Physics For Scientists And Engineers 6E - part 330

A.34

A p p e n d i x E • Nobel Prizes

1922 (P) Niels Bohr for his model of the atom and its radiation (1913).

(C) Francis W. Aston for using the mass spectrograph to study atomic weights,
thus discovering 212 of the 287 naturally occurring isotopes.

1923 (P) Robert A. Millikan for measuring the charge on an electron (1911) and for

studying the photoelectric effect experimentally (1914).

1924 (P) Karl M. G. Siegbahn for his work in x-ray spectroscopy.
1925 (P) James Franck and Gustav Hertz for discovering the Franck–Hertz effect in

electron–atom collisions.

1926 (P) Jean-Baptiste Perrin for studying Brownian motion to validate the discontinu-

ous structure of matter and measure the size of atoms.

1927 (P) Arthur Holly Compton for discovering the Compton effect on x-rays, their

change in wavelength when they collide with matter (1922), and Charles T. R.
Wilson for inventing the cloud chamber, used to study charged particles (1906).

1928 (P) Owen W. Richardson for studying the thermionic effect and electrons emit-

ted by hot metals (1911).

1929 (P) Louis Victor de Broglie for discovering the wave nature of electrons (1923).
1930 (P) Chandrasekhara Venkata Raman for studying Raman scattering, the scatter-

ing of light by atoms and molecules with a change in wavelength (1928).

1932 (P) Werner Heisenberg for creating quantum mechanics (1925).
1933 (P) Erwin Schrödinger and Paul A. M. Dirac for developing wave mechanics

(1925) and relativistic quantum mechanics (1927).
(C) Harold Urey for discovering heavy hydrogen, deuterium (1931).

1935 (P) James Chadwick for discovering the neutron (1932).

1936 (P) Carl D. Anderson for discovering the positron in particular and antimatter

in general (1932) and Victor F. Hess for discovering cosmic rays.
(C) Peter J. W. Debye for studying dipole moments and diffraction of x-rays and
electrons in gases.

1937 (P) Clinton Davisson and George Thomson for discovering the diffraction of elec-

trons by crystals, confirming de Broglie’s hypothesis (1927).

1938 (P) Enrico Fermi for producing the transuranic radioactive elements by neutron

irradiation (1934–1937).

1939 (P) Ernest O. Lawrence for inventing the cyclotron.
1943 (P) Otto Stern for developing molecular-beam studies (1923) and using them to

discover the magnetic moment of the proton (1933).

1944 (P) Isidor I. Rabi for discovering nuclear magnetic resonance in atomic and

molecular beams.
(C) Otto Hahn for discovering nuclear fission (1938).

1945 (P) Wolfgang Pauli for discovering the exclusion principle (1924).
1946 (P) Percy W. Bridgman for studying physics at high pressures.
1947 (P) Edward V. Appleton for studying the ionosphere.
1948 (P) Patrick M. S. Blackett for studying nuclear physics with cloud-chamber pho-

tographs of cosmic-ray interactions.

1949 (P) Hideki Yukawa for predicting the existence of mesons (1935).
1950 (P) Cecil F. Powell for developing the method of studying cosmic rays with pho-

tographic emulsions and discovering new mesons.

1951 (P) John D. Cockcroft and Ernest T. S. Walton for transmuting nuclei in an acceler-

ator (1932).
(C) Edwin M. McMillan for producing neptunium (1940) and Glenn T. Seaborg
for producing plutonium (1941) and further transuranic elements.

1952 (P) Felix Bloch and Edward Mills Purcell for discovering nuclear magnetic reso-

nance in liquids and gases (1946).

1953 (P) Frits Zernike for inventing the phase-contrast microscope, which uses inter-

ference to provide high contrast.

1954 (P) Max Born for interpreting the wave function as a probability (1926) and

other quantum-mechanical discoveries and Walther Bothe for developing the co-

A P P E N D I X E • Nobel Prizes

A.35

incidence method to study subatomic particles (1930–1931), producing, in
particular, the particle interpreted by Chadwick as the neutron.

1955 (P) Willis E. Lamb, Jr., for discovering the Lamb shift in the hydrogen spectrum

(1947) and Polykarp Kusch for determining the magnetic moment of the elec-
tron (1947).

1956 (P) John Bardeen, Walter H. Brattain, and William Shockley for inventing the tran-

sistor (1956).

1957 (P) T.-D. Lee and C.-N. Yang for predicting that parity is not conserved in beta

decay (1956).

1958 (P) Pavel A. ˇCerenkov for discovering ˇCerenkov radiation (1935) and Ilya M.

Frank and Igor Tamm for interpreting it (1937).

1959 (P) Emilio G. Segrè and Owen Chamberlain for discovering the antiproton (1955).
1960 (P) Donald A. Glaser for inventing the bubble chamber to study elementary par-

ticles (1952).
(C) Willard Libby for developing radiocarbon dating (1947).

1961 (P) Robert Hofstadter for discovering internal structure in protons and neutrons

and Rudolf L. Mössbauer for discovering the Mössbauer effect of recoilless
gamma-ray emission (1957).

1962 (P) Lev Davidovich Landau for studying liquid helium and other condensed

matter theoretically.

1963 (P) Eugene P. Wigner for applying symmetry principles to elementary-particle

theory and Maria Goeppert Mayer and J. Hans D. Jensen for studying the shell
model of nuclei (1947).

1964 (P) Charles H. Townes, Nikolai G. Basov, and Alexandr M. Prokhorov for develop-

ing masers (1951–1952) and lasers.

1965 (P) Sin-itiro Tomonaga, Julian S. Schwinger, and Richard P. Feynman for developing

quantum electrodynamics (1948).

1966 (P) Alfred Kastler for his optical methods of studying atomic energy levels.
1967 (P) Hans Albrecht Bethe for discovering the routes of energy production in stars

(1939).

1968 (P) Luis W. Alvarez for discovering resonance states of elementary particles.
1969 (P) Murray Gell-Mann for classifying elementary particles (1963).
1970 (P) Hannes Alfvén for developing magnetohydrodynamic theory and Louis Eugène

Félix Néel for discovering antiferromagnetism and ferrimagnetism (1930s).

1971 (P) Dennis Gabor for developing holography (1947).

1972 (P) John Bardeen, Leon N. Cooper, and John Robert Schrieffer for explaining super-

conductivity (1957).

1973 (P) Leo Esaki for discovering tunneling in semiconductors, Ivar Giaever for dis-

covering tunneling in superconductors, and Brian D. Josephson for predicting
the Josephson effect, which involves tunneling of paired electrons
(1958–1962).

1974 (P) Anthony Hewish for discovering pulsars and Martin Ryle for developing radio

interferometry.

1975 (P) Aage N. Bohr, Ben R. Mottelson, and James Rainwater for discovering why some

nuclei take asymmetric shapes.

1976 (P) Burton Richter and Samuel C. C. Ting for discovering the J/psi particle, the

first charmed particle (1974).

1977 (P) John H. Van Vleck, Nevill F. Mott, and Philip W. Anderson for studying solids

quantum-mechanically.
(C) Ilya Prigogine for extending thermodynamics to show how life could arise in
the face of the second law.

1978 (P) Arno A. Penzias and Robert W. Wilson for discovering the cosmic background

radiation (1965) and Pyotr Kapitsa for his studies of liquid helium.

1979 (P) Sheldon L. Glashow, Abdus Salam, and Steven Weinberg for developing the the-

ory that unified the weak and electromagnetic forces (1958–1971).

A.36

A p p e n d i x E • Nobel Prizes

1980 (P) Val Fitch and James W. Cronin for discovering CP (charge-parity) violation

(1964), which possibly explains the cosmological dominance of matter over
antimatter.

1981 (P) Nicolaas Bloembergen and Arthur L. Schawlow for developing laser spec-

troscopy and Kai M. Siegbahn for developing high-resolution electron spec-
troscopy (1958).

1982 (P) Kenneth G. Wilson for developing a method of constructing theories of

phase transitions to analyze critical phenomena.

1983 (P) William A. Fowler for theoretical studies of astrophysical nucleosynthesis

and Subramanyan Chandrasekhar for studying physical processes of importance
to stellar structure and evolution, including the prediction of white dwarf stars
(1930).

1984 (P) Carlo Rubbia for discovering the W and Z particles, verifying the elec-

troweak unification, and Simon van der Meer, for developing the method of sto-
chastic cooling of the CERN beam that allowed the discovery (1982–1983).

1985 (P) Klaus von Klitzing for the quantized Hall effect, relating to conductivity in

the presence of a magnetic field (1980).

1986 (P) Ernst Ruska for inventing the electron microscope (1931), and Gerd Binnig

and Heinrich Rohrer for inventing the scanning-tunneling electron microscope
(1981).

1987 (P) J. Georg Bednorz and Karl Alex Müller for the discovery of high-temperature

superconductivity (1986).

1988 (P) Leon M. Lederman, Melvin Schwartz, and Jack Steinberger for a collaborative ex-

periment that led to the development of a new tool for studying the weak nu-
clear force, which affects the radioactive decay of atoms.

1989 (P) Norman Ramsay for various techniques in atomic physics; and Hans Dehmelt

and Wolfgang Paul for the development of techniques for trapping single-
charge particles.

1990 (P) Jerome Friedman, Henry Kendall and Richard Taylor for experiments important

to the development of the quark model.

1991 (P) Pierre-Gilles de Gennes for discovering that methods developed for studying

order phenomena in simple systems can be generalized to more complex
forms of matter, in particular to liquid crystals and polymers.

1992 (P) George Charpak for developing detectors that trace the paths of evanescent

subatomic particles produced in particle accelerators.

1993 (P) Russell Hulse and Joseph Taylor for discovering evidence of gravitational

waves.

1994 (P) Bertram N. Brockhouse and Clifford G. Shull for pioneering work in neutron

scattering.

1995 (P) Martin L. Perl and Frederick Reines for discovering the tau particle and the

neutrino, respectively.

1996 (P) David M. Lee, Douglas C. Osheroff, and Robert C. Richardson for developing a

superfluid using helium-3.

1997 (P) Steven Chu, Claude Cohen-Tannoudji, and William D. Phillips for developing

methods to cool and trap atoms with laser light.

1998 (P) Robert B. Laughlin, Horst L. Störmer, and Daniel C. Tsui for discovering a new

form of quantum fluid with fractionally charged excitations.

1999 (P) Gerardus ’T Hooft and Martinus J. G. Veltman for studies in the quantum

structure of electroweak interactions in physics.

2000 (P) Zhores I. Alferov and Herbert Kroemer for developing semiconductor het-

erostructures used in high-speed electronics and optoelectronics and Jack St.
Clair Kilby for participating in the invention of the integrated circuit.

2001 (P) Eric A. Cornell, Wolfgang Ketterle, and Carl E. Wieman for the achievement of

Bose–Einstein condensation in dilute gases of alkali atoms.

2002 (P) Raymond Davis Jr. and Masatoshi Koshiba for the detection of cosmic neutri-

nos and Riccardo Giacconi for contributions to astrophysics that led to the dis-
covery of cosmic x-ray sources.

A.37

CHAPTER 1

1. 0.141 nm
3. 2.15 ! 10

kg/m

5. 4"#(r

)/3

7. (a) 4.00 u % 6.64 ! 10

g (b) 55.9 u % 9.28 ! 10

9. 8.72 ! 10

atom/s

11. (a) 72.6 kg (b) 7.82 ! 10

atoms

13. No.
15. (b) only
17. The units of G are m

/kg · s

19. 9.19 nm/s
21. 1.39 ! 10

23. (a) 0.071 4 gal/s (b) 2.70 ! 10

/s (c) 1.03 h

25. 11.4 ! 10

kg/m

27. 667 lb/s
29. (a) 190 yr (b) 2.32 ! 10

times

31. 151&m
33. 1.00 ! 10

35. (a) 2.07 mm (b) 8.62 ! 10

times as large

37. 5.0 m
39. 2.86 cm
41.

! 10

balls

43.

! 10

45.

! 10

kg;

! 10

47.

! 10

tuners

49. (a) (346 ' 13) m

(b) (66.0 ' 1.3) m

51. (1.61 ' 0.17) ! 10

kg/m

53. 31 556 926.0 s
55. 5.2 m

, 3%

57. 2.57 ! 10

59. 0.579 t ft

/s ( 1.19 ! 10

61. 3.41 m
63. 0.449%
65. (a) 0.529 cm/s (b) 11.5 cm/s
67. 1 ! 10

gal/yr

69.

! 10

stars

71. (a) 3.16 ! 10

s/yr (b) 6.05 ! 10

CHAPTER 2

1. (a) 2.30 m/s (b) 16.1 m/s (c) 11.5 m/s
3. (a) 5 m/s (b) 1.2 m/s (c) $ 2.5 m/s (d) $ 3.3 m/s (e) 0

5. (a) 3.75 m/s (b) 0
7. (a) $ 2.4 m/s (b) $ 3.8 m/s (c) 4.0 s
9. (a) 5.0 m/s (b) $ 2.5 m/s (c) 0 (d) 5.0 m/s

11. 1.34 ! 10

m/s

13. (a) 52.4 ft/s, 55.0 ft/s, 55.5 ft/s, 57.4 ft/s (b) 0.598 ft/s

15. (a) 2.00 m (b) $3.00 m/s (c) $2.00 m/s

17. (a) 1.3 m/s

(b) 2.0 m/s

at 3 s

at 8 s

19. 2.74 ! 10

m/s

, which is 2.79 ! 10

21. $ 16.0 cm/s

23. (a) 4.53 s (b) 14.1 m/s
25. (a) 2.56 m (b) $ 3.00 m/s
27. (a) 20.0 s (b) no
29. 3.10 m/s
31. (a) $ 202 m/s

(b) 198 m

33. (a) 4.98 ! 10

s (b) 1.20 ! 10

m/s

35. (a) v

/2 (d) v

(e) yes, no

37. (a) 3.00 m/s (b) 6.00 s (c) $ 0.300 m/s

(d) 2.05 m/s

39. 31 s
41. $99.3/h
43. (a) 10.0 m/s up (b) 4.68 m/s down
45. (a) 2.17 s (b) $ 21.2 m/s (c) 2.23 s
47. (a) 29.4 m/s (b) 44.1 m
49. (a) 7.82 m (b) 0.782 s
51. 7.96 s
53. (a) a

(t) % a

(

Jt, v

(t) % v

(

t ( (1/2)Jt

x(t) % x

(

t ( (1/2)a

(

(1/6)Jt

55. (a) a % $ (10.0 ! 10

m/s

)t ( 3.00 ! 10

m/s

;

x % $ (1.67 ! 10

m/s

(

(1.50 ! 10

m/s

(b) 3.00 ! 10

s (c) 450 m/s (d) 0.900 m

59. (a) Acela steadily cruises out of the city center at 45 mi/h. In

less than a minute it smoothly speeds up to 150 mi/h; then
its speed is nudged up to 170 mi/h. Next it smoothly slows to
a very low speed, which it maintains as it rolls into a railroad
yard. When it stops, it immediately begins backing up and
smoothly speeds up to 50 mi/h in reverse, all in less than
seven minutes after it started. (b) 2.2 mi/h/s % 0.98 m/s

61. 48.0 mm
63. (a) 15.0 s (b) 30.0 m/s (c) 225 m
65. (a) 5.43 m/s

and 3.83 m/s

(b) 10.9 m/s and 11.5 m/s

67.

!10

m/s

Answers to Odd-Numbered Problems

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