%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % template.tex: template for camera.cls/camera.sty: % camera-ready papers (Societ\`a Italiana di Fisica) % 1997/03/18 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % If you have LaTeX2e, replace the line below with: % \documentclass{camera} % If you don't know which version of LaTeX you have, % leave it as it is and try it out; if it doesn't work, % try with \documentclass. % If you really want to know which version of LaTeX % you have, just % 1. typeset this (or any other file) with the command % latex camera % 2. ignore the errors % 3. search among the first lines of output for % a line such as % LaTeX2e <1996/06/01> % or % LaTeX Version 2.09 <25 March 1992> % \documentstyle{camera} % if you have landscape tables % put your own definitions here: % \newcommand{\cZ}{\cal{Z}} % \newtheorem{def}{Definition}[section] % ... \newcommand{\ttbs}{\char'134} \newcommand{\AmS}{{\protect\the\textfont2 A\kern-.1667em\lower.5ex\hbox{M}\kern-.125emS}} \newcommand{\ud}{\mathrm{d}} \newcommand{\beq}{\begin{equation}} \newcommand{\eeq}{\end{equation}} \newcommand{\bea}{\begin{eqnarray}} \newcommand{\eea}{\end{eqnarray}} \newcommand{\iii}{\mathrm{i}} \newcommand{\der}{\mathrm{d}} \newcommand{\Ima}{\mathrm{Im}} \newcommand{\Rea}{\mathrm{Re}} \newcommand{\JoB}{\mathrm{J_0}} \newcommand{\eex}{\mathrm{e}} \newcommand{\lambdabar}{\lambda\!\!\bar{ }\ } \newcommand{\dummy}[2]{\begin{array}{c} #1\\#2 \end{array} } \newcommand{\bino}[2]{\left ( \begin{array}{c} #1\\#2 \end{array} \right )} \newcommand\nutau{{\nu_\tau}} \newcommand\anutau{\bar\nu_\tau} \newcommand\numu{{\nu_\mu}} \newcommand\anumu{\bar\nu_\mu} \newcommand\nue{{\nu_e}} \newcommand\anue{\bar\nu_e} \newcommand{\Reg}{I\!R} \newcommand{\Pom}{I\!P} \newcommand{\fx} {$F(x)=\frac{1}{\sigma}\frac{2E_{CM}}{\pi\sqrt s}\frac{\der \sigma} {\der x_F}$} \newcommand{\FLUKA}{{\sc FLUKA}} \newcommand{\PEANUT}{{\sc PEANUT}} \newcommand{\DPMJET}{{\sc DPMJET}} \def\dm2{\Delta m^2} \def\sq2{sin^2(2\Theta)} \def\nubar{\overline {\nu} } \def\aprle{\buildrel < \over {_{\sim}}} \def\aprge{\buildrel > \over {_{\sim}}} \def\to{\rightarrow} \def\pep{$p\to e^+\pi^0$} \def\pkn{$p\to \bar{\nu}K^+$} \def\ra{\rightarrow} % add words to TeX's hyphenation exception list \hyphenation{author another created financial paper re-commend-ed Post-Script} \input epsf \begin{document} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % The title, all uppercase; if you want to split it in % two or more lines, put a \\ macro at each line break % example: % \title{TITLE: FIRST LINE\\ SECOND LINE} % \title{EXAMPLE OF A PAPER PRESENTED AT THE VULCANO WORKSHOP 2004: FRONTIER OBJECTS IN ASTROPHYSICS AND PARTICLE PHYSICS} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % The Author(S), Separated By Commas; Do not put a % comma before the last author, use instead the \And % macro which produces a normal ``and'' in the % caps/small caps context % \author{FRANCO GIOVANNELLI} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % \organization{Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR\\ Area di Ricerca di Roma-2, Via del Fosso del Cavaliere, 100 - I 00133, Roma, Italy} \maketitle \begin{abstract} In this paper I would like to discuss several hot points of today astroparticle physics. \end{abstract} \vspace{1.0cm} \section{Introduction} In the last few decades, cosmic-ray physics and high energy astrophysics strongly developed thanks to ground- and space-based experiments. Higher and higher capabilities in reproducing extreme conditions in which the nature demonstrates, and better and better sensitivities of the detectors used have been the key of such a development. \section{Cosmology} Modern physical cosmology has now converged on the Big Bang framework. Such a framework is supported by four principal pillars: \begin{itemize} \item Hubble expansion \item microwave background \item light element abundances \item inflation \end{itemize} \subsection{Hubble Expansion} The absolute magnitude M of the galaxies can be determined through the measurement of the apparent magnitude m and redshift z. \subsubsection{Title of the Subsubsection} Please write the text of the subsubsection. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{figure}[h!] %%% FIGURE 1 %%% \epsfysize=5cm \hspace{4.0cm} \epsfbox{CMBR_T_vs_z.PS} \vspace{0.3cm} \caption[h]{CMBR temperature versus redshift (Srianand, Petitjean \& Ledoux, 2000). {\bf We want the Figure 1 just here, then it is necessary to use the command [h!].}} \end{figure} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \section{Active Galactic Nuclei and Galactic Collapsed Objects: Unified Schemes} The main idea in order to explain the emission from extragalactic X-ray emitters, now very popular, was suggested many years ago (Giovannelli \& Polcaro, 1986): the {\it engine} producing high energy radiation is of the same kind for all extragalactic emitters. Mass and mass accretion rates are the unique parameters differentiating extragalactic emitters, containing central black holes, by the galactic black holes. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{figure}[t!] %%% FIGURE 2 %%% \epsfysize=10cm \hspace{1.0cm} \epsfbox{COLLIDING-GALAXIES_CHANDRA.ps} \vspace{0.3cm} \caption[h]{Image of the Antennae colliding galaxies obtained with the Chandra observatory. It shows superbubbles produced by the combined effect of thousands of supernovae, as well as dozens of bright point-like sources produced by neutron stars and black holes (NASA/SAO/Fabbiano, Zezas \& Murray, 2001). {\bf We want the Figure 2 at the top of page, then it is necessary to use the command [t!].} } \end{figure} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% More detailed unified schemes have been produced. For instance, in Vagnetti, Cavaliere \& Giallongo (1991) and Vagnetti \& Spera (1994) and in the references therein, the evolutionary unified scheme is based on the changing balance among three optical luminosities, namely: \begin{itemize} \item nuclear isotropic component; \item relativistic beam component; \item host galaxy component. \end{itemize} The intrinsic jet luminosity is assumed to have the same cosmic evolution as the nuclear isotropic component. The bulk Lorentz factor of the beam is able to account for the slower evolution of flat-spectrum QSOs. The comparison of the total nuclear luminosity ($L_{NUC} = L_{IS} + L_{BEAM}$) with the non-evolutionary galactic luminosity, ($L_{HG}$), predicts the appearance of a source as a radio galaxy if $L_{HG} > L_{NUC}$. \begin{figure}[t!] \vspace{10truecm} \special{psfile=M51_LARGE_SCALE_B.ps voffset=140 hoffset=0 hscale=30.0 vscale=18.7 angle=0} \special{psfile=M83_LARGE_SCALE_B.ps voffset=141 hoffset=220 hscale=18.0 vscale=18.5 angle=0} \special{psfile=NGC4631_B_2-8cm.ps voffset=-8 hoffset=35 hscale=18.3 vscale=20 angle=0} \special{psfile=M82_B_VLA.ps voffset=0 hoffset=220 hscale=18 vscale=18.2 angle=0} \caption[h]{The magnetic field structures of different galaxies. Clockwise from the left upper panel: orientation of the large-scale magnetic fields in M51, orientation of the large-scale magnetic fields in M83 (Neininger et al., 1991), magnetic fields in NGC 4631 from 2.8 cm observations (Wielebinski \& Krause, 1993), and magnetic fields in M82 from VLA observations (Reuter et al., 1993). {\bf The use of the commands for this composed figures is rather simple. It is necessary to vary "voffset" and "hoffset" in order to move each figure in vertical and in horizontal, respectively. It is necessary to vary "hscale" and "vscale" in order to resize each figure in horizontal and in vertical, respectively. With the command "angle" it is possible to rotate a figure.}} \label{fig1} \end{figure} Table 1 shows 28 GRBs detected by different satellites, for which the redshifts of the {\it host galaxies} have been determined (Djorgovski et al., 2001; Greiner, 2002). \begin{table}[t!] \begin{center} \caption{Gamma-ray bursts, detected by different satellites and the redshifts of the host galaxies (Djorgovski et al., 2001; Greiner, 2002)} \bigskip \begin{tabular}{lll} \hline GRB Name & Host-Galaxy Redshift & Localization Source\\ \hline 970228 & $0.625 \pm 0.002$ & BeppoSAX\\ 970508 & 0.835 & BeppoSAX\\ 970828 & 0.9579 & RXTE/ASM\\ 971214 & 3.418 & BeppoSAX\\ 980326 & 1 ? & BeppoSAX\\ 980329 & < 3.9 & BeppoSAX\\ 980425 & 0.0085 & BeppoSAX\\ 980613 & $1.0964 \pm 0.0003$ & BeppoSAX\\ 980703 & $0.9660 \pm 0.0002$ & RXTE/ASM\\ 990123 & $1.6004 \pm 0.0005$ & BeppoSAX\\ 990506 & 1.3 & BATSE/PCA\\ 990510 & $1.619 \pm 0.002$ & BeppoSAX\\ 990705 & 0.86 & BeppoSAX\\ 990712 & $0.430 \pm 0.005$ & BeppoSAX\\ 991208 & $0.7055 \pm 0.0005$ & IPN\\ 991216 & 1.020 & RXTE/PCA\\ 000131 & 4.50 & Uly/KO/NE (IPN)\\ 000214 & 0.37-0.47 & BeppoSAX\\ 000301C & $2.0335 \pm 0.0003$ & RXTE/ASM+IPN\\ 000418 & $1.1185 \pm 0.0007$ & IPN\\ 000911 & 1.0585 & IPN\\ 000926 & 2.0369 & Uly/KO/NE (IPN)\\ 001109 & 0.37 & BeppoSAX\\ 010222 & 1.477 & BeppoSAX\\ 010921 & 0.45 & HETE/Uly/BeppoSAX\\ 011121 & 0.36 & BeppoSAX\\ 011211 & 2.14 & BeppoSAX\\ 020405 & 0.69 & Uly/MO/BeppoSAX\\ %020813 & 1.25 & HETE\\ %021004 & 2.3 & HETE\\ %021211 & 1.01 & HETE\\ %030226 & 1.98 & HETE\\ \hline \end{tabular} \end{center} \end{table} \section{X-Ray Binaries} X-ray binary systems are a cauldron of physical processes and their multi-frequency studies improved a lot the knowledge of the accreting processes onto collapsed objects. \section{Radio Pulsars, Millisecond Pulsars} The observable quantities are the rotational period $P$ and the spin-down rate $\dot{P}$. Then substituting these quantities to $\Omega$ and $\dot{\Omega}$, it is possible to express the pulsar magnetic field in terms of the observable quantities, by using typical values for the moment of inertia and the radius of the neutron star (Zi{\'o}{\l}kowski, 1997): $$B = 3.2 \times 10^{19}(P\dot{P})^{1/2}G\,. \hspace{2.0cm} (8.3)$$ \noindent The rate of energy loss is (Thompson, 2000): $$\dot{E} \simeq 4 \times 10^{46}\dot{P}P^{-3}\, erg\, s^{-1}\,. \hspace{2.0cm} (8.4)$$ \noindent The line open field line voltage is (Thompson, 2000): $$V \simeq 4 \times 10^{20}\dot{P}^{1/2}P^{-3/2}\, V \simeq \dot{E}^{1/2}\,. \hspace{2.0cm} (8.5)$$ %%%%%% Table 2 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% \begin{table}[h!] \begin{center} \caption{Black holes in the Milky Way Galaxy (Blandford \& Gehrels, 1999; Filippenko et al., 1999; Casares, 2001) } \bigskip \begin{tabular}{llllll} \hline Source Name & Identification &Companion&f(M)&$M_{Opt}$ & $M_{BH}$ \\ & & & &($M_\odot$)&($M_\odot$)\\ \hline Cygnus X-1 & HD226868 & O9.7 Iab & 0.24 & 24-42 & 11-21\\ GS2023+338 & V404 Cyg & K0 IV & 6.26 & $\sim 0.6$ & 10-15\\ GS2000+25 & QZ Vul & K3-K5 V & 4.97 & $\sim 0.7$ & 6-14\\ H1705-250 & V2107 Oph & K3 & 4.86 & 0.3-0.6 & 6.4-6.9\\ GROJ1655-40 & N Sco 1994& F6 IV & 3.24 & 2.34 & 7.02\\ A0620-00 & V616 Mon & K3-K5 V & 3.18 & 0.2-0.7 & 5-10\\ GS1124-68 & GU Mus & K3-K4 V & 3.10 & 0.5-0.8 & 4.2-6.5\\ GROJ0422+32 & V518 Per & M2 V$\pm2$ & 1.21 & $\sim 0.3$ & 6-14\\ 4U1543-47 & & A2 V & 0.22 & $\sim 2.5$ & 2.7-7.5\\ GRS1009-45 & N Vel 1993& K8 V$\pm2$ & 3.17 & $\sim 0.6$ & 4.4\\ \hline \end{tabular} \end{center} \end{table} %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% Although no single model for high-energy emission from pulsars has emerged, the observations with the present generation of high-energy telescopes have channelled all models in certain directions: \begin{itemize} \item the particle acceleration by the strong electric fields takes place somewhere above the magnetic poles; \item the principal high-energy emission processes are synchrotron radiation, curvature radiation, and inverse Compton scattering, with thermal-emission secondary contributor; \item the high-energy pulsed emission is probably associated with a single magnetic pole of the neutron star. \end{itemize} \smallskip \noindent Thompson (2000) pointed out several open questions about spin-down pulsars: \begin{itemize} \item Where in the magnetosphere are the particles accelerated? \item What is the shape of the beam? \item Are there many more radio-quiet pulsars to be found in X-rays and $\gamma$-rays? \item How do these recent discoveries affect our thinking about supernovae and neutron star formation? \end{itemize} \smallskip \noindent These open questions can be solved by improving the studies of the X-ray archives of the ROSAT, ASCA, BeppoSAX, and RXTE, while AXAF-Chandra, and XMM-Newton will give significant improvements in sensitivity and resolution. In the $\gamma$-ray range, the study of the CGRO archives and the new data from the INTEGRAL mission will help in filling some gaps in such a low-energy $\gamma$-ray band. The next major step in high-energy $\gamma$-rays will come with the GLAST experiment (e.g. Kamae, et al., 2000). \section{Conclusions} In this paper I have discussed several of the most important problems of astroparticle physics today and the hot questions still open have been remarked. \section{Acknowledgements} This work was partially supported by the European Community. Many thanks to Drs Black and White for useful discussions. \begin{thebibliography}{9} \bibitem{} {\bf We strongly recommend to insert in the text the references with the name of the author and the date, like (Beall, 2002) or following the results obtained by Baade \& Zwicky (1934) or, in the case of three authors we suggest to write the three names (Beall, Guillory \& Rose, 1999). For more than three authors please use: following the paper by Atkins et al. (2000) we can deduce..... or: the result of this measurement has been used for obtaining a new model of the system (Bednarek et al., 1990). We strongly recommend to write the references in this section in alphabetical order. It is much easier to find them in any moment!} \bibitem{} Atkins, R., Benbow, W., Berley, D., Chen, M.L., Coyne, D.G., Dingus, B.L., Dorfan, D.E., Ellsworth, R.W., Evans, D., Falcone, A., Fleysher, L., Fleysher, R., Gisler, G., Goodman, J.A., Haines, T.J., Hoffman, C.M., Hugenberger, S., Kelly, L.A., Leonor, I., McConnell, M., McCullough, J.F., McEnery, J.E., Miller, R.S., Mincer, A.I., Morales, M.F., Nemethy, P., Ryan, J.M., Shen, B., Shoup, A., Sinnis, C., Smith, A.J., Sullivan, G.W., Tumer, T., Wang, K., Wascko, M.O., Westerhoff, S., Williams, D.A., Yang, T., Yodh, G.B.: 2000, {\it Astrophys. J. Letters} {\bf 533}, L119. \bibitem{} Baade, W. and Zwicky, F.: 1934, {\it Phys. Rev.} {\bf 45}, 138. \bibitem{} Backer, D., Kulkarni, S., Heiles, C., Davis, M., Goss, M.: 1982, {\it IAU Circ.} {\bf No. 3743}. \bibitem{} Bailes, M., Lorimer, D.: 1995, in {\it Millisecond Pulsars. A Decade of Surprise}, A.S. Fruchter, M. Tavani \& D.C. Backer (eds.), ASP Conference Series {\bf 72}, 17. \bibitem{} Baring, M.G., Harding, A.K.: 1997, in {\it Proceedings of the Fourth Compton Symposium}, C.D. Dermer, M.S. Strickman \& J.D. Kurfess (eds.), AIP Conf. Proc. {\bf 410}, 638. \bibitem{} Bartolini, C., Beskin, G.M., Guarnieri, A., Masetti, N., Piccioni, A.: 1998, in {\it Gamma-Ray Bursts}, C.A. Meegan, R.D. Preece \& T.M. Koshut (eds.), AIP Conference Proceedings {\bf 428}, 540. \bibitem{} Beall, J.H.: 2002, in {\it Multifrequency Behaviour of High Energy Cosmic Sources}, F. Giovannelli \& L. Sabau-Graziati (eds.), {\it Mem. S.A.It.} {\bf 73}, 379. \bibitem{} Beall, J.H., Guillory, J., Rose, D.V.: 1999, in {\it Multifrequency Behaviour of High Energy Cosmic Sources}, F. Giovannelli \& L. Sabau-Graziati (eds.), {\it Mem. S.A.It.} {\bf 70}, 1235. \bibitem{} Becker, W.: 2000, {\it Adv. Space Res.} {\bf 25}, 647. \bibitem{} Becker, W., Tr\'{u}mper, J.: 1997, {\it J. Astron. Astrophys.} {\bf 326}, 682. \bibitem{} Becker, W., Tr\'{u}mper, J.: 1997, {\it J. Astron. Astrophys.} {\bf 326}, 682. \bibitem{} Becker, W., Tr\'{u}mper, J.: 1998, in {\it The Many Faces of Neutron Stars}, R. Buccheri, J. van Paradijs \& M. A. Alpar (eds.), Kluwer Academic Publ., p. 525. \bibitem{} Bednarek, W., Giovannelli, F., Karakula, S., Tkaczyk, W.: 1990, {\it Astron. Astrophys.} {\bf 236}, 268. \bibitem{} Bednarek, W., Giovannelli, F.: 1999, in {\it Multifrequency Behaviour of High Energy Cosmic Sources}, F. Giovannelli \& L. Sabau-Graziati (eds.), {\it Mem. S.A.It.} {\bf 70}, 1071. \bibitem{} de Bernardis, P., Ade, P.A.R., Bock, J.J., Bond, J.R., Borrill, J., Boscaleri, A., Coble, K., Crill, B.P., De Gasperis, G., Farese, P.C., Ferreira, P.G., Ganga, K., Giacometti, M., Hivon, E., Hristov, V.V., Iacoangeli, A., Jaffe, A.H., Lange, A.E., Martinis, L., Masi, S., Mason, P.V., Mauskopf, P.D., Melchiorri, A., Miglio, L., Montroy, T., Netterfield, C.B., Pascale, E., Piacentini, F., Pogosyan, D., Prunet, S., Rao, S., Romeo, G., Ruhl, J.E., Scaramuzzi, F., Sforna, D., Vittorio, N. : 2000, {\it Nature} {\bf 404}, 955. \bibitem{} Bhattacharya, D.: 1995, {\it J. Astron. Astrophys.} {\bf 16}, 217. \bibitem{} Bildsten, L., Strohmayer, T.: 1999, in {\it Physics Today} {\bf 52, No. 2}, 40. \bibitem{} Bisnovatyi-Kogan, G.: 2002, in {\it Multifrequency Behaviour of High Energy Cosmic Sources}, F. Giovannelli \& L. Sabau-Graziati (eds.), Mem. S.A.It. {\bf 73}, 357. \bibitem{} Fabbiano, G., Zezas, A., Murray, S.S.: 2001, {\it Astrophys. J.} {\bf 554}, 1035. \bibitem{} Feroci, M.: 2001, in {\it Frontier Objects in Astrophysics and Particle Physics}, F. Giovannelli \& G. Mannocchi (eds.), Italian Physical Society, Editrice Compositori, Bologna, Italy, {\bf 73}, 287. \end{thebibliography} \bigskip \bigskip \noindent {\bf DISCUSSION} \bigskip \noindent {\bf MARIO MACRI:} Can you comment on the contribution of Antimatter search in space experiments to the understanding of cosmological evolution? \bigskip \noindent {\bf FRANCO GIOVANNELLI:} The detection of exotic cosmic rays due to pair annihilation of dark matter particles in the Milky Way halo is a viable techniques to search for supersymmetric dark matter candidates. The study of the spectrum of gamma-rays, antiprotons and positrons offers good possibilities to perform this search in a significant portion of the Minimal Supersymmetric Standard Model parameter space. .............. \bigskip \noindent {\bf JAMES WHITE's Comment:} I would like to remind that.......... \end{document}