The Relationship Between the Energy Spectra of Anomalous Cosmic Rays and Particles in the Termination Foreshock and Heliosheath

Details The Relationship Between the Energy Spectra of Anomalous Cosmic Rays and Particles in the Termination Foreshock and Heliosheath The Relationship Between the Energy Spectra of Anomalous Cosmic Rays and Particles in the Termination Foreshock and Heliosheath

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh22a..06h&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH22A-06

Physics

7845 Particle Acceleration, 7851 Shock Waves (4455), 7859 Transport Processes, 2104 Cosmic Rays, 2124 Heliopause And Solar Wind Termination

Scientific paper

There are at least three ion populations near the termination shock (TS): (i) termination foreshock particles (FSPs), highly anisotropic, low-energy (~50 keV - 30 MeV) beams in the termination foreshock (TFS) [Krimigis et al., 2003], (ii) heliosheath particles (HSPs), a slowly changing, low-energy population in the heliosheath (HS) [Decker et al. 2005], and (iii) anomalous cosmic rays (ACRs), non-locally accelerated particles with energies above ~30 MeV. At Voyager 1 (V1), the FSPs streamed outward along the nominal Parker spiral field and showed large temporal intensity variations on a ~26 day time scale. In contrast, the spectral change as V1 penetrates deeper into the HS includes a gradual but steady increase in HSP and/or ACR intensities. This slow spectral evolution could be due to easier transport from the ACR source to the spacecraft [Stone et al., 2005], a continual increase in the HSP high-energy role-over arising from an energy cascade process that heats the HSPs [Fisk & Gloeckler, 2006], or perhaps due to progressive sampling of flux tubes deeper in the HS that are connected to higher flux regions in an acceleration region along the heliospheric flanks [McComas & Schwadron, 2006]. We will compare the spectra and composition of the three populations as well as the temporal variation of FSPs and ACRs in the foreshock. We will also discuss potential additional sources of particles at the TS. For instance, we will examine the relationship between the previously reported [Hill et al., 2005] "third source" spectral feature observed in the TFS and the "bulge" now identifiable in HS spectra [Cummings et al., 2005].

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