diff --git a/autotests/export/docbook/bibliography_precooked_aastex.xml b/autotests/export/docbook/bibliography_precooked_aastex.xml index fe77b72494..71fe700e56 100644 --- a/autotests/export/docbook/bibliography_precooked_aastex.xml +++ b/autotests/export/docbook/bibliography_precooked_aastex.xml @@ -3,25 +3,53 @@ See http://www.lyx.org/ for more information -->
-Collapsed Cores in Globular Clusters, Gauge-Boson Couplings, and AASTeX Examples -S. Djorgovski and Ivan R. King -Astronomy Department, University of California, Berkeley, CA 94720 -Visiting Astronomer Cerro Tololo Inter-American Observatory.CTIO is operated by AURA Inc. under contract to the National Science Foundation. -Society of Fellows, Harvard University. -present address: Center for Astrophysics60 Garden Street, Cambridge, MA 02138 -C. D. Biemesderfer -National Optical Astronomy Observatories, Tucson, AZ 85719 -Visiting Programmer, Space Telescope Science Institute -Patron, Alonso's Bar and Grill -aastex-help@aas.org -R. J. Hanisch -Space Telescope Science Institute, Baltimore, MD 21218 -Patron, Alonso's Bar and Grill -clusters: globular, peanut—bosons: bozos - +Collapsed Cores in Globular Clusters, Gauge-Boson Couplings, and AASTeX Examples + +S. Djorgovski and Ivan R. King + +Astronomy Department, University of California, Berkeley, CA 94720 + + +Visiting Astronomer Cerro Tololo Inter-American Observatory.CTIO is operated by AURA Inc. under contract to the National Science Foundation. + + +Society of Fellows, Harvard University. + + +present address: Center for Astrophysics60 Garden Street, Cambridge, MA 02138 + + + +C. D. Biemesderfer + +National Optical Astronomy Observatories, Tucson, AZ 85719 + + +Visiting Programmer, Space Telescope Science Institute + + +Patron, Alonso's Bar and Grill + +aastex-help@aas.org + + +R. J. Hanisch + +Space Telescope Science Institute, Baltimore, MD 21218 + + +Patron, Alonso's Bar and Grill + + +clusters: globular, peanut—bosons: bozos + + + This is a preliminary report on surface photometry of the major fraction of known globular clusters, to see which of them show the signs of a collapsed core. We also explore some diversionary mathematics and recreational tables. - - + + + +
Introduction A focal problem today in the dynamics of globular clusters is core collapse. It has been predicted by theory for decades , , , but observation has been less alert to the phenomenon. For many years the central brightness peak in M15 , seemed a unique anomaly. Then suggested a central peak in NGC 6397, and a limited photographic survey of ours found three more cases, including NGC 6624, whose sharp center had often been remarked on . @@ -107,7 +135,8 @@
Helicity Amplitudes -It has been realized that helicity amplitudes provide a convenient means for Feynman diagramFootnotes can be inserted like this. +It has been realized that helicity amplitudes provide a convenient means for Feynman diagram +Footnotes can be inserted like this. evaluations. These amplitude-level techniques are particularly convenient for calculations involving many Feynman diagrams, where the usual trace techniques for the amplitude squared becomes unwieldy. Our calculations use the helicity techniques developed by other authors ; we briefly summarize below.
Formalism @@ -133,7 +162,8 @@ - collisions can be expressed in terms of fermion strings of the form + collisions can be expressed in terms of fermion strings of the form + \bar{v}(p_{2},\sigma_{2})P_{-\tau}\hat{a}_{1}\hat{a}_{2}\cdots\hat{a}_{n}u(p_{1},\sigma_{1}), @@ -352,7 +382,9 @@ may be formed from particle four-momenta, gauge-boson polarization vectors or fermion strings with an uncontracted Lorentz index associated with final-state fermions. -Figures 1 and 2 should appear side-by-side in print + +Figures 1 and 2 should appear side-by-side in print + In the chiral representation the \gamma @@ -376,7 +408,8 @@ σ - and the unit matrix 1 as + and the unit matrix 1 as + \gamma^{\mu} & = & \left(\begin{array}{cc} 0 & \sigma_{+}^{\mu}\\ \sigma_{-}^{\mu} & 0 @@ -486,7 +519,8 @@ - giving + giving + \hat{a}=\left(\begin{array}{cc} 0 & (\hat{a})_{+}\\ (\hat{a})_{-} & 0 @@ -564,11 +598,13 @@ - The spinors are expressed in terms of two-component Weyl spinors as + The spinors are expressed in terms of two-component Weyl spinors as + u=\left(\begin{array}{c} (u)_{-}\\ (u)_{+} -\end{array}\right),v={\textbf{(}}\vdag_{+}{\textbf{,}}\vdag_{-}{\textbf{)}}.MathML export failed. Please report this as a bug. +\end{array}\right),v={\textbf{(}}\vdag_{+}{\textbf{,}}\vdag_{-}{\textbf{)}}. +MathML export failed. Please report this as a bug. The Weyl spinors are given in terms of helicity eigenstates \chi_{\lambda}(p) @@ -694,7 +730,8 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi
Floating material and so forth -Consider a task that computes profile parameters for a modified Lorentzian of the form +Consider a task that computes profile parameters for a modified Lorentzian of the form + I=\frac{1}{1+d_{1}^{P(1+d_{2})}} @@ -732,7 +769,8 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi - where + where + d_{1}=\sqrt{\left(\begin{array}{c} \frac{x_{1}}{R_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c} \frac{y_{1}}{R_{min}}\end{array}\right)^{2}} @@ -817,11 +855,14 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi - + + d_{2}=\sqrt{\left(\begin{array}{c} \frac{x_{1}}{PR_{maj}}\end{array}\right)^{2}+\left(\begin{array}{c} -\case{y_{1}}{PR_{min}}\end{array}\right)^{2}}MathML export failed. Please report this as a bug. - +\case{y_{1}}{PR_{min}}\end{array}\right)^{2}} +MathML export failed. Please report this as a bug. + + x_{1}=(x-x_{0})\cos\Theta+(y-y_{0})\sin\Theta @@ -858,7 +899,8 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi - + + y_{1}=-(x-x_{0})\sin\Theta+(y-y_{0})\cos\Theta @@ -951,7 +993,8 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi -, but the assumption is that the alternate results should be less than 90° out of phase with previous values. We have no observations of . Roughly +, but the assumption is that the alternate results should be less than 90° out of phase with previous values. We have no observations of +. Roughly \nicefrac{4}{5} @@ -965,33 +1008,49 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi of the electronically submitted abstracts for AAS meetings are error-free. -We are grateful to V. Barger, T. Han, and R. J. N. Phillips for doing the math in section . More information on the AASTeX macros package are available at http://www.aas.org/publications/aastex or the AAS ftp site. -IRAF, AIPS, Astropy, ... + +We are grateful to V. Barger, T. Han, and R. J. N. Phillips for doing the math in section . More information on the AASTeX macros package are available at http://www.aas.org/publications/aastex or the AAS ftp site. + +IRAF, AIPS, Astropy, ... + + +
-Aurière, M. 1982, , 109, 301 -Canizares, C. R., Grindlay, J. E., Hiltner, W. A., Liller, W., and McClintock, J. E. 1978, , 224, 39 -Djorgovski, S., and King, I. R. 1984, , 277, L49 +Aurière, M. 1982, +, 109, 301 +Canizares, C. R., Grindlay, J. E., Hiltner, W. A., Liller, W., and McClintock, J. E. 1978, +, 224, 39 +Djorgovski, S., and King, I. R. 1984, +, 277, L49 Hagiwara, K., and Zeppenfeld, D. 1986, Nucl.Phys., 274, 1 -Harris, W. E., and van den Bergh, S. 1984, , 89, 1816 +Harris, W. E., and van den Bergh, S. 1984, +, 89, 1816 Hénon, M. 1961, Ann.d'Ap., 24, 369 -King, I. R. 1966, , 71, 276 +King, I. R. 1966, +, 71, 276 King, I. R. 1975, Dynamics of Stellar Systems, A. Hayli, Dordrecht: Reidel, 1975, 99 -King, I. R., Hedemann, E., Hodge, S. M., and White, R. E. 1968, , 73, 456 -Kron, G. E., Hewitt, A. V., and Wasserman, L. H. 1984, , 96, 198 -Lynden-Bell, D., and Wood, R. 1968, , 138, 495 -Newell, E. B., and O'Neil, E. J. 1978, , 37, 27 -Ortolani, S., Rosino, L., and Sandage, A. 1985, , 90, 473 -Peterson, C. J. 1976, , 81, 617 +King, I. R., Hedemann, E., Hodge, S. M., and White, R. E. 1968, +, 73, 456 +Kron, G. E., Hewitt, A. V., and Wasserman, L. H. 1984, +, 96, 198 +Lynden-Bell, D., and Wood, R. 1968, +, 138, 495 +Newell, E. B., and O'Neil, E. J. 1978, +, 37, 27 +Ortolani, S., Rosino, L., and Sandage, A. 1985, +, 90, 473 +Peterson, C. J. 1976, +, 81, 617 Spitzer, L. 1985, Dynamics of Star Clusters, J. Goodman and P. Hut, Dordrecht: Reidel, 109 - - + + - - - + + - - - - - - - + - - - +b + - - - - - - - - - - - - - + + + + + + + + + + + + + - - - - - - - - - - - - - + + + + + + + + + + + + + - - - - - - - - - - - - - + + + + + + + + + + + + + - - - - - - - - - - - - - + + + + + + + + + + + + + - - - - - - - - - - - - - + + + + + + + + + + + + + - - - - - - - - - - - - - + + + + + + + + + + + + + -
Terribly relevant tabular information.Terribly relevant tabular information.
Star Height +Star Height d_{x} @@ -1005,7 +1064,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + d_{y} @@ -1019,7 +1078,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + n @@ -1027,7 +1086,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + \chi^{2} @@ -1041,7 +1100,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + R_{maj} @@ -1057,7 +1116,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + R_{min} @@ -1073,15 +1132,15 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + P P -a +a PR_{maj} @@ -1099,7 +1158,7 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + PR_{min} @@ -1117,113 +1176,126 @@ v(p,\lambda)_{\pm} & = & \pm\lambda(E\mp\lambda|{\textbf{p}}|)^{1/2}\chi + \Theta Θ -bRef.Ref.
1 33472.5 -0.1 0.4 53 27.4 2.065 1.940 3.900 68.3 116.2 -27.6391,2 +1 33472.5 -0.1 0.4 53 27.4 2.065 1.940 3.900 68.3 116.2 -27.6391,2
2 27802.4 -0.3 -0.2 60 3.7 1.628 1.510 2.156 6.8 7.5 -26.7643 2 27802.4 -0.3 -0.2 60 3.7 1.628 1.510 2.156 6.8 7.5 -26.7643
3 29210.6 0.9 0.3 60 3.4 1.622 1.551 2.159 6.7 7.3 -40.2724 3 29210.6 0.9 0.3 60 3.4 1.622 1.551 2.159 6.7 7.3 -40.2724
4 32733.8 -1.2c-0.5 41 54.8 2.282 2.156 4.313 117.4 78.2 -35.8475,6 4 32733.8 -1.2c-0.5 41 54.8 2.282 2.156 4.313 117.4 78.2 -35.8475,6
5 9607.4 -0.4 -0.4 60 1.4 1.669c1.574 2.343 8.0 8.9 -33.4177 5 9607.4 -0.4 -0.4 60 1.4 1.669c1.574 2.343 8.0 8.9 -33.4177
6 31638.6 1.6 0.1 39 315.2 3.433 3.075 7.488 92.1 25.3 -12.052 8 6 31638.6 1.6 0.1 39 315.2 3.433 3.075 7.488 92.1 25.3 -12.052 8
aSample footnote for table  that was generated with the LaTeX table environment
-bYet another sample footnote for table 
-cAnother sample footnote for table 
-We can also attach a long-ish paragraph of explanatory material to a table. Use \tablerefs to append a list of references. The following references were from a different table: I've patched them in here to show how they look, but don't take them too seriously—I certainly have not. -(1) Barbuy, Spite, & Spite 1985; (2) Bond 1980; (3) Carbon et al. 1987; (4) Hobbs & Duncan 1987; (5) Gilroy et al. 1988: (6) Gratton & Ortolani 1986; (7) Gratton & Sneden 1987; (8) Gratton & Sneden (1988); (9) Gratton & Sneden 1991; (10) Kraft et al. 1982; (11) LCL, or Laird, 1990; (12) Leep & Wallerstein 1981; (13) Luck & Bond 1981; (14) Luck & Bond 1985; (15) Magain 1987; (16) Magain 1989; (17) Peterson 1981; (18) Peterson, Kurucz, & Carney 1990; (19) RMB; (20) Schuster & Nissen 1988; (21) Schuster & Nissen 1989b; (22) Spite et al. 1984; (23) Spite & Spite 1986; (24) Hobbs & Thorburn 1991; (25) Hobbs et al. 1991; (26) Olsen 1983. - -
+ +a +Sample footnote for table  that was generated with the LaTeX table environment +
+ +b +Yet another sample footnote for table  +
+ +c +Another sample footnote for table  +
+ +We can also attach a long-ish paragraph of explanatory material to a table. Use \tablerefs to append a list of references. The following references were from a different table: I've patched them in here to show how they look, but don't take them too seriously—I certainly have not. + + +(1) Barbuy, Spite, & Spite 1985; (2) Bond 1980; (3) Carbon et al. 1987; (4) Hobbs & Duncan 1987; (5) Gilroy et al. 1988: (6) Gratton & Ortolani 1986; (7) Gratton & Sneden 1987; (8) Gratton & Sneden (1988); (9) Gratton & Sneden 1991; (10) Kraft et al. 1982; (11) LCL, or Laird, 1990; (12) Leep & Wallerstein 1981; (13) Luck & Bond 1981; (14) Luck & Bond 1985; (15) Magain 1987; (16) Magain 1989; (17) Peterson 1981; (18) Peterson, Kurucz, & Carney 1990; (19) RMB; (20) Schuster & Nissen 1988; (21) Schuster & Nissen 1989b; (22) Spite et al. 1984; (23) Spite & Spite 1986; (24) Hobbs & Thorburn 1991; (25) Hobbs et al. 1991; (26) Olsen 1983. + +
\ No newline at end of file diff --git a/lib/layouts/aastex.layout b/lib/layouts/aastex.layout index 74d2ab6ade..d79cd02d07 100644 --- a/lib/layouts/aastex.layout +++ b/lib/layouts/aastex.layout @@ -179,6 +179,7 @@ Style Affiliation DocBookWrapperTag author DocBookWrapperMergeWithPrevious true DocBookItemTag orgname + DocBookItemTagType paragraph DocBookInInfo always End @@ -207,6 +208,7 @@ Style Altaffilation DocBookWrapperTag author DocBookWrapperMergeWithPrevious true DocBookItemTag orgname + DocBookItemTagType paragraph DocBookInInfo always End @@ -228,6 +230,7 @@ Style Email Shape Italic EndFont DocBookTag email + DocBookTagType paragraph DocBookWrapperTag author DocBookWrapperMergeWithPrevious true DocBookInInfo always