one can live quite happily with ghosts.

This approach to higher derivatives and ghosts allows one to revive the original inflation model of Starobinski and other Russians. In this, the inflationary expansion of the universe is driven by the quantum effects of a large number of matter fields. Based on the no boundary proposal, I picture the origin of the universe as like the formation of bubbles of steam in boiling water. Quantum fluctuations lead to the spontaneous creation of tiny universes, out of nothing. Most of the universes collapse to nothing, but a few that reach a critical size will expand in an inflationary manner and will form galaxies and stars, and maybe beings like us.

It has been a glorious time to be alive and doing research in theoretical physics. Our picture of the universe has changed a great deal in the last 40 years, and I'm happy if I have made a small contribution. I want to share my excitement and enthusiasm. There's nothing like the Eureka moment of discovering something that no one knew before. I won't compare it to sex, but it lasts longer.

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