Voyager Observations in the Heliosheath: An Overview

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Presentation transcript:

Voyager Observations in the Heliosheath: An Overview ICRC 8/15/11 E. C. Stone A. C. Cummings

Plasma Science (Voyager 2) J.D. Richardson, J. W. Belcher, L. F. Burlaga, A.J. Lazarus, R. McNutt, E.C. Sittler, Jr., C. Wang Low-Energy Charged Particles S.M. Krimigis, T.P. Armstrong, R.B. Decker, G. Gloeckler, D.C. Hamilton, L.J. Lanzerotti, B.H. Mauk, R. McNutt, E.C. Roelof Cosmic Ray Subsystem E.C. Stone, A.C. Cummings, N. Lal, F.B. McDonald, W.R. Webber Magnetometer N.F. Ness, L.F. Burlaga, J.P. Connerney, R.P. Lepping, C. Smith, F.M. Neubauer Plasma Wave Subsystem D.A. Gurnett, W.S. Kurth

V1 found two components in the heliosheath: Termination Shock Particles from nearby shock; Anomalous Cosmic Rays from remote source Heliosheath spectra ~70 days after V1 shock crossing TSP H spectral break at ~3.5 MeV Filled circles are from LECP Dashed and dotted lines are model ACR spectra for a strong and weak shock respectively 1.0

V2 TSP H spectrum approximation for 2007/261-312 (m2 s sr MeV)-1 (m2 s sr MeV)-1 V2 H Double pwr V2 H Pwr-Exp Ratio to Fit 1.0 Ratio to Fit MeV MeV Conclude that double power-law with exponential transition (Band et al. 1993) function is better approximation to TSP spectrum than is single power-law with exponential roll off. Four parameters, 3.5 decades

TSP V1 113 AU TSP 40 V2 85 220 840 TSPs steady for 3 years, but decreasing since 2010.3 Diffusive leakage across nearby heliopause, but no energy dependence? Dynamical effect? VR = 0? 1500

Interstellar Wind Muller, Zank

Side view of the heliosphere The speed in the outward direction decreases as the flow turns in the N direction to flow down the tail (green flow arrows) TS N R Opher et al. Sun is ~1500 times larger than scale 7/20/2011-4

N -R T

High Gain Antenna viewed from Earth C LECP CRS High Gain Antenna viewed from Earth Science Boom T V1 orientation with Rigel Kentaurus lockstar

V1: 53-85 keV 2007/345 V Decker et al.

-17 km/s Decker et al. SH23D-02

The Heliosheath Solar Wind Has Turned the Corner Since mid-2010, the radial wind speed has been essentially zero The average Tangential (longitudinal) speed hasn’t changed The Normal speed (latitudinal) is unmeasured Decker et al. SH23D-02

Krimigis et al. 2011

Transition layer - close to or at the heliopause? Krimigis et al. 2011

Side view of the heliosphere The speed in the outward direction decreases as the flow turns in the N direction to flow down the tail (green flow arrows), but VR was not expected to go to zero. TS N R Opher et al. Sun is ~1500 times larger than scale 7/20/2011-4

N -R T 10 revolutions about R axis CCW as viewed from Sun 2000 seconds per revolution. N Intensity of low energy ions normal to roll axis measured every 48 sec -R T

2008/71 2009/69 3.1±0.2% 2.3±0.2% N -T 59±4° V N -T 62±5°

2010/218 2010/309 0.9±0.2% 0.4±0.2% N -T 44±13° N -T 18±27°

2011/217 0.9±0.2% 1.5±0.2% N -T 44±13° N -T 71±8°

Flow is not turning northward, but is mainly tangential and variable 59±4° 116±8 N -T 62±5° N -T 44±13° 2008/071 2009/069 82±7 36±8 N -T N -T 2010/218 2010/309 61±6 16±8 Flow is not turning northward, but is mainly tangential and variable

Flows deflected to parallel the blunt heliopause Interstellar B Flat current sheet Flows deflected to parallel the blunt heliopause Radial component non-zero except near stagnation point, south of V1 Dynamical effect of declining pressure? Interstellar B Opher et al.

V1 at 117.8 AU in Boundary Region Inner Edge 113 AU Radial extent is unknown V1 moves outward 1 billion km every 2 years Outer Edge- any day or several years 7/20/2011-6

Termination Shock Particles Summary Termination Shock Particles Double power law, exponential knee (Band function) Superposition of varying exponential rolloffs (like SEPs) Recent decrease seen at V1; diffusive leakage (no energy dependence? transient? dynamical response? VR=0? Boundary layer; VR~0; small, variable, mainly tangential Transition layer (Suess, Krimigis et al.) Magnetic wall Plasma sheet layer inside heliopause (Washimi et al.) Reconnection (Drake et al.) Transient (Borovikov et al.) How much further to the heliopause? Anytime in next several years (V1 speed 3.6 AU/y) Power for all instruments until 2020 (~150 AU)