Alam Semesta Mengembang

Pengembangan Alam Semesta

Astronom Belanda  Willem de Sitter sekitar 1898.

Teori tentang Alam Semesta Statik Belum pernah terjadi di dalam sejarah Sains di mana ada satu periode ketika teori-teori serta hipotesis-hipotesis baru muncul, berkembang, dan segera ditinggalkan dalam waktu begitu singkat sebagaimana telah ditunjukkan 15an atau 20an tahun terakhir ini.                                      —Willem de Sitter, 1931 Kilas balik masa-masa penuh penemuan dan kehebohan Antara tahun 1915 dan 1930, Astronom Belanda Willem de Sitter secara benar telah dengan tepat mengidentifikasi masa masa tersebut sebagai masa paling luarbiasa bagi Ilmuwan Kealaman. Dalam teori relativitas dan kuantum, yang dipelopori oleh Albert Einstein para Fisikawan telah memberikan sebuah penjelasan sama sekali baru bagi konsep energi, materi, gravitasi bahkan ruang dan waktu. Ketika para astronom mencoba untuk menerapkan perangkat-perangkat teoretis baru ini pada kajian kosmologi, mereka terkejut dengan hasil penjelajahan mereka ini.  Konsep dari Harlow Shapley tentang Galaksi besar  (Harlow Shapley's concept of the Big Galaxy) dengan cepat disusul oleh temuan Edwin Hubble tentang bukti bagi adanya pulau-pulau alam semesta (Edwin Hubble's proof of the existence of island universes.) Meskipun terasa tidak lazim, akhirnya dipenghujung tahun 1920an disadari bahwa alam semesta benar-benar mengembang. Penerimaan ini dicapai setelah melewati rangkaian pertarungan kandidat teori yang menjelaskan alam semesta. Di awal abad 20 pandangan umum yang berlaku adalah bahwa alam semesta pada dasarnya bersifat statik—di mana alam semesta dianggap lebih kurang tetap sama dalam perjalanannya mengarungi keabadian.  Einstein mengungkapkan pendapat umum di tahun 1917 sesudah de Sitter mengeluarkan persamaannya yang mampu menggambarkan sebuah alam semesta yang mengembang, yang berimplikasi alam semesta juga mempunyai awal mula. Einstein di kala itu menulis, "situasi ini benar-benar menjengkelkan." Di surat lainnya Einstein menambahkan " untuk menerima kemungkinan seperti ini benar-benar tidaklah masuk akal." Dalam persamaan medannya bagi gravitasi, Einstein telah memberikan sebuah perangkat matematis kompak yang dapat menggambarkan konfigurasi umum materi dan ruang yang membentuk alam semesta secara keseluruhan. Kelengkungan ruang waktu yang cukup aneh sebagaimana diprediksi oleh teori tersebut, segeralah di uji oleh eksperimen, dan di awal 1920an sebagian besar ilmuwan terkemuka mengakui bahwa persamaan medan Einstein dapat menjadi fondasi bagi kosmologi. Tinggal persoalannya menemukan solusi bagi persamaan sederhana tersebut--yang menghasilkan sebuah model bagi alam semesta--yang terbukti merupakan sebuah mimpi buruk matematis karena cukup sulit dipecahkan. Saya membayangkan diri saya telah membangun kastil yang megah di udara,......Marilah kita puas begitu saja dan tidak mengharapkan sebuah jawaban, dan agaknya lebih senang sesegera mungkin saling melihat satu sama lain kembali – Einstein kepada de Sitter, 1916 [full quote]

EXIT to read more about Einstein's general theory and the observations that made it famous

Albert Einstein (kiri) dan Willem de Sitter (kanan) mendiskusikan di papan tulis teori de Sitter tentang pengembangan alam semesta. Gambar ini diambil pada  1932 Institut Teknologi Kalifornia. Selama tahun 1916, di pertengahan Perang Dunia 1,Einstein berjumpa dengan de Sitter di Belanda yang merupakan zona netral perang masa itu. Saling merangsang dan mengkritisi pemikiran masing-masing, mereka menelorkan dua model kosmologis, dua solusi yang berbeda bagi persamaan medan Einstein Relativitas Umum. Namun kedua model tampaknya membutuhkan sentuhan khusus. Model De Sitter hanya stabil jika tidak mengandung materi. De Sitter berharap model tersebut bagaimanapun juga dapat disempurnakan untuk menggambarkan alam semesta sesungguhnya, asalkan kerapatan materi mendekati nol. Yang paling mengejutkan tentang alam semesta kosong ini adalah efek ganjil dari cahaya — makin jauh dari pusat matematis  (asal koordinat), makin lambat frekuensi cahaya. That meant that the farther away an object was in this odd universe, the more the light coming from it would seem to have a slowed-down frequency. Einstein's first try at a model likewise could not contain matter and be stable. For the equations showed that if the universe was static at the outset, the gravitational attraction of the matter would make it all collapse in upon itself. That seemed ridiculous, for there was no reason to suppose that space was so unstable. Einstein found he could stabilize his model by adding a simple constant term to the equations. If this constant was not zero, the model would not have to collapse under its own gravity. This "cosmological constant," Einstein admitted, was only "a hypothetical term." It was "not required by the theory as such nor did it seem natural from a theoretical point of view." In fact, "The term is necessary only for the purpose of making possible a quasi-static distribution of matter."

The introduction of such a constant implies a considerable renunciation of the logical simplicity of the theory... Since I introduced this term, I had always a bad conscience... I am unable to believe that such an ugly thing should be realized in nature.        —Einstein to Lemaître, 1947

Vesto Slipher How Slipher could measure velocities in the heavens Andromeda Spiral Nebula in Ursa Major (M. 101)

The Light from Distant Nebulae The powerful belief in a static universe could only be overturned by the weight of accumulating observations. The first of these observations had already been reported in 1915. Probably the observation was unknown to Einstein when he was developing his theory and corresponding with de Sitter. World War I had disrupted communications between the English-speaking nations and Germany, where Einstein worked, while de Sitter had only a second-hand, incomplete report of the crucial observation. The observation had been made at the Lowell Observatory in Arizona. Its founder, Percival Lowell, suspected that spectral lines seen in the light from one species of nebula, the "planetary" nebulae, might also be found in the spectra of spiral nebulae. In 1909 Lowell asked his assistant Vesto Slipher to get spectra of spiral nebulae. Slipher initially doubted that it could be done. Then he realized that for nebulae with their extended surfaces, in contrast to the point images of stars, the critical instrumental factor was not telescope size (rival Lick Observatory in California had a much larger telescope) but camera "speed" — the exposure time needed to photograph spectra of nebulae. With a new camera, its speed increased by a factor of 30, on the night of 17 September 1912 Slipher obtained a spectrogram for the Andromeda Nebula. The spectrogram indicated that the nebula was approaching the solar system at an amazingly high velocity. Slipher made more observations, exposing the same photographic plate over multiple nights (for example, 29, 30, and 31 December 1912). These yielded velocities averaging 300 km/sec. That was so large that some astronomers did not believe it possible. Over the next two years, Slipher measured velocities for other spiral nebulae. The first few measurements revealed approaching nebulae on the south side of our galaxy and receding nebulae on the opposite side. Slipher formed a "drift" hypothesis. He thought that it was our galaxy that was moving relative to the nebulae, toward the south and away from the north. However, observations of more spirals contradicted this. Receding spirals were found on the south side of our galaxy as well as on the north side. Slipher nevertheless clung to his drift hypothesis. Perhaps more observations, he argued, would find at least a preponderance of approaching nebulae on the south side, toward which he thought our galaxy was moving. A different interpretation of the velocities seen in spiral nebulae soon turned up. De Sitter's model of a static universe had a diminishing frequency of light vibrations with increasing distance. Slipher had calculated velocities by using the rule that the frequency of light observed will change if the source of the light is moving rapidly away — but perhaps this was an illusion. Perhaps distant objects were not really receding at great speeds, but were only emitting a different frequency of light. Nothing like that happened in Einstein's model of a static universe, so Slipher's measurements might give a way to choose between the two models. World War I had slowed communications, but by 1921 de Sitter knew of Slipher's velocity measurements for 25 spiral nebulae. Only 3 were approaching. They could be explained away as the result of large velocities in random directions, superimposed on a much smaller systematic recession. Still, de Sitter hesitated to draw any conclusions. Velocities were known, but the other half of the predicted relation — the distances to the nebulae — were unknown. This crucial information would be developed by Edwin Hubble as he extended his measurements of "Island Universes" (described on the previous page).

"Planetary" nebulae like the one above are immense blobs of gas that often appear as rings, something like the orbit of a planet. They are now known to be in our own galaxy, relatively nearby. Spiral nebulae like the one below, seen side-on, are now known to be galaxies like our Milky Way, far more distant.

Milton Humason on Mount Wilson How Hubble found the distances MORE about: Hubble's distances to the nebulae were too small Who Was Edwin Hubble? Hubble's campaign to establish the velocity-distance relation

Hubble's Surprising Relationship In 1928 Edwin Hubble attended a meeting of the International Astronomical Union, held that year in Holland. There Hubble discussed cosmological theories with de Sitter. Hubble returned to the Mount Wilson Observatory determined to test de Sitter's theory. Hubble directed his assistant Milton Humason, a gifted and meticulous observer, to study faint nebulae, which would presumably be especially distant. Did the frequency of their light differ from the light coming from closer nebulae? Now, a slower frequency corresponds to a longer wavelength of light, that is, light closer to the red end of the spectrum. Thus what Hubble and Humason were seeking was a displacement of lines in the spectrum toward the red, what later came to be called a "red shift". Such a shift, Humason later explained, was what "might be expected on de Sitter's theory of curved space-time." Humason obtained velocities and Hubble obtained distances. They found a linear relationship — roughly speaking, the greater the receding velocity of a nebula, the farther the distance to it. Their data were skimpy, and the interpretation was shaky in detail. (Indeed it was later discovered that Hubble's distances to the nebulae were only half the actual distances.) Indeed his figures disagreed with what scientists already knew about the age of the universe. Nonetheless, the velocity-distance relation was a bold and brilliant extrapolation. The results establish a roughly linear relation between velocities and distance among nebulae.        —Edwin Hubble, 1929 Not until the final paragraph of his 1929 paper did Hubble mention de Sitter, or indeed theory at all. And then Hubble simply noted that the velocity-distance relation might represent the de Sitter effect and might be of interest for cosmological discussion. Hubble emphasized the empirical, observational aspect of his work. His chief goal was to convince skeptical readers that the velocity-distance relation really existed. Hubble's 1929 velocity-distance relation for 46 nebulae. The black dots and the solid line represent the solution obtained from the 24 nebulae for which individual distances were determined, using them separately. Empty circles and the dashed line represent the solution obtained by combining the nebulae into groups. The cross represents the mean velocity for a set of 22 nebulae whose distances could not be estimated individually. There is more to the advance of science than new observations and new theories. Ultimately, people must be persuaded. In science, as in a court of law, advocates for each side of an issue present the best case possible in an attempt to reach the truth. A heroic image of pristine science may exclude the use of rhetorical skills. Advocacy, however, is an integral part of real science. There can be no judgment until the arguments are laid out clearly and energetically. Meanwhile Hubble carried on a scientific campaign to pin down the velocity-distance relation beyond question with improved observations . New observations by Hubble and Humason … concerning the redshift of light in distant nebulae make the presumptions near that the general structure of the Universe is not static.        —Einstein Hubble's undeniable observations that the light from nebulae showed a red shift increasing with distance ruled out the possibility that Einstein's static model represented the real universe. De Sitter's alternative static model, without matter, was also ruled out by new observations. De Sitter had supposed that the density of matter in the universe might be close enough to zero so that his model could work. A new estimate, in 1927, of the mass of our galaxy caused de Sitter to reexamine this assumption and reject it. There could be no more pretense that de Sitter's model might correspond to reality. Einstein too soon acknowledged that the red shift overthrew the old assumption of a static universe.

How old is the Universe? Read about an example of Hubble's rhetorical skill

Friedmann in 1922 or 1923.

An Expanding Universe? At a meeting in London of the Royal Astronomical Society early in 1930, de Sitter admitted that neither his nor Einstein's solution to the field equations could represent the observed universe. The English astronomer Arthur Eddington next raised "one puzzling question." Why should there be only these two solutions? Answering his own question, Eddington supposed that the trouble was that people had only looked for static solutions. Both the solutions [to the field equations, de Sitter's and Einstein's] must be rejected, and as these are the only statical solutions of the equations… the true solution represented in nature must be a dynamical solution.        —Willem de Sitter, 1931 Georges Lemaître In fact a few astronomers had been looking for other solutions to Einstein's equations. Back in 1922, the Russian meteorologist andmathematician Alexander Friedmann had published a set of possible mathematical solutions that gave a non-static universe. Einstein noted that this model was indeed a mathematically possible solution to the field equations. Later, Friedmann would be hailed as an example of great Soviet science. But through the 1920s, neither Einstein nor anyone else took any interest in Friedmann's work, which seemed merely an abstract theoretical curiosity. Most astronomers continued to take it for granted that the real universe was static. When Friedmann published again in 1924, the paper, seen as a matter of pure relativity theory with no astronomical interest, was omitted from the annual survey of scientific papers on astronomical topics. He could not stand up for his ideas, for a year later he died of typhoid fever, only 37 years old. The Belgian astrophysicist Georges Lemaître had also published a model of an expanding universe, in 1927. Lemaître was a Catholic priest (from 1960 until his death in 1966 he was president of the Pontifical Academy of Sciences). His contribution to science is now celebrated, but at the time it made no impression. Published in the little-read Annals of the Brussels Scientific Society, it was easily overlooked. Those (including Eddington) who did read Lemaître's 1927 paper had promptly forgotten it. I have found the true solution, or at least a possible solution, which must be somewhere near the truth, in a paper... by Lemaître... which had escaped my notice at the time.        —de Sitter to Shapley, 1930 Lemaître saw a report of the 1930 Royal Astronomical Society meeting and wrote to Eddington, his former teacher, to remind him of the 1927 paper. Eddington now recognized the value of Lemaître's study. Eddington shared Lemaître's paper with de Sitter, who soon after wrote to Harlow Shapley at Harvard, "I have found the true solution, or at least a possible solution, which must be somewhere near the truth, in a paper… by Lemaître… which had escaped my notice at the time." Einstein soon confirmed that Lemaître's work "fits well into the general theory of relativity." In 1931 de Sitter publicly praised Lemaître's "brilliant discovery, the ‘expanding universe'." In that same year, Lemaître went on to propose that the present universe is the "ashes and smoke of bright but very rapid fireworks." We can now see this "fireworks theory" (as it came to be called) as a first version of the "Big Bang" theory of the origin of the universe. What did it mean, that strange new phrase, expanding universe? It meant that the light from distant nebulae was red-shifted not from some peculiar de Sitter effect, but because the nebulae were actually moving away from us. This was not because there is anything special about us — by now astronomers understood that the nebulae are galaxies more or less like our own. Each of these galaxies was moving away from all the other galaxies. Space itself was expanding between them. There was no special point somewhere among the stars where the great expansion had started—we and all other galaxies are inside that place. Thus the farther any two galaxies were apart, the faster they continued to separate—which was precisely Hubble's velocity-distance relation. Cosmologists recognized at once that an expanding universe means that in the far future the galaxies will be spread much farther apart. Looking back, long ago the universe must have been far denser. Did time itself have a beginning? Hubble's few measurements were enough to persuade the world's best scientists to take up a radically new view of the nature, the origin, and the fate of the universe. Perhaps scientists could take up this view so quickly because quantum and relativity theory had prepared them for remarkable revelations. The recognition that the universe is expanding was no less revolutionary — the culmination of a truly exceptional period in the history of science. The expansion of the universe is now seen as one of the great scientific discoveries, and Hubble generally gets the credit. More precisely, however, Hubble established an empirical formula that led the great majority of scentists to believe in the expansion. It is an open historical and philosophical question in what sense Hubble's correlation of data was a "discovery," and exactly how the claim that the universe is expanding grew in scientists' minds. Many observations have confirmed the model of an expanding universe that Hubble's relationship validated. But Hubble should not be judged simply by which of his conclusions are now believed to be correct. More important was the direction he pointed out: using galaxies as a key to cosmic history. Hubble's work should be appreciated for the assumptions it overthrew, and for the vistas it opened, as a landmark accomplishment of human intellect. 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