Heavy nuclei enrichment of the galactic cosmic rays at high energy: astrophysical interpretation

Maurin, D.; Cassé, Michel; Vangioni‐Flam, Elisabeth

doi:10.1016/s0927-6505(02)00163-9

Cited by 14 publications

(24 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The difference observed in Fig. 7 between small (lower panels) and large δ (upper panels) is readily explained: a large value of δ also corresponds to a large value of K 0 (see Maurin et al (2003) for details), so that a greater wind is needed in order to prevent from too many spallations occurring at low energy. The net result is that the wind blow the particles away, reducing the effective zone from where they come from.…”

Section: Antiprotons and Antideuteronsmentioning

confidence: 98%

Spatial origin of Galactic cosmic rays in diffusion models

Maurin

Taillet

2003

A&A

View full text Add to dashboard Cite

Abstract. In a companion paper, we investigated the question of the spatial origin of the cosmic rays detected in the Solar neighborhood, in the case of standard sources located in the Galactic disk. There are some reasons to believe that there may also be a large number of sources located in the halo, for example if the Galactic dark matter is made of supersymmetric particles or if Primordial Black Holes are present. These exotic sources could enhance thep,d or positrons above the standard background, indicating the existence of new physics. The spatial distribution of these hypothetical sources, though an important ingredient to evaluate these exotic signals, is poorly known. The aim of this paper is to point out that this discussion should not be disconnected from that of the propagation properties in the Galaxy. More precisely, we determine the regions of the halo from which a significant fraction f of cosmic rays antiprotons and antideuterons detected in the Solar neighborhood were emitted (we refer to these regions as f -volumes), for different sets of propagation parameters consistent with B/C data, as derived in Maurin et al. (2002). It is found that some of them lead to rather small f -volumes, indicating that the exotic cosmic rays could have a local origin (in particular for a small diffusive halo or a large Galactic convective wind), coming from the Solar neighborhood or the Galactic center region. It is also found that the dark matter density enhancement (spike) due to the accretion around the central supermassive black hole gives a negligible contribution to the exotic charged particle signal on Earth. The case of electrons and positrons is also discussed.

show abstract

Section: Antiprotons and Antideuteronsmentioning

confidence: 98%

Spatial origin of Galactic cosmic rays in diffusion models

Maurin

Taillet

2003

A&A

View full text Add to dashboard Cite

show abstract

“…A detailed study shows that there is some degeneracy among the parameters of the propagation model. This can be used to decrease the size of L and thereby reduce the antiproton flux from gravitino decays relative to the flux from spallation [40]. The solution of the transport equation at the Solar System, r = r ⊙ , z = 0, can be formally expressed by the convolution…”

Section: Jcap09(2009)021mentioning

confidence: 99%

Probing gravitino dark matter with PAMELA and Fermi

Buchmüller

Ibarra

Shindou

et al. 2009

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Abstract. We analyse the cosmic-ray signatures of decaying gravitino dark matter in a model-independent way based on an operator analysis. Thermal leptogenesis and universal boundary conditions at the GUT scale restrict the gravitino mass to be below 600 GeV. Electron and positron fluxes from gravitino decays, together with the standard GALPROP background, cannot explain both the PAMELA positron fraction and the electron + positron flux recently measured by Fermi LAT. For gravitino dark matter, the observed fluxes require astrophysical sources. The measured antiproton flux allows for a sizable contribution of decaying gravitinos to the gamma-ray spectrum, in particular a line at an energy below 300 GeV. Future measurements of the gamma-ray flux will provide important constraints on possible signatures of decaying gravitino dark matter at the LHC.

show abstract

“…The change of the cosmic ray mass composition at the knee region is often explained as a result of rigidity dependent acceleration causing heavy nuclei start to dominate at higher energies (Peters 1961). The heavy nuclei enrichment of the galactic CRs might be also due to propagation effects in the galactic disk and halo (e.g., Maurin et al 2003). Moreover, a contribution of another type of sources to CRs above the knee region, e.g.…”

Section: Introductionmentioning

confidence: 99%

Cosmic rays from Galactic pulsars

Bednarek¹,

Bartosik²

2004

A&A

View full text Add to dashboard Cite

Abstract. We calculate energy spectra and mass composition of cosmic rays accelerated by the galactic population of pulsars during their radio and gamma-ray phase. It is assumed that a significant part of the pulsar rotational energy is lost on acceleration of iron nuclei extracted from the surface of the neutron star. The nuclei are accelerated, at first when passing the outer gap of the inner pulsar magnetosphere and later in the pulsar wind zone, to energies corresponding to 50% of the total potential drop through the polar cap region of the neutron star. We calculate energy spectra of the nuclei injected from the pulsar wind nebulae into the Galaxy including different energy loss processes of nuclei during their propagation in the pulsar magnetosphere and the expanding nebula, their fragmentation in collisions with radiation and matter, adiabatic energy losses, and escape from the nebula. Several models proposed for the distribution of the initial parameters of the galactic pulsar population are considered. It is shown that the best description of the observed cosmic ray spectrum and the mass composition between a few 10 15 eV and a few 10 18 eV is obtained for the model B of Lorimer et al., in which the logs of initial pulsar periods and surface magnetic fields are given by the Gaussian distributions with the average values of log P[ms] = 2.6 and log B[G] = 12.3, respectively. In order to supply the cosmic rays into the Galaxy with the required rate, the product of the efficiency of cosmic ray acceleration by pulsars and their birth rate should be about 10 −2 yr −1 .

show abstract

Heavy nuclei enrichment of the galactic cosmic rays at high energy: astrophysical interpretation

Cited by 14 publications

References 53 publications

Spatial origin of Galactic cosmic rays in diffusion models

Spatial origin of Galactic cosmic rays in diffusion models

Probing gravitino dark matter with PAMELA and Fermi

Cosmic rays from Galactic pulsars

Contact Info

Product

Resources

About