Frontiers of Cosmology
Description
More details
Other editions
Additional editions
Content
Dedication, Preface Acknowledgments;
1 Basics of Cosmology
1. Geometry and Dynamics ; 2.Important quantities needed for observations
3. Some solutions of EFL equations:some cosmological models; 4. The standard Big Bang Nucleosynthesis (SBBN);5. Observations of ``primordial abundances'; 6. Confrontation of the observed ``primordial abundances'' to the predictions of the sBBN; Conclusions; References
2 X-ray View of Galaxy Clusters,
1. Observing Clusters in X-rays -- the Chandra Observatory;2. Regular Clusters XD Cooling Flows A478;3. Physics of Cluster Cores; Acknowledgments; References;
3 Clusters: an optical point of view;
1. Cluster detections in the optical;2. Studies of clusters;3. Acknowledgements;References
4 Cosmology with Clusters;
1. Introduction;2. What is a cluster? ; 3. The spherical model;4. The mass function;
5. Connection to the observations; 6. Properties of Clusters and scaling relations; 7. Clusters abundance evolution; 8. The baryon fraction; 9. Conclusion; References
5 Astrophysical detection of Dark Matter ;
1. Signals from the Dark universe ; 2. Inference probes;3. Physical probes;4. Conclusion; References
6 Non-thermal processes in galaxy clusters ;
1. Non-thermal and relativistic phenomena in galaxy clusters;2. The origin of cosmic rays in galaxy clusters; 3. The astrophysics of cosmic rays in galaxy clusters ; 4. Conclusions; References
7 Cosmological Inflation ;
1. Introduction; 2. The hot Big-Bang scenario and its problems ;3. Inflation and inflationary dynamics;4. Basics of cosmological perturbations ;Synchronous gauge;Longitudinal or Newtonian gauge; Flat-slicing gauge ; 5. Inflationary perturbations; 6. Basics of quantum field theory;7. Perturbation spectrum; 8. Conclusion; References
8 An introduction to quintessence ;
1. The two cosmological constant problems;2. A scalar field asdark energy;3. Stability of the wQ = Const regime ;4. Model building;5. Dark energy and structure formation; 6. Observational status; References
9 CMB Observational Techniques and Recent Results
1. Introduction;2. Observational Techniques ;3. Recent Observations; 4. Summary; Acknowledgments; References;
10 Fluctuations in the CMB ; Andrew H. Jaffe
1. Introduction;2. Cosmological Preliminaries; 3. The Last Scattering Surface ; 4. Perturbations on Large and Small Scales;5. Oscillations in the Primordial Plasma;6. The Power Spectrum of CMB Fluctuations;7. The CMB and Cosmological Parameters;8. Conclusions; Acknowledgments; References
11 Supernovae as astrophysical objects;
1. Some History;2. Supernova classification;3. Input Energy;4. Core-collapse supernovae ;
5. Type Ia supernovae ;6. Conclusions; References
12 Cosmology with Supernovae ;
1. Introduction;2. The Hubble constant;3. The expansion history of the universe;4. Universal acceleration according to Type Ia supernovae ;5. Characterising dark energy ;6. Conclusions; References
13 Gravitational lensing;
1. Introduction;2. Physical mechanisms; Multiple images and displacement field;The amplification matrix ;3. Gravitational lenses in Cosmology;The case of a spherically symmetric mass distribution;Critical lines and caustics in realistic mass distributions; 4. Cosmic Shear: weak lensing as a probe of the large-scale structure;5. Conclusions and perspectives: cosmic shear in a precision;Cosmology era; References
14 Dark Matter ;
1. Introduction;2. Local Dark Matter;3. Clusters and Groups of Galaxies;4. Masses of Galaxies ;
5. The Nature of Dark Matter;6. Summary;Acknowledgments;References
15 Dark Matter and Galaxy Formation;
1. Challenges of dark matter;2. Global baryon inventory;3. Confirmation via detailed census of MWG/M31; 4. Hierarchical galaxy formation;5. Unresolved issues in galaxy formation theory; 6. Resurrecting CDM ;7. An astrophysical solution: early winds;8. Observing CDM via the WIMP LSP; 9. The future ; References
16 Non-Baryonic Dark Matter;
1. The need for non-baryonic dark matter;2. Popular candidates for non-baryonic dark matter; 3. Neutralino dark matter searches; High energy neutrinos from the core of the Sun or of the Earth; Gamma-rays and cosmic rays from neutralino annihilation in galactic halos;Signals from neutralino annihilation at the Galactic Center; 4. Conclusions ; References
It is interesting to evaluate the energy sources of the two explosion mechanisms. Gravity is the drive behind the core-collapse supernovae. The collapse of about 1.5 M to nuclear densities or beyond release about 1053 erg. Most of this energy is radiated in anti-neutrinos, which escape in the formation of neutrons out of protons and electrons. About 1051 erg go into kinetic energy pushing the envelope away and only 1049 erg go into electromagnetic radiation signalling the death of the star across the universe. The thermonuclear explosions draw their energy from the energy difference of the binding energy of oxygen and carbon compared to the iron-peak elements. About one solar mass of O and C are burned and an energy of 1049 erg is released in electro-magnetic radiation.
There are several effects that can in.uence the electro-magnetic display of supernovae. Shocks further convert kinetic energy into radiation. Some of the radiation can not escape the dense explosion and only when the debris expand and adiabatically cool is some of it released. Energy that went into ionising the envelope is released when the material cools down enough so that the atoms recombine again. For supernovae with extended envelope this recombination can create an extended plateau phase in the light curve, where the expansion of the atmosphere is balanced by the inward moving wave of recombination.
One of the best observed examples is SN 1999em Hamuy et al. 2001, Elmhamdi et al. 2003 where the plateau lasted for about 100 days. However, the largest energy reservoir is stored in radioactive isotopes that release ?-rays after typical decay times. The most important channel is the ?-decay of 56Ni into 56Co and then stable 56Fe (e.g. Diehl &, Timmes 1998. For the core-collapse supernovae this channel provides the energy input for the late light curves (after the plateau phase), while it is the only energy input for SNe Ia Leibundgut &, Suntzeff 2003. Bolometric light curves can be used to track the change in escape fraction of the ?-rays from the supernova ejecta Leibundgut. &, Pinto 1992, Contardo et al. 2000.
For massive supernovae the absolute luminosity after about 120 days, together with the age of the supernova, gives a relatively accurate measure of the amount of 56Co synthesised in the explosion Hamuy et al. 2003B, Elmhamdi et al. 2003. This measurement is now available for many core-collapse supernovae and is typically a factor 10 less than assumed in thermonuclear supernovae but spans almost a factor of 100 Pastorello et al. 2004. The long and rich light curve observed for SN 1987A is a clear demonstration of how the various physical effects form the light curve Leibundgut &, Suntzeff 2003. It shows many of the described features and some more.
Hypernovae have been added to the list of supernovae and they represent the high energy end (at least in their kinematics) with the high velocities observed in these objects. The connection of gamma-ray burst with supernovae has now been generally accepted with the observations of SN 2003dh/GRB030329 (e.g. Stanek et al. 2003, Matheson et al. 2003, Hjorth. et al. 2003. It should be noted that already SN 1998bw/GRB980425 showed all the signatures of a supernova Galama et al. 1998, Patat et al. 2001.
