VUV Spectroscopy of Atoms, Molecules and Surfaces

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126 REFERENCES [152] T.-C. Chiang, Comments At. Mol. Phys. 13, 299 (1983). [153] A. B. McLean, Surf. Sci. 220, L671 (1989). [154] J. N. Andersen and U. O. Karlsson, Phys. Rev. B 41, 3844 (1990). [155] G. L. Lay et al., Prog. Surf. Sci. 48, 145 (1995). [156] S. K. So and W. Ho, Appl. Phys. A 47, 213 (1988). [157] Y. Chen et al., J.Chem.Phys.95, 8442 (1991). [158] S. Conrad et al., Surf. Sci. 382, 79 (1997). [159] L. J. Richter and R. R. Cavanagh, Prog. Surf. Sci. 39, 155 (1992). [160] V. Liberman et al., J.Chem.Phys.96, 1590 (1992). [161] X.-Y. Zhu et al., J.Chem.Phys.97, 5856 (1992). [162] R. D. Schnell et al., Phys.Rev.B32, 8052 (1985). [163] W. Ranke and J. Wasserfall, Surf. Sci. 292, 10 (1993). [164] B. Murphy et al., Surf. Sci. 317, 73 (1994). [165] K. Prabhakaran and T. Ogino, Surf. Sci. 325, 263 (1995). [166] I. L. Shumay and U. Höfer, Phys. Rev. B 53, 15878 (1996). [167] K. Sokolowski-Tinten et al., Phys. Rev. Lett. 81, 3679 (1998). [168] C. Guo et al., Phys. Rev. Lett. 84, 4493 (2000).
Chapter 6 Two-colour pump-probe experiments on He using high-order harmonics 6.1 Introduction Knowledge about basic atomic and molecular properties such as radiative transition probabilities and excitation- and ionization cross sections is important for the interpretation of astrophysical spectra and in the modelling of stellar properties [1]. For the latter purpose the opacities of stellar envelopes are of particular importance as reflected by the launch of the international Opacity Project [2, 3]. The opacity determines the degree of penetration of radiation through matter and depends on atomic transition frequencies, oscillator strengths and excitation- and ionization cross sections [4]. The Opacity Project aims at systematic and accurate calculations of these quantities using the R-matrix method, in order to compensate for the lack of experimental data [5]. Recently, a synchrotron radiation beamline was constructed at Aarhus University, dedicated to measurements of absolute photoionization cross sections of astrophysically relevant ions. So far, experimental data have been recorded for C + ,N + ,O + ,Mg + ,Al + and S + , providing a test ground for the opacity calculations (see, e.g., [6, 7]). Oscillator strengths (or transition probabilities) are related to the estimated abundances of the elements in the stars, thus constituting important input parameters for models dealing with the origin and evolution of the universe [8]. Since the oscillator strength is proportional to the square of the
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VUV Spectroscopy of Atoms, Molecule
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ii CONTENTS 4 .6 Conclusion . . . .
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iv Experimental and theoretical stu
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vi me to the principle of negative-
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viii
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2 VUV light generation: possibiliti
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10 VUV light generation: possibilit
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18 REFERENCES [14 ] C. R. Vidal, in
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20 REFERENCES [55] C. J. G. Uiterwa
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22 REFERENCES [98] Parameters from
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24 Negative ions ing the binding en
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26 Negative ions located energetica
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28 Negative ions available has been
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30 Negative ions assignment will th
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32 Negative ions feel the repulsion
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34 Negative ions Figure 2.1: Adiaba
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36 Negative ions
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38 REFERENCES [16] E. Kopp, Adv. Sp
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40 REFERENCES [63] P. Balling et al
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42 REFERENCES
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44 High-resolution VUV spectroscopy
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60 REFERENCES [19] J. S. Nielsen an
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62 Lifetimes of molecular negative
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Page 86 and 87: 76 REFERENCES [19] V. V. Petrunin e
Page 88 and 89: 78 REFERENCES [66] F. Robicheaux, P
Page 90 and 91: 80 Chapter 5. Femtosecond VUV core-
Page 110 and 111: 100 Chapter 5. Femtosecond VUV core
Page 130 and 131: 120 REFERENCES [17] A. Cavalleri et
Page 132 and 133: 122 REFERENCES [61] R. J. Finlay et
Page 134 and 135: 124 REFERENCES [104]R.W.Joyner,inTh
Page 138 and 139: 128 Chapter 6. Two-colour pump-prob
Page 154 and 155: 144 REFERENCES [16] Information ava
Page 156 and 157: 146 REFERENCES [62] S. Baier et al.
Page 158 and 159: 148 The following three chapters ar
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