“[A] wonderful book about Stephen Hawking's Hawking’s ‘biggest legacy’.”―Spectator
“Truly mind-stretching . . . Immensely immensely rewarding.”―The Times
“Why is our universe the way it is? How did everything begin? How might it end? Thomas Hertog probed these overwhelming questions in collaboration with Stephen Hawking, achieving a privileged perspective into how, struggling against daunting physical odds, Hawking’s imprisoned mind yielded astonishing insights even in his later years. This superbly written book offers insight into an extraordinary individual, the creative process generally, and the scope and limits of our current understanding of the cosmos.”―Lord Martin Rees, Emeritus Professor of Cosmology and Astrophysics, University of Cambridge, and author of Just Six Numbers
“Like his mentor and colleague Stephen Hawking, Thomas Hertog has never shied away from being ambitious in theorizing about the universe. This sweeping book provides an accessible overview of both what we know about cosmology and some audacious ideas for moving into the unknown. It is an introduction to Hawking’s final theory, but also a glimpse into even grander theories yet to come.”―Sean Carroll, author of The Biggest Ideas in the Universe: Space, Time, and Motion
“Stephen Hawking’s final theory is lucidly explained in this splendidly accessible book. Author Thomas Hertog, one of Hawking’s closest collaborators, gives us a vivid insight into Hawking as both a brilliant physicist and an astonishingly determined human being.”―Graham Farmelo, Churchill College, University of Cambridge, and author of The Strangest Man
“A beautifully written, thought-provoking account of both the physics and the personalities involved in Hawking’s visionary struggle to comprehend the cosmos. Thomas Hertog has provided a fascinating insider’s view.”―Neil Turok, co-author of Endless Universe
Contents
Preface
I. Hesitations
II. History and the Earth
III. Biology and History
IV. Race and History
V. Character and History
VI. Morals and History
VII. Religion and History
VIII. Economics and History
IX. Socialism and History
X. Government and History
XI. History and War
XII. Growth and Decay
XIII. Is Progress Real?
Bibliographical Guide
Notes
Index
Chapter 1
A Paradox
Es konnte sich eine seltsame Analogie ergeben, daß das Okular auch des riesigsten Fernrohrs nicht großer sein darf, als unser Auge.
A curious correlation may emerge in that the eyepiece of even the biggest telescope cannot be larger than the human eye.
―Ludwig Wittgenstein, Vermischte Bemerkungen
The late 1990s were the culmination of a golden decade of discovery in cosmology. Long regarded as a realm of unrestrained speculation, cosmology―the science that dares to study the origin, evolution, and fate of the universe as a whole―was finally coming of age. Scientists all over the world were buzzing with excitement about spectacular observations from sophisticated satellites and Earth-based instruments that were transforming our picture of the universe beyond recognition. It was as if the universe was speaking to us. These developments posed quite a reality check for theoreticians, who were told to rein in their speculation and flesh out the predictions of their models.
In cosmology we discover the past. Cosmologists are time travelers, and telescopes their time machines. When we look into deep space we look back into deep time, because the light from distant stars and galaxies has traveled millions or even billions of years to reach us. Already in 1927 the Belgian priest-astronomer Georges Lemaitre predicted that space, when considered over such long periods of time, expands. But it wasn’t until the 1990s that advanced telescope technology made it possible to trace the universe’s history of expansion.
This history held some surprises. For example, in 1998 astronomers discovered that the stretching of space had begun to speed up around five billion years ago, even though all known forms of matter attract and should therefore slow down the expansion. Since then, physicists have wondered whether this weird cosmic acceleration is driven by Einstein’s cosmological constant, an invisible ether-like dark energy that causes gravity to repel rather than to attract. One astronomer quipped that the universe looks like Los Angeles: one-third substance and two-thirds energy.
Obviously, if the universe is expanding now, it must have been more compressed in the past. If you run cosmic history backward―as a mathematical exercise, of course―you find that all matter would once have been very densely packed together and also very hot, since matter heats up and radiates when it is squeezed together. This primeval state is known as the hot big bang. Astronomical observations since the golden 1990s have pinned down the age of the universe―the time elapsed since the big bang―to 13.8 billion years, give or take 20 million.
Curious to learn more about the universe’s birth, the European Space Agency (ESA) launched a satellite in May 2009 in a bid to complete the most detailed and ambitious scanning of the night sky ever undertaken. The target was an intriguing pattern of flickers in the heat radiation left over from the big bang. Having travele...d through the expanding cosmos for 13.8 billion years, the heat from the universe’s birth reaching us today is cold: 2.725 K, or about ？270 degrees Celsius. Radiation at this temperature lies mainly in the microwave band of the electromagnetic spectrum, so the remnant heat is known as the cosmic microwave background radiation, or CMB radiation.
ESA’s efforts to capture the ancient heat culminated in 2013 when a curious speckled image resembling a pointillist painting decorated the front pages of the world’s newspapers. This image is reproduced in figure 2, which shows a projection of the entire sky, compiled in exquisite detail from millions of pixels representing the temperature of the relic CMB radiation in different directions in space. Such detailed observations of the CMB radiation provide a snapshot of what the universe was like a mere 380,000 years after the big bang, when it had cooled to a few thousand degrees, cold enough to liberate the primeval radiation, which has traveled unhindered through the cosmos ever since.
The CMB sky map confirms that the relic big bang heat is nearly uniformly distributed throughout space, although not quite perfectly. The speckles in the image represent minuscule temperature variations indeed, tiny flickers of no more than a hundred-thousandth of a degree. These slight variations, however small, are crucially important, because they trace the seeds around which galaxies would eventually form. Had the hot big bang been perfectly uniform everywhere, there would be no galaxies today.
The ancient CMB snapshot marks our cosmological horizon: We cannot look back any farther. But we can glean something about processes operating in yet earlier epochs from cosmological theory. Just as paleontologists learn from stone fossils what life on Earth used to be like, cosmologists can, by deciphering the patterns encoded in these fossil flickers, stitch together what might have happened before the relic heat map was imprinted on the sky. This turns the CMB into a cosmological Rosetta Stone that enables us to trace the universe’s history even farther back, perhaps as far back as a fraction of a second after its birth.
And what we learn is intriguing. As we will see in chapter 4, the temperature variations of the CMB radiation indicate that the universe initially expanded fast, then slowed down, and, more recently (about five billion years ago), began accelerating again. Slowing down appears to be the exception rather than the rule on the scales of deep time and deep space. This is one of those seemingly fortuitous biofriendly properties of the universe, for only in a slowing universe does matter aggregate and cluster to form galaxies. If it hadn’t been for the extended near-pause in expansion in our past, there would, again, be no galaxies and no stars, and thus no life.
In effect, the universe’s expansion history was at the center of one of the very first moments in which the conditions for our existence slipped into modern cosmological thinking. This moment occurred in the early 1930s, when Lemaitre made a remarkable sketch in one of his purple notebooks of what he called a “hesitating” universe, one with an expansion history much like the bumpy ride that would emerge from observations seventy years later (see insert, plate 3). Lemaitre embraced the idea of a long pause in the expansion by considering the universe’s habitability. He knew that astronomical observations of nearby galaxies pointed to a high expansion rate in recent times. But when he ran the evolution of the universe backward in time at this same rate, he found that the galaxies must all have been on top of one another no more than a billion years ago. This was impossible, of course, for Earth and the sun are much older than that. To avoid an obvious conflict between the history of the universe and that of our solar system, he imagined an intermediate era of very slow expansion, to give stars, planets, and life time to develop.
In the decades since Lemaitre’s pioneering work, physicists have continued to stumble across many more such “happy coincidences.” Make but a small change in almost any of its basic physical properties, from the behavior of atoms and molecules to the structure of the cosmos on the largest scales, and the universe’s habitability would hang in the balance.
Take gravity, the force that sculpts and governs the large-scale universe. Gravity is extremely weak; it requires the mass of Earth just to keep our feet on the ground. But if gravity were stronger, stars would shine more brightly and hence die far younger, leaving no time for complex life to evolve on any of the orbiting planets warmed by their heat.
Or consider the tiny variations, one part in a hundred thousand, in the temperature of the relic big bang radiation. Were these differences slightly larger―say one part in ten thousand―the seeds of cosmic structures would have mostly grown into giant black holes instead of hospitable galaxie
Hertog, Thomas [저]
스티븐 호킹의 공동 연구자이자 빅뱅의 양자적 특성을 연구하는 우주론학자. 케임브리지대학교에서 세계적인 물리학자 스티븐 호킹의 지도하에 박사학위를 받았으며, 이때의 인연을 시작으로 2018년 호킹이 세상을 떠나기 전까지 20년 동안 호킹과 함께 우주의 기원을 파헤치는 연구를 해나갔다. 케임브리지대학교 이론물리학과 연구실에서 몇 년에 걸쳐 우주가 어떻게 생명체에 유리한 환경을 갖게 되었는지 파고든 끝에, 양자물리학의 극단을 탐험, 물리법칙이 우주와 함께 진화해왔다는 결론에 도달하게 된다. 현재는 벨기에 루뱅가톨릭대학교 이론물리학과에서 학생들을 가르치고 있다.
전체 0개의 구매후기가 있습니다.
인터파크도서는 고객님의 단순 변심에 의한 교환과 반품에 드는 비용은 고객님이 지불케 됩니다.
단, 상품이나 서비스 자체의 하자로 인한 교환 및 반품은 무료로 반품 됩니다.
교환 및 반품이 가능한 경우
상품을 공급 받은 날로부터 7일이내 가능 공급받으신 상품의 내용이 표시, 광고 내용과 다르거나 다르게 이행된 경우에는 공급받은 날로부터 3개월 이내, 혹은 그사실을 알게 된 날 또는 알 수 있었던 날로부터 30일 이내 상품에 아무런 하자가 없는 경우 소비자의 고객변심에 의한 교환은 상품의 포장상태 등이 전혀 손상되지 않은 경우에 한하여 가능
교환 및 반품이 불가능한 경우
구매확정 이후(오픈마켓상품에 한함) 고객님의 책임 있는 사유로 상품 등이 멸실 또는 훼손된 경우
(단, 상품의 내용을 확인하기 위하여 포장 등을 훼손한 경우는 제외) 시간이 지남에 따라 재판매가 곤란할 정도로 물품의 가치가 떨어진 경우 포장 개봉되어 상품 가치가 훼손된 경우
다배송지의 경우 반품 환불
다배송지의 경우 다른 지역의 반품을 동시에 진행할 수 없습니다. 1개 지역의 반품이 완료된 후 다른 지역 반품을 진행할 수 있으므로, 이점 양해해 주시기 바랍니다.
중고상품의 교환
중고상품은 제한된 재고 내에서 판매가 이루어지므로, 교환은 불가능합니다.
오픈마켓 상품의 환불
오픈마켓상품에 대한 책임은 원칙적으로 업체에게 있으므로, 교환/반품 접수시 반드시 판매자와 협의 후 반품 접수를 하셔야하며, 반품접수 없이 반송하거나, 우편으로 보낼 경우 상품 확인이 어려워 환불이 불가능할 수 있으니 유의하시기 바랍니다.
배송예정일 안내
인터파크 도서는 모든 상품에 대해 배송완료예정일을 웹사이트에 표시하고 있습니다.
<인터파크 직배송 상품>
상품은 월~토요일 오전 10시 이전 주문분에 대하여 당일 출고/당일 배송완료를 보장하는 상품입니다.
상품은 서울지역/평일 주문분은 당일 출고/익일 배송완료를 보장하며, 서울외지역/평일 주문분의 경우는 오후 6시까지 주문분에 대하여 익일 배송완료를 보장하는 상품입니다. (단, 월요일은 12시까지 주문에 한함)
상품은, 입고예정일(제품출시일)+택배사배송일(1일)에 배송완료를 보장합니다.
~
상품은 유통특성상 인터파크에서 재고를 보유하지 않은 상품으로 주문일+기준출고일+택배사배송일(1일)에 배송완료를 보장합니다.(토/공휴일은 배송기간에 포함되지 않습니다.) ※기준출고일:인터파크가 상품을 수급하여 물류창고에서 포장/출고하기까지 소요되는 시간
<업체 직접배송/오픈마켓 상품>
~
상품은 업체가 주문을 확인하고, 출고하기까지 걸리는 시간입니다. 주문일+기준출고일+택배사배송일(2일)에 배송완료를 보장합니다.(토/공휴일은 배송기간에 포함되지 않습니다.) ※5일이내 출고가 시작되지 않을시, 오픈마켓 상품은 자동으로 주문이 취소되며, 고객님께 품절보상금을 지급해 드립니다.
배송비 안내
도서(중고도서 포함)만 구매하시면 : 배송비 2,000원 (1만원이상 구매 시 무료배송) 음반/DVD만 구매하시면 : 배송비 1,500원 (2만원이상 구매 시 무료배송) 잡지/만화/기프트만 구매하시면 : 배송비 2,000원 (2만원이상 구매 시 무료배송) 도서와 음반/DVD를 함께 구매하시면 : 배송비 1,500원 1만원이상 구매 시 무료배송) 도서와 잡지/만화/기프트/중고직배송상품을 함께 구매하시면 : 2,000원 (1만원이상 구매 시 무료배송) 업체직접배송상품을 구매시 : 업체별로 상이한 배송비 적용
* 세트상품의 경우 부분취소 시 추가 배송비가 부과될 수 있습니다.
* 북카트에서 배송비없애기 버튼을 클릭하셔서, 동일업체상품을 조금 더 구매하시면, 배송비를 절약하실 수 있습니다.
해외배송 안내
인터파크도서에서는 국내에서 주문하시거나 해외에서 주문하여 해외로 배송을 원하실 경우 DHL과 특약으로 책정된 요금표에
의해 개인이 이용하는 경우보다 배송요금을 크게 낮추며 DHL(www.dhl.co.kr)로 해외배송 서비스를 제공합니다. 해외배송은 도서/CD/DVD 상품에 한해 서비스하고 있으며, 다른 상품을 북카트에 함께 담으실 경우 해외배송이 불가합니다.
해외주문배송 서비스는 인터파크 도서 회원 가입을 하셔야만 신청 가능합니다.
알아두세요!!!
도매상 및 제작사 사정에 따라 품절/절판 등의 사유로 취소될 수 있습니다. 오픈마켓업체의 배송지연시 주문이 자동으로 취소될 수 있습니다. 출고가능 시간이 서로 다른 상품을 함께 주문할 경우 출고가능 시간이 가장 긴 기준으로 배송됩니다. 유통의 특성상 출고기간은 예정보다 앞당겨지거나 늦춰질 수 있습니다. 택배사 배송일인 서울 및 수도권은 1~2일, 지방은 2~3일, 도서, 산간, 군부대는 3일 이상의 시간이 소요됩니다.
;)
전체 0개의 구매후기가 있습니다.
교환 및 반품이 가능한 경우 
상품을 공급 받은 날로부터 7일이내 가능 
상품은 월~토요일 오전 10시 이전 주문분에 대하여 당일 출고/당일 배송완료를 보장하는 상품입니다.
상품은 서울지역/평일 주문분은 당일 출고/익일 배송완료를 보장하며,
상품은, 입고예정일(제품출시일)+택배사배송일(1일)에 배송완료를 보장합니다.
~ 
상품은 유통특성상 인터파크에서 재고를 보유하지 않은 상품으로
상품은 업체가 주문을 확인하고, 출고하기까지 걸리는 시간입니다.
