Date: Wed, 5 Sep 2001 11:16:27 +0900 (JST) From: <seki@neutrino.kek.jp> To: opc.nuint01@neutrino.kek.jp Subject: The second draft of Sessions 5 and 6 Message-ID: <Pine.LNX.3.95LJ1.1b3.1010905111105.20600A-100000@neutrino.kek.jp> Folks, The following is my second draft of the proposed Sessions 5 and 6, which is to be discussed at the TV conference at 8:00am on September 8 (in Japan time). Thank you. Seki p.s. I will complete the benchmark list around the middle of the next week and will distribute to you for your suggestions and corrections. ******************************* \documentclass[12pt]{article} \usepackage{epsfig} \addtolength{\textheight}{1in} \addtolength{\textwidth}{1in} \addtolength{\topmargin}{-0.5in} \addtolength{\oddsidemargin}{-0.5in} \pagestyle{empty} \begin{document} \noindent {\bf A. Benchmark MC and Theoretical Calculations of $\nu_\mu-{}^{16}{\rm O}$ Reactions } \begin{itemize} \item Guidelines \begin{itemize} \item Make the binning size as small as possible. \item Draw straight plots (neither semi-log, nor log plots). \item Use the neutrino-nucleon cross section as specified in the attach (not shown yet). \end{itemize} \item[\bf 1. ] $(\nu_\mu,\mu^-)$ inclusive. \\ \begin{itemize} \item[\bf a.] Two figures for $E_\nu =$ 1.0 and 2.0 GeV each\\ $\frac{d\sigma}{d E_\mu}$ as a function of $E_\mu$ from 0 to 1.0 GeV. \item[\bf b.] Two figures for $E_\nu =$ 1.0 and 2.0 GeV each\\ $\frac{d\sigma}{4\pi d(\cos\theta_\mu)}$ as a function of $\theta_\mu$ from 0 to 60 degree. \item[\bf c.] Two figures for $E_\nu =$ 1.0 and 2.0 GeV each\\ $\frac{d^2\sigma}{4\pi d(\cos\theta_\mu)d E_\mu}$ at $\theta_\mu = 30{}^o$ \\ as a function of $E_\nu - E_\mu$ from 0 to 500 MeV. \end{itemize} \item[\bf 2. ] $(\nu_\mu,\mu^-p)$ semi-inclusive\\ \begin{itemize} \item[\bf a.] Two figures for $E_\nu =$ 1.0 and 2.0 GeV each\\ $\frac{d\sigma}{d^3p_p}$ ($d^3\vec{k}_\mu$ integrated) at $\theta_p =$ 60${}^o$ \\ as a function of $|\vec{p}_p|$ from 0 to 500 MeV/c. \item[\bf b.] Two figures for $E_\nu =$ 1.0 and 2.0 GeV each\\ $\frac{d\sigma}{d^3p_p}$ ($d^3\vec{k}_\mu$ integrated) at $|\vec{p}_p|=$ 500 MeV \\ as a function of $\theta_p$from 0 to 90${}^o$. \end{itemize} \item[\bf 3. ] Pion production \begin{itemize} \item (to be shown) \end{itemize} \end{itemize} \bigskip \bigskip \bigskip %\input{bench.tex} % % % figure % \begin{picture}(0,0)% \epsfig{file=bench.ps,scale=0.5}% \end{picture}% %\setlength{\unitlength}{3947sp}% \setlength{\unitlength}{2000sp}% % \begingroup\makeatletter\ifx\SetFigFont\undefined% \gdef\SetFigFont#1#2#3#4#5{% \reset@font\fontsize{#1}{#2pt}% \fontfamily{#3}\fontseries{#4}\fontshape{#5}% \selectfont}% \fi\endgroup% \begin{picture}(6143,3597)(1455,-3433) \put(7201,-3361){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\vec{p}_p$}}} \put(1951,-961){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\nu$}}} \put(5476,-361){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\mu^-$}}} \put(5776,-1261){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\theta_\mu$}}} \put(7501,-136){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\vec{k}_\mu$}}} \put(5926,-2011){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$\theta_p$}}} \put(5551,-2986){\makebox(0,0)[lb]{\smash{\SetFigFont{20}{24.0}{\rmdefault}{\mddefault}{\updefault}$p$}}} \end{picture} \vfill\eject \noindent {\bf B. Format and List of Participants } \begin{itemize} \item Guidelines \begin{itemize} \item Keep showing all (or as many as possible) relevant plots for comparison by using as many projected screens as possible. \item Also use one standard OHP for lay-over presentations as needed during the two sessions. \item Accept as many comments and questions as possible from the audience at any time during the sessions. \end{itemize} \item {\bf Session 5.} (Chair, Seki; Associate Chair, Y. Hayato) (3 hours +)\\ Results of the benchmark calculations are presented by: \begin{itemize} \item 1. Presentation of Monte Carlo results (1.5 hours) \begin{itemize} \item NEUT \item NUANCE \item MINOS/Soudan II \item OPERA/NOMAD/DONUT \item A brief summary of MC results \end{itemize} \item 2. Theoretical calculations (1 hour +) \begin{itemize} \item J. Marteau \item E. Paschos \item H. Nakamura \item plus? \end{itemize} \item 3. Summary of comparison of benchmark calculations (MC+Theory)(0.5 hours) \end{itemize} \item {\bf Session 6.} (Chair, Seki; Associate Chair, D. Casper) (3.5 hours)\\ Panel discussions are carried out by: \begin{itemize} \item Y. Hayato \item K. Kaneyuki \item V. R. Pandharipande \item P. Vogel \item K. Kubodera \item K. Langanke \item G. Garvey \item plus? Especially on resonances and DIS. \end{itemize} The following six issues are discussed. An leader is assigned for each issue, who is responsible to come up with consensus among the panelers and the audiance on the current status of the issue in 30 minutes. For each topic, the leaders are first to describe his view of the issue briefly (say, 5-10 minutes), and discussions are to follow it. The leaders will be responsible to write a summary for the proceedings. Tentative leaders are listed in parentheses. \begin{itemize} \item In MC environment for ($\nu$, $\ell$) and ($\nu$,$\ell p$) (separately): \begin{itemize} \item [\bf 1.] How should Fermi gas model be applied and made realistic? (Vogel) \item [\bf 2.] How important nuclear correlations are and how should be incorporated, and how the final-state interactions are best treated? (Pandharipande) \item[\bf 3.] How should the pion production be treated? (Hayato/Kaneyuki) \end{itemize} \item As an item which is uncertain but likely to have practical consequences: \begin{itemize} \item [\bf 4.] How vector current is made to be conserved in nuclei, off-shell effects should be treated, and how the axial currents and form factors are modified in nuclei? (Kubodera) \item [\bf 5.] Re: resonances/DIS (what and who?) \item [\bf 6.] Re: DIS (what and who?) \end{itemize} \item [\bf 7.] The "standard" neutrino-nucleus MC code. (Casper) The questions are to be addressed: \begin{itemize} \item Whether and how such a code be constructed? \item What is its scope (reaction processes and energies etc. to be covered)? \item What ingredients (physics) should such code(s) includes? \item Who would actually do the work? \end{itemize} \end{itemize} \end{itemize} \end{document}
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