Ultrahigh Energy Cosmic Rays propagation II

Transcription

1 Ultrahigh Energy Cosmic Rays propagation II The March 6th lecture discussed the energy loss processes of protons, nuclei and gamma rays in interactions with the microwave background. Today I will give you some idea of the results from propagation calculations. Propagation of UHECR protons Propagation of UHE nuclei Propagation of UHE gamma rays But first we will summarize the contant of the previous lecture.

2 Experimental data: The spectra measured by several experiments have absolute normalization different by 40%. Note that the differential flux is multiplied by E 3 to emphasize the shape of the spectrum. The results are obtained with the same hadronic interaction model. The AGASA and HiRes experiments had the highest statistics before Auger Observatory. AGASA shows no end of the cosmic ray spectrum while HiRes does.

3 Astrophysical parameters derived from data before the latest measurements: UHECR source luminosity: 4.5x1044 erg/mpc3/yr between ev for α=2 spectrum (W&B) to 4x1046 (same units) for α=2.7 (BGG). Strong dependence on spectral index and the minimum acceleration energy. UHECR source density: 10-5 Mpc-3 ± order of magnitude: from the clustering of AGASA data set. UHECR source distribution: - isotropic homogeneous + local source + galactic CR - isotropic homogeneous + top-down + galactic CR (no local or top-down sources needed for HiRes) UHECR source cosmological evolution: depends on injection spectrum. Steep spectra require weak cosmological evolution.

4 Cosmic rays of energy above 1020 ev exist, but their flux is not well known. Very few astrophysical objects can accelerate charged nuclei to such energy in shock acceleration processes. Protons and heavier nuclei lose energy in propagation in photoproduction (photodisintegration) on MBR and other photon fields. The sources have thus to be within tens of Mpc from our Galaxy. The other possibility are `top-down' scenarios where these particles are generated in the decay of ultraheavy X-particles, which could be emitted by cosmic strings or are long lived remnants of the early Universe. Not supported by recent data. The current experimental data are not able to give us good indication on the type of these UHECR and their arrival direction distributions. New third (and fourth generation) giant air shower experiments are being built and designed. They will increase the data sample by orders of magnitude and help understanding the nature and sources of these exceptional events.

5 Propagation of UHE protons in CMB photoproduction mean free path

6 for photoproduction and pair production and for adiabatic loss with H0 = 75 km/s/mpc

7 Protons of energy 1021 ev are injected in MBR and are propagated at different distances. The graph shows the energy distribution at arrival. The propagation code simulates the fluctuations in energy loss in photoproduction interactions.

8 Fluctuations are huge at very high proton energy and start decreasing when pair production and adiabatic losses dominate. Higher energy particles lose more energy and energy distributions become tight.

9 Formation of the proton energy spectrum at propagation The injection spectrum is E-2 with an exponential cutoff in this example. Note the formation of a bump after propagation on Mpc. The upper graph is without cosmological evolution of the cosmic ray sources, the lower one is with evolution. In the latter the bump is slightly higher. To obtain the observed spectrum on has to integrate over distance (time).

10 Other possible inputs: cosmic ray luminosity

11 The effect on the observed spectra is much lower because of the decrease of the injection time with redshift (1 + z)-5/2 for EinsteinDeSitter cosmology ( M = 1).

12 In the more general case ( term cosmology) the relation is In contemporary cosmological models M = 0.3 and = 0.7 which represents the dark energy causing the faster expansion of the Universe. The cosmological evolution of the UHECR sources is not very important for the highest energy cosmic rays have such large energy loss that they can only come from cosmologically nearby objects with redshifts smaller than It is very important, though, for the secondary particles generated during propagation.

13 Relation between redshift and distance to an object. The dotted shows uniform expansion of the Universe (which does not agree with the Einstein-De Sitter model.

14 Distance for z = 0.2 as a function of the redshift. Think of this as a decrease of the injection time of the UHECR sources. Since the Universe is expanding the distance/redshift dependence is different at large redshift. Currently z = 0.01 corresponds to a distance of about 40 Mpc. At z = 4.5 this distance is 40 times shorter, only about 1 Mpc.

15 Fitting the observed cosmic ray spectra with protons requires the use of injection spectrum with index steeper than 2.5. Agasa and HiRes spectra versus a calculation of proton primaries after propagation

16 Propagation of UHECR nuclei: one needs to know a lot about nuclear fragmentation. From: Khan et al

17 Results from the propagation calculation of Allard et al for the energy loss length of different nuclei. Vertical lines show the fluctuations from the simulation of the photodisintegration.

18 Fits of the observed cosmic ray spectrum with heavy nuclei accelerated at the cosmic ray sources. Source composition is the same as the galactic chemical composition at 1 GeV. (Allard, Parizot and Olinto)

19 Spectrum of the observed UHECR if the source composition contains different fractions of protons. Spectral index is 2.6. (Allard, Parizot and Olinto)

20 Importance of the extragalactic magnetic fields. Propagation of 100 EeV protons on a distance of 100 Mpc in 1 ng field. Effect will be Z times stronger for heavier nuclei. Scattering angle Time delay

21 Propagation of UHE gamma rays. The gamma rays are injected with energy GeV. The highest pair production cross section is at 3 PeV which causes the dip at that energy. At lower energy the gamma rays interact on the infrared background radiation.