Voyager Observations of Anomalous Cosmic Rays in the Outer Heliosphere

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Voyager Observations of Anomalous Cosmic Rays in the Outer Heliosphere ICRC 8/15/11 A. C. Cummings, E. C. Stone, F. B. McDonald, B. C. Heikkila, N. Lal, W. R. Webber

McComas and Schwadron (2006) picture V2 ACR intensities would be expected to be higher than those at V1 because closer to source region along flanks of shock. See also Kota 2007 for similar picture with source on tail of shock. V2 high intensity V1 low

TSP TSP ACR TSP ACR ACR GCR GCR GCR TSP spectrum normalized at low energies to estimate TSP contributions at higher energies Thanks to LECP team for low-E Ions, He, and O data

a= -0.70; b= -3.14; E0= 3.27 MeV

V1 H V1 H V2 H TSP intensities very similar at V1 and V2 until 2010 0.035 0.35 1.0 1.6 TSP intensities very similar at V1 and V2 until 2010 Recent V1 decrease due to transient of leakage out heliosphere? Not observe expected energy dependence

V1 H TSPs dominate through mid 2007 1.8 TSPs dominate through mid 2007 Then ACRs begin appearing above ~3 MeV Do increasing ACRs mask a decrease in TSPs at 2 to 3 MeV? 2.2 3.0 4.6 6.2

V1 H V1 H Higher energy ACRs appear earlier as expected

Large ACR intensity increase at V2 over last year; small decrease at V1 V2 intensity > V1 intensity Region of strong gradient 92-95 AU at V2? Latitudinal, longitudinal, dynamical?

07 08 09 10 11 12 V1 ACR O intensities peaked in 2010 ~25% decease at higher, ~15% at lower energy Particles could be leaking out heliopause Not expect if ACR source near heliopause ACR O intensities now ~2x higher at V2 than at V1 and at an all-time high. ACR source higher in south than in north? ACR source at shock on flanks or tail? (McComas and Schwadron; Kota) Recovery from transient that began ~ 2009.2 may contribute to the V2 intensity increase Origin of V2 decrease not known 07 08 09 10 11 12

07 08 09 10 11 12 V1 ACR O intensities peaked in 2010 ~25% decease at higher energy, ~15% at lower Particles could be leaking out heliopause Not expect if ACR source near heliopause ACR O intensities now ~2x higher at V2 than at V1 and at an all-time high. ACR source higher in south than in north? ACR source at shock on flanks or tail? (McComas and Schwadron; Kota) Recovery from transient that began ~ 2009.2 may contribute to the V2 intensity increase Origin of V2 decrease not known 07 08 09 10 11 12

Evidence for 2008 transient but not in 2009 No significant change in plasma at time of 2010 increase Vsw 2008 2009 2010 2011 Richardson et al.

V2 No consistent correlation with unipolar (U) or sector (S) regions V2 > V1 is expected if ACR source is on the flanks (McComas et al., Kota) Vsw 2008 2009 2010 Burlaga e al. 2011

V2 ACR H and He intensities have exceeded V1 ACR intensities by ~40% in several energy bands in early 2011. Now approaching 100%

Free Escape Boundary V2 V1 Kota & Jokipii ICRC 2011

ACRs intensity at V1 has decreased from intensity peak in 2009 Summary ACRs intensity at V1 has decreased from intensity peak in 2009 Suggests source is not beyond 112 AU in nose region Larger ACR O decrease at higher energies Suggestive of diffusive loss out of nearby heliopause Transient effect at V1? ACR intensity rapidly increased at V2, is now up to ~2x V1 V2 is 22 AU closer to sun than V1 V1 is on nose meridian, V2 is closer to flank Consistent with source on flanks on at tail (McComas & Schwadron; Kota) Latitudinal or dynamical origin?