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Biographical Memoirs: VOLUME 75

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Biographical Memoirs: VOLUME 75 BRUNO BENEDETTO ROSSI April 13, 1905–November 21, 1993 BY GEORGE W. CLARK The initial motivation of the experiment which led to this discovery [of Sco X-1] was a subconscious feeling for the inexhaustible wealth of nature, a wealth that goes far beyond the imagination of man. That feeling was possibly generated by experiences in my previous work on cosmic rays; more likely it was inborn and was the reason why, as a young man, I went into the field of cosmic rays. In any case, whenever technical progress opened a new window into the surrounding world, I felt the urge to look through this window, hoping to see something unexpected.1 BEGINNINGS BRUNO ROSSI WAS BORN April 13, 1905, in Venice, the eldest of three sons of Rino Rossi and Lina Minerbi. His father was an electrical engineer whose successful career began with work on the electrification of Venice. He wrote in his autobiography2 that his father loved science and would have chosen it for a career except for practical considerations. He attributes to his father the influence that turned what may have been an “inborn tendency toward science into a lifelong commitment.” He recalled: perfectly clear winter mornings when the air was so unusually transparent that the Alps surrounding Venice became clearly visible and appeared incredibly close (Fata Morgana if you are a child or a poet, anomalous atmospheric refraction if you are a scientist). On those mornings I would try to find a sandalo (a small gondola) and, accompanied by a friend, I would

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Biographical Memoirs: VOLUME 75 row standing on the stern, Venetian style, from the Lido, where I lived, to the school in Venice, where I studied. Throughout his life Rossi reveled in the natural beauty of the mountains, where he did many of his cosmic-ray experiments, the desert around Los Alamos, where he worked on the atomic bomb, and the seashore of Cape Cod, where he strolled in summer with a student or colleague, discussing the progress of research and his ideas for future experiments. He found pleasure and solace in art and poetry, especially the works of Dante Aligieri. His personality has been described by one of his young colleagues as “complex, that of a poet as much as a scientist.” Rossi was tutored at home until the age of fourteen, and then he attended the Ginnasio and the Liceo in Venice. After completing his university studies at the University of Padua and his doctorate in physics at the University of Bologna, he was appointed assistant to Antonio Garbasso, professor of experimental science at the University of Florence. His laboratory was in the Physics Institute of the university, located among the olive trees on the hill of Arcetri overlooking the ancient city. The austerity of the working conditions—an unheated laboratory and a meager salary—was offset by the stimulation of the intellectual life provided by a brilliant group that included Gilberto Bernardini, a recent doctoral graduate from the University of Pisa, the young Enrico Persico, professor of theoretical physics at the University of Florence, who gave lectures on the new quantum mechanics of Heisenberg and Schrödinger, and enthusiastic students, especially Guiseppe Occhialini, Rossi's first doctoral student and lifelong friend. ARCETRI AND PADUA (1928-38) From the beginning of his work at Arcetri, Rossi sought a line of investigation that would lead to something novel

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Biographical Memoirs: VOLUME 75 and important. His first publications describe several investigations that fell short of his ambitions. Then he read the paper of Walter Bothe and Walter Kolhörster describing their discovery of charged particles that penetrated 4.1 cm of gold. Their results were astonishing at a time when the most penetrating charged particles previously known were beta-decay electrons, which could be stopped by less than a millimeter of gold. The penetrating particles were clearly related to the Höhenstrahlung discovered by Victor Hess in manned balloon flights during 1911-12. Hess had proved the existence of a “radiation from above” that arrives from outer space and generates ionization throughout the atmosphere. Höhenstrahlung was generally assumed to be composed of photons of very great energy, since it was believed (before the discovery of pair production) that the penetrating power of photons increased with energy without limit. During the 1920s Robert Millikan made extensive measurements of the ionization produced by the mysterious radiation, which he renamed cosmic rays, and he proposed the theory that they were photons created as the birth cries of the elements formed by the fusion of hydrogen atoms in interstellar space. Although Rossi was skeptical of Millikan's theory, he had seen no way to make a significant contribution to cosmic-ray research by the established methods of investigation. It seemed to him that the Bothe and Kolhörster experiment, based on Bothe's recent invention of the coincidence method, had opened a new window on nature. They had set up two Geiger counters, one above the other in a vertical plane, each connected to a separate fiber electrometer. Discharge of a counter, caused by traversal of a charged particle, produced a fiber deflection, which was recorded photographically on a moving film. Coincident deflections within a small fraction of a second indicated a traversal of both counters

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Biographical Memoirs: VOLUME 75 by a single cosmic-ray-charged particle. Bothe and Kolhörster observed that insertion of a gold brick between the two counters caused only a small reduction in the rate of coincidences. This demonstrated that most of the cosmic rays at ground level are charged particles capable of penetrating at least 4.1 cm of gold. Their analysis led them to conclude that the primary radiation itself must also be charged particles. Independent evidence in support of this conclusion had been obtained in 1927 by the Dutch physicist Jacob Clay, who measured a small change in the rate of ionization produced by cosmic rays during a trip from Leiden to Java. Such a latitude effect was attributable to deflection of primary charged particles by the Earth's magnetic field. Millikan, on the other hand, had found no latitude variation in similar measurements, and stuck to his theory that the primaries were photons. Within a few weeks of reading the Bothe and Kohlhörster paper, Rossi had invented and published in Nature the design of an electronic coincidence circuit, based on a novel use of triode vacuum tubes (1). The much finer time resolution of the Rossi coincidence circuit and its adaptability to the detection of coincidences among any number of pulses enabled the detection and identification of interesting rare events that produce coincident pulses in several counters in the midst of high rates of background pulses in each counter. It was the first electronic AND circuit, a basic logic element of the electronic computers of the future. Its applications by Rossi to experiments on cosmic rays marked the beginning of electronic experimentation in nuclear and particle physics. By the spring of 1930 Rossi had fabricated Geiger-Müller counters according to the recently published description and had carried out several coincidence experiments. He communicated his early results to Bothe, who invited him

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Biographical Memoirs: VOLUME 75 to visit his Berlin laboratory that summer. There he carried out an improved version of the Bothe and Kolhörster experiment with his electronic coincidence circuit, detecting cosmic-ray particles that traversed 9.7 cm of lead. During his visit, Rossi's attention was drawn to the work of the Norwegian physicist Carl Störmer on the motion in the Earth's magnetic field of the low-energy-charged particles responsible for exciting the aurora. Where others had been daunted by the complexity of the Störmer theory, Rossi perceived a simple consequence that led him to predict an azimuthal asymmetry in the intensity of cosmic rays that would depend on the sign of the charge of the primary particles. Detection of such an effect would not only demonstrate that the primary radiation is, indeed, charged particles, but would also determine the sign of their charge. He published his prediction of what came to be known as the east-west effect in a letter to the Physical Review sent from Berlin in July 1930 (2). Back at Arcetri his attempt to detect an asymmetry yielded a statistically inconclusive resuit, a consequence of the high geomagnetic latitude of Florence, where the effect is small. On the basis of his theory, Rossi expected the asymmetry would be much greater at low geomagnetic latitudes and began preparations for an expedition to the Italian colony of Eritrea, where he expected to find a result consistent with the assumption that the primary particles were negative electrons. At this time, an enduring friendship began between Enrico Fermi, already famous for his work in theoretical physics, and Rossi as they led their respective groups in pioneering experimental investigations—of nuclear physics in Rome and high-energy particle physics in Florence. At the invitation of Fermi, Rossi delivered the introductory talk on cosmic rays at the Rome international conference on nuclear physics sponsored by the Royal Italian Academy in the fall of

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Biographical Memoirs: VOLUME 75 1931. To an audience that included Millikan and Arthur Compton, Rossi outlined the current experimental knowledge of cosmic rays and his reasons for doubting Millikan's theory of their nature and origin. He explained how coincidence experiments had demonstrated that most of the local cosmic rays are charged particles with more energy than could possibly be released in the synthesis of the heaviest atoms. Long afterwards, Rossi wrote2 that “Millikan clearly resented having his beloved theory torn to pieces by a mere youth, so much so that from that moment on he refused to recognize my existence.” Compton's reaction was quite different, and he later told Rossi that Rossi's talk had persuaded him to begin his own research on cosmic rays. Two of Rossi's experiments, carried out in the period immediately following the Rome conference, are striking for their simplicity and far-reaching implications. In the first he demonstrated the existence of cosmic-ray particles capable of penetrating an astonishing 1 meter of lead by observing the threefold coincidences of pulses from three Geiger counters aligned with respect to one another and separated by blocks of lead (3). Four years later, in three independent investigations at Caltech, Harvard, and Tokyo, the penetrating particles were identified as charged particles of a new species called mesotrons (later renamed muons) with a mass of approximately 200 times that of the electron. In the other experiment, inspired by Skobelzyn's description of high-energy particle tracks observed in a magnet cloud chamber, Rossi placed three Geiger counters in a triangular configuration so that they could not all three be discharged by a single particle traveling in a straight line. With the setup enclosed in a lead box, he found a rate of triple coincidences that demonstrated an abundant production of secondary particles (later called showers) by the

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Biographical Memoirs: VOLUME 75 interaction of cosmic rays in the lead (4). In an extension of this experiment, he measured the rate of triple coincidences as a function of the thickness of the lead above the counters. The results, which came to be known as the Rossi curve, showed a rapid rise of the triple coincidence rate as the thickness was increased to about 1.5 cm, followed by a slow decline (5). The Rossi curve showed that the local cosmic rays consist of two components, a soft component capable of prolific generation of particle showers but rapidly attenuated in lead and the penetrating component capable of traversing great thicknesses of lead and only occasionally giving rise to a shower. It also provided the first quantitative test of the theory of electron-photon cascade showers developed four years later by Bhabha and Heitler. Meanwhile, Rossi had arranged for Occhialini to work with Patrick Blackett in Manchester. Bringing to Manchester the new technique of electronic coincidence, Occhialini collaborated with Blackett in developing the first counter-controlled cloud chamber, achieving thereby a great increase in the efficiency of operation over random expansions. Photographs were soon obtained of locally produced particle showers that confirmed Rossi's results. In 1932, having won a national competition for an academic position, Rossi was called to the University of Padua as professor of experimental physics. Planning a new physics institute and supervising its construction left him little time to continue his experimental investigations. His project for measurement of the azimuthal asymmetry in the cosmic-ray intensity at low latitudes was delayed until 1933, when he finally was able to travel to Eritrea. In a publication (6) on the results of the experiment Rossi asserted that “cosmic rays consist chiefly of a charged corpuscular radiation with a continuous energy spectrum extending to very great energies. Moreover, the new results on the azi-

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Biographical Memoirs: VOLUME 75 muthal effect show that the charge is predominantly positive.” Much to his disappointment, the delay of his expedition had cost him the priority of discovery. Just as he was leaving on the expedition, he read the Physical Review articles of Thomas Johnson and of Luis Alvarez and Arthur Compton, who had independently measured the east-west effect in experiments in Mexico City. During the experiments in Eritrea, Rossi discovered a phenomenon that would have far-reaching consequences for cosmic-ray physics and astrophysics in the future—extensive cosmic-ray air showers (7). The discovery occurred during tests to determine the rate of accidental coincidences between the Geiger counters of his detector. To assure that no single particle could trigger all three counters he spread them out in a horizontal plane. He wrote (Rossi's translation from the original Italian): The frequency of the coincidences recorded with the counters at a distance from one another, shown in the tables as “chance coincidences” appears to be greater than would have been predicted on the basis of the resolving power of the coincidence circuit. Those observations made us question whether all of these coincidences were actually chance coincidences. This hypothesis appears to be supported by the following observation Since the interference of possible disturbances was ruled out by suitable tests, it seems that once in a while the recording equipment is struck by very extensive showers [degli sciami molto estesi di corpuscoli] of particles, which cause coincidences between counters, even placed at large distances from one another. Unfortunately, I did not have time to study this phenomenon more closely. Extensive air showers were rediscovered four years later by Auger and Maze, who carried out the first systematic study of their structure and size distribution. Air showers would be a principal theme of Rossi's postwar cosmic-ray research.

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Biographical Memoirs: VOLUME 75 FROM ITALY TO AMERICA (1938-43) While on vacation in Venice in 1937, Rossi was introduced to Nora Lombroso, daughter of Ugo Lombroso, professor of physiology at the University of Palermo, and Silvia Forti and granddaughter of the renowned physician and criminologist Cesare Lombroso. They were married in April of the following year. Meanwhile, the political climate in Italy was darkening with the growing influence of Hitler on Mussolini and the enactment of the Jewish laws. In September of 1938 Rossi was deprived of his position at the university. Recognizing the danger that loomed, the Rossis left Italy. After a brief stay at the Bohr Institute for Nuclear Physics in Copenhagen, they were invited by Patrick Blackett to come to the University of Manchester. There Rossi renewed his cosmic-ray research in discussions with Blackett concerning the evidence for the instability of the mesotron, and in an experiment with Ludwig Jánossy on the production of cascade showers in lead by cosmic-ray photons, in which he introduced the novel technique of anti-coincidence. In the spring of 1939 Rossi received an invitation from Arthur Compton to participate in a cosmic-ray symposium at the University of Chicago planned for the summer, and was offered the possibility of some kind of a job. With great reluctance to leave Europe and especially the warm hospitality of Patrick and Constance Blackett in Manchester, the Rossis sailed to New York in June. Before going on to Chicago they visited the Fermis, who had arrived six months earlier in New York City, where Enrico Fermi had accepted a professorship at Columbia University. Laura Fermi recalled their meeting: “Bruno, a few years younger than Enrico, was a quiet man, rather silent and shy. He let his lively wife do all the talking, and he was happy if he could withdraw

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Biographical Memoirs: VOLUME 75 into the background.”3 Many years later, Nora Rossi told me that she would replace the word “shy” with “reserved.” The mesotron was a major topic at the Chicago symposium. Afterwards, during a visit with the Comptons at their summer cottage in Michigan, Rossi roused enthusiastic support for a definitive test of the mesotron's instability. Within a few weeks he had constructed an apparatus to detect mesotrons by the coincidences of three Geiger counters aligned in a vertical plane and separated by blocks of lead. He packed it into an old bus and drove with Nora and a young collaborator, Barton Hoag, to Mt. Evans in Colorado. The measurements showed that the attenuation of the mesotron intensity is greater in the air between two altitudes on the mountain than in an equivalent thickness of a solid absorber. The result could be unequivocally attributed to radioactive decay of mesotrons in flight with a mean life at rest of approximately 2 microseconds. It was the first clear demonstration of the decay of a sub-nuclear particle (8). Rossi was appointed associate professor of physics at Cornell University in the spring of 1940. There he acquired his first American Ph.D. student, Kenneth Greisen, who would become one of the leading contributors to cosmic-ray research after the war. Greisen has recalled that, as a graduate student in theoretical physics with no knowledge of experimental physics, he went to Rossi's office and “asked if I would be welcome as a student under him; and he needed one, no matter how ignorant. So he took me, and for a couple of years I was his only student.” With a grant of $2,000, which Rossi had “demanded” for the startup of his research, they set up a facility for making Geiger counters and electronic circuits with the aim of carrying out an improved version of the experiment on the anomalous atmospheric attenuation of mesotrons and spent $1,000 on a station wagon to transport the equipment and themselves

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Biographical Memoirs: VOLUME 75 medium had been neglected. Rossi sensed a unique opportunity “to see something unexpected” through the new window of space technology. Rossi discussed with Herbert Bridge and Frank Scherb his ideas for an experiment aimed at measuring the composition and motion of ionized gas in interplanetary space. These ideas were embodied in the MIT plasma cup, developed and flown in a collaboration that included Alberto Bonetti, visiting from Italy, and Alan Lazarus. The plasma cup was launched aboard the space probe Explorer 10 on March 25, 1961, together with a magnetometer prepared at the Goddard Space Flight Center. The probe yielded data that revealed the boundary of the geomagnetic cavity and determined the supersonic speed and direction of the solar plasma flowing just outside the cavity (24). There followed a series of experiments in which ever more sophisticated plasma cups were sent on journeys around the planets and to the farthest reaches of the solar system, some on trips that returned data for more than two decades. Another idea that excited Rossi as he thought about the scientific opportunities offered by space vehicles was the possibility of exploring the sky in X rays. The pioneering work on solar X rays by Herbert Friedman and his collaborators at the Naval Research Laboratory was carried out with detectors with small sensitive areas and narrow fields of view. Their observational strategy, well suited to solar studies, had limited the chances of detecting an extra-solar source. It was obvious that if the nearest stars were only as luminous in X rays as the Sun, they would be far too faint to be detected by the most sensitive instruments then available. Even the most optimistic estimates of the intensities of possible celestial X-ray sources that had been made by various astronomers were discouragingly low. Rossi, however, sensed that the X-ray window on the universe had not

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Biographical Memoirs: VOLUME 75 yet been fully opened. It seemed to him that an exploratory observation with an X-ray detector having a much greater sensitivity than those used previously in solar studies might widen the window sufficiently to reveal something unexpected. The MIT group was fully occupied at the time with air shower experiments in Bolivia and New Mexico, a satellite gamma-ray astronomy program initiated by Kraushaar, and preparations for the interplanetary plasma experiment. Rossi therefore presented his idea for an exploratory effort in X-ray astronomy to Martin Annis, then president of a research and development company in Cambridge called American Science and Engineering, Inc. (AS&E). Annis had founded the company in 1958 with my participation and that of two other investors. The following year Rossi accepted Annis's invitation to be chairman of the board and chief scientific consultant to the company, and to devote whatever time he could spare from his MIT responsibilities and scientific advisory activities. In addition to his desire to find a means to carry out such an exploration, Rossi was eager to find new activities for the company outside of the defense-related research on which it was dependent at the time. Annis has described how Rossi was: more excited and enthusiastic that I ever saw him, before or since. He told me that on the way home on the plane [from a meeting] he had one of the best ideas that he had ever thought of. He described, in detail, his view that there was a “window” in the universe through which we had never looked. This window was the soft X-ray region of the spectrum. He was totally convinced that there were exciting discoveries to be made in this unknown world Perhaps I would be willing to spend AS&E money to begin the effort. I shared his enthusiasm, although I had no idea how the company might benefit. During that first conversation, he requested that I ask my people to think about new designs of large-area X-ray detectors and means to focus these soft X rays.

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Biographical Memoirs: VOLUME 75 Annis suggested that the person to implement the ideas might be Riccardo Giacconi, who had recently joined the company. Giacconi had done his thesis research at the University of Milan, where he had worked with Occhialini on cosmic-ray experiments, and he had held postdoctoral positions at the University of Indiana with Robert Thompson and at Princeton. Giacconi later wrote: In September 1959 [I] attended a party at Rossi's house and met Rossi for the first time. Rossi suggested that a venture into X-ray astronomy might prove very fruitful, not because of any theoretical predictions, but because nothing was known and there was the possibility for major new discoveries.5 Giacconi initiated a study of the theoretical and experimental possibilities for X-ray astronomy. With the help of Stanislaw Olbert and myself, acting as consultants to the company, he prepared an internal report6 that surveyed the prospects for X-ray astronomy and provided a basis for proposals to NASA. The report contained estimates for the intensities of various possible extra-solar X-ray sources, including certain types of stars, the Crab Nebula, and the Moon as a source of scattered solar X rays. It also described several instrumentation concepts, including an X-ray concentrator consisting of nested paraboloidal grazing-incidence mirrors invented by Giacconi and Rossi (21). NASA accepted a proposal for the development of X-ray optics, but refused the one for exploratory rocket experiments; NASA had already funded proposals from Cornell University and Lockheed Corporation for X-ray astronomy experiments, which ultimately failed to produce significant results. Giacconi then turned to the Air Force Cambridge Research Laboratory with which AS&E had contracts for research on the effects of X rays from high-altitude nuclear explosions. One of the offices of AFCRL, interested in the

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Biographical Memoirs: VOLUME 75 possibility of determining the lunar surface composition by analysis of scattered solar X rays, accepted proposals for experiments using detectors of large sensitive area on rotating rockets, which would scan a broad swath of the sky that included the Moon. The first two flights suffered mechanical failures. The third, in June 1962, detected no X rays from the Moon, but instead, an astonishingly bright X-ray source in the southern sky, which came to be called Sco X-1 (23). The paper, submitted to the Physics Review by Giacconi, Herbert Gursky, Frank Paolini, and Rossi, was considered so strange by Samuel Goudsmit, the editor, that he accepted the paper for publication only after receiving Rossi's personal assurance that “he assumed personal responsibility for its contents.”2 Optical studies of the optical counterpart of Sco X-1 by others eventually showed that it is a close binary system consisting of an ordinary dwarf star and a neutron star in a 19-hour orbit, one of several hundred similar systems in the galaxy in which matter drawn from a normal star falls to the surface of the neutron star. In the process, the potential gravitational energy of the falling matter is converted into heat and radiated as X rays with an energy yield per unit mass of accreted matter on the order of one-third times the square of the speed of light. The discovery of Sco X-1 inaugurated the new field of extra-solar X-ray astronomy, which became a major activity of the world's space research programs. AS&E maintained its leading position in X-ray astronomy for a decade until Giacconi left to become professor at Harvard University. Meanwhile, the MIT Cosmic Ray Group developed a variety of activities in X-ray astronomy encompassing balloon, rocket, and satellite experiments, several of which were carried out in collaboration with the AS&E group. For many years Rossi maintained an active role in the design and interpretation of the MIT plasma experiments.

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Biographical Memoirs: VOLUME 75 He did not participate directly in the MIT X-ray program, but he encouraged and supported it through his influence on promotions and the allocation of institute resources. Most of Rossi's work in X-ray astronomy was devoted to writings and talks devoted to reviews and interpretations of progress in the field. LATER YEARS: MIT (1970-93) During the 1960s the manner of Rossi's participation in space research changed once again, due to changes in the sociology of university research and the mechanisms of federal support. Just after the war, support came mostly in the form of large grants from the Office of Naval Research and the Atomic Energy Commission to institutions like the MIT Laboratory for Nuclear Science and Engineering. Resources were allocated according to the judgments of its director and senior professors, each responsible for some broad area of research. As more professorial positions became available, responsibility gradually shifted to individual faculty members for procuring funding to support graduate students, portions of their own salaries, and the purchase of materials for carrying out instrument-building projects or observational programs using existing national facilities. This trend was especially characteristic of the space research sponsored by NASA. Although NASA distributed large grants in its formative years, success of individual investigators in peer-judged competition for support of proposals gradually became the principal criterion for funding and a factor in academic promotion. In the Cosmic Ray Group, now located in the MIT Center for Space Research, Rossi's ideas continued to be influential, particularly in space plasma research, and the spirit of cooperation he engendered continued to pervade its activities. Although it was not an easy time for him as he became more remote from day-to-day

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Biographical Memoirs: VOLUME 75 scientific planning and analysis, he encouraged the growing autonomy of his former students and colleagues and helped in every way to advance their careers. In the last decade of his life, Rossi wrote several monographs on the history of the sciences in which he had been engaged for half a century (25, 26) and an autobiography. His writings are remarkable for the accuracy and objectivity with which he describes his own work and its relations to the work of others. They form a permanent monument to a scientist whose genius laid many of the foundations of high-energy physics and astrophysics, and whose leadership and humanity profoundly enhanced the lives of students and colleagues around the world. His own writings, together with the reminiscences generously provided in letters to me by his former students, have eased the task of a memoirist who owes the satisfactions of his own life in science to the leader of the group he joined as a graduate student. Bruno Rossi died at his home in Cambridge, Massachusetts, on November 21, 1993. His ashes rest in the graveyard of the church of San Miniato al Monte, which looks over the city of Florence and across to the hill of Arcetri, where he began his scientific odyssey. HONORS AND AWARDS 1949 Research Corporation Scientific Award 1963 Order of Merit of the Republic of Italy 1964 Honorary doctorate, University of Palermo 1965 Honorary professor, Universidad Mayor de San Andres, La Paz, Bolivia 1970 Gold Medal of the Italian Physical Society 1971 International “Fellrinelli” Award, l'Academia dei Lincei 1971 Honorary fellow, Tara Institute of Fundamental Research, India 1974 Honorary doctorate, University of Durham 1974 Cresson Medal, Franklin Institute, Philadelphia

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Biographical Memoirs: VOLUME 75 1975 Honorary fellow, Physical Research Institute, Ahmadabad, India 1976 Rumford Prize Award, American Academy of Arts and Sciences 1977 Honorary doctorate, University of Chicago 1985 National Medal of Science 1987 Wolf Prize in Physics NOTES 1. B. B. Rossi. Bull. Am. Acad. Arts Sci. 30(1977):17 2. B. B. Rossi. Moments in the Life of a Scientist. New York: Cambridge University Press, 1990. 3. L. Fermi. Atoms in the Family. Chicago: University of Chicago Press, 1954. 4. L. Hoddeson et al. Critical Assembly. New York: Cambridge University Press, 1993. 5. W. Tucker and R. Giacconi. The X-Ray Universe. Cambridge, Mass.: Harvard University Press, 1985. 6. R. Giacconi, G. Clark, and B. Rossi. A Brief Review of Experimental and Theoretical Progress in X-Ray Astronomy. ASE-TN-49, 1960.

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Biographical Memoirs: VOLUME 75 SELECTED BIBLIOGRAPHY REFERENCES 1930 (1) Method of registering multiple simultaneous impulses of several Geiger counters.Nature 125:636. (2) On the magnetic deflection of cosmic rays. Phys. Rev. 36:606. 1932 (3) Absorptionmessungen der durchdringenden korpuskularstrahlung in einem meter blei. Naturwiss. 20:65. (4) Nachweis einer sekundarstrahlung der durchdringenden korpuskularstrahlung Physik. Z. 33:304-305. 1933 (5) Uber die eigengschaften der durchdringenden korpuskularstrahlung in Meeresniveau.Z. Physik 82:151-78. 1934 (6) Directional measurement on the cosmc rays near the geomagnetic equator Phys. Rev. 45:212. (7) Misure della distribuzione angolare di intensita della radiazione penetrante all'Asmara. Ric. Sci. 5(1):579-89. 1939 (8) with N. Hilberry and J. B. Hoag. The disintegration of mesotrons. Phys. Rev. 56:837-38. 1941 (9) with K. Greisen. Cosmic ray theory. Rev. Mod. Phys. 13:240-309. 1942 (10) with N. Nereson. Experimental determination of the disintegration curve of mesotrons Phys. Rev. 62:417-22.

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Biographical Memoirs: VOLUME 75 1946 (11) with N. Nereson. Experimental arrangement for the measurement of small time intervals between the discharges of Geiger-Müller counters. Rev. Sci. Instrum. 17:65-71. 1947 (12) with H. S. Bridge. Cosmic-ray bursts in an unshielded chamber and under one inch of lead at different altitudes. Phys. Rev. 71:379-80. 1948 (13) with R. I. Hulsizer. Search for electrons in the primary radiation.Phys. Rev. 73:1402-1403. 1950 (14) with B. P. Gregory and J. H. Tinlot. Production of gamma rays in nuclear interactions of cosmic rays. Phys. Rev. 77:299-300. 1952 (15) with H. S. Bridge, C. Peyrou, and R. Safford. Cloud-chamber observations of the heavy charged unstable particles in cosmic rays. Phys. Rev. 90:912-33. 1953 (16) with H. S. Bridge, C. Peyrou, and R. Safford. Study of neutral V particles in a multiplate cloud chamber. Phys. Rev. 91:362-72. (17) with P. Bassi and G. W. Clark. Distribution of arrival times of air shower particles.Phys. Rev. 92:441-51. (18) Where do cosmic rays come from?Sci. Am. 189:64-70. 1954 (19) with H. S. Bridge. H. Courant, and H. DeStaebler, Jr. Possible example of the annihilation of a heavy particle. Phys. Rev. 95:1101-1103. 1957 (20) with G. Clark, J. Earl, W. Kraushaar, and F. Scherb. An experiment on air showers produced by high-energy cosmic rays. Nature 180:353-56.

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Biographical Memoirs: VOLUME 75 1960 (21) with R. Giacconi. A “telescope” for soft X-ray astronomy.J. Geophys. Res. 65:773-75. 1961 (22) with J. Linsley and L. Scarsi. Extremely energetic cosmic-ray event. Phys. Rev. Lett. 6:485-86. 1962 (23) with R. Giacconi, H. Gursky, and F. Paolini. Evidence for X rays from sources outside of the solar system. Phys. Rev. Lett. 9:439-43. 1963 (24) with A. Bonetti, H. S. Bridge, A. J. Lazarus, and F. Scherb. Explorer 10 plasma measurements. J. Geophys. Res. 68:4017-63. 1977 (25) X-ray astronomy. Daedalus 106:37-47. 1983 (26) The decay of “mesotrons” (1939-1943): Experimental particle physics in the age of innocence. In The Birth of Particle Physics, ed. L. M. Brown and L. Hoddeson. Cambridge: Cambridge University Press. BOOKS Rayons Cosmiques ( Paris: Hermann & Co., 1935). with L. Pincherle. Lezioni di Fisica Sperimentale ( Padova, 1936). with H. Staub. Ionization Chambers and Counters ( New York: McGraw-Hill Book Co., 1949). HIgh-Energy Particles ( New York: Prentice-Hall, Inc., 1952). Optics ( Reading: Addison-Wesley Publ. Co., Inc., 1957). Cosmic Rays ( New York: McGraw-Hill Book Co., 1964).

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Biographical Memoirs: VOLUME 75 with S. Olbert. Introduction to the Physicis of Space ( New York: McGraw-Hill Book Co., 1970). Moments in the Life of a Scientist ( New York: Cambridge University Press, 1990).