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Evolution of PUI Distributions E. Möbius 1, B. Klecker 2, P. Bochsler 1, G. Gloeckler 3, H. Kucharek 1, P.A. Isenberg 1 1 Institute for the Study of Earth,

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Presentation on theme: "Evolution of PUI Distributions E. Möbius 1, B. Klecker 2, P. Bochsler 1, G. Gloeckler 3, H. Kucharek 1, P.A. Isenberg 1 1 Institute for the Study of Earth,"— Presentation transcript:

1 Evolution of PUI Distributions E. Möbius 1, B. Klecker 2, P. Bochsler 1, G. Gloeckler 3, H. Kucharek 1, P.A. Isenberg 1 1 Institute for the Study of Earth, Oceans & Space and Department of Physics, University of New Hampshire, Durham, NH, USA 2 Max-Planck-Institut für extraterrestrische Physik, Garching, Germany 3 Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, USA 1 Institute for the Study of Earth, Oceans & Space and Department of Physics, University of New Hampshire, Durham, NH, USA 2 Max-Planck-Institut für extraterrestrische Physik, Garching, Germany 3 Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, USA Supported by NASA SR&T, STP, ACE, Prodex, Swiss NF, & DLR

2 Strong Variations in Pickup Ion Distributions Pickup Ion Distributions are Highly Variable Pickup Ions React to: - IMF Orientation (early Rollover) - IMF Strength (Compression and Rarefaction) - SW Density (Compression and Rarefaction) - Ionization rates & probably several unknown causes For Deduction of LIC Parameters Mitigation Sought with: - Long Integration Times Plan: Attempt to Understand Causes - Also Provides Handle on Ion Transport and Acceleration STEREO A,B & ACE Provide Simultaneous Observations Pickup Ion Distributions are Highly Variable Pickup Ions React to: - IMF Orientation (early Rollover) - IMF Strength (Compression and Rarefaction) - SW Density (Compression and Rarefaction) - Ionization rates & probably several unknown causes For Deduction of LIC Parameters Mitigation Sought with: - Long Integration Times Plan: Attempt to Understand Causes - Also Provides Handle on Ion Transport and Acceleration STEREO A,B & ACE Provide Simultaneous Observations

3 STEREO-A & STEREO-B He + Cone Observations in 2007 At STEREO-B: Cone has Double Peak At STEREO-B: Cone has Double Peak At STEREO A: Cone has Single Peak Cone appears narrower At STEREO A: Cone has Single Peak Cone appears narrower Phasing with SW Streams Determines Shape

4 STEREO-A & STEREO-B He + Cone Observations in 2007 He + relates to N sw, particularly at CIR compressions

5 STEREO-A He + Observations in 2007 & 2008 He + Peaks Related to J sw but not much better than with N sw Phasing with SW Streams Determines Shape Pickup Ions are Related to SW Density and Flux, but not the full story Sorting according to IMF Orientation doesn’t improve correlation

6 Additional Cone Variations Could Transport with IMF Play a Role? IMF Could Transport PUIs out of the Cone Different IMF Orientation Could Enable Varying Transport Implicit Assumption: PUIs ride with SW - But only part of the PUI phase space does Other phase space parts ride (along B) from different directions STEREO A&B April 1, 2007 approx. Parker ACE

7 Pickup Ion Phase Space Distribution and their Observation Assume Isotropic Distribution - Fast pitch-angle scattering - Adiabatic Cooling - Mapping of Neutral Source Assume Isotropic Distribution - Fast pitch-angle scattering - Adiabatic Cooling - Mapping of Neutral Source PUI PSD Centered on SW - V sw cut symmetric about SW - But not in flux! PUI PSD Centered on SW - V sw cut symmetric about SW - But not in flux! Observed PUI PSD - Integrated over ∆  & ∆E in SW Sector Observed PUI PSD - Integrated over ∆  & ∆E in SW Sector Good Agreement 1.4<w< 1.8! Differences: - At Cut-off - Near SW Good Agreement 1.4<w< 1.8! Differences: - At Cut-off - Near SW

8 Study of Variations Requires Baseline of Neutral Distribution and Mapping into PUI Distributions via Ionization & Cooling Start to Tackle this Issue! Previous Paradigm: Cooling is Completely Adiabatic Implies - Expansion as 1/r 2 for SW and IMF - Immediate Isotropization of PUIs Yet:- Evidence for Compressions & Decompressions - Evidence for Slow Scattering for PUIs How Can We Separate the Cooling Coefficient? Study of Variations Requires Baseline of Neutral Distribution and Mapping into PUI Distributions via Ionization & Cooling Start to Tackle this Issue! Previous Paradigm: Cooling is Completely Adiabatic Implies - Expansion as 1/r 2 for SW and IMF - Immediate Isotropization of PUIs Yet:- Evidence for Compressions & Decompressions - Evidence for Slow Scattering for PUIs How Can We Separate the Cooling Coefficient? Perplexing Variations of Pickup Ions - Impact of Ionization & Cooling

9 Influence of Ionization & Cooling PUI Distribution Determined by Ionization & Cooling: Along Inflow Axis Assume  = 1.5 Assume  = 1.2 PUI Distribution Determined by Ionization & Cooling: Along Inflow Axis Assume  = 1.5 Assume  = 1.2

10 Influence of Ionization & Cooling PUI Distribution Determined by Ionization & Cooling: Along Inflow Axis Use  = 1.5 & 1.2 Assume  = 1 AU (SolMax) Assume  = 0.3 AU (SolMin) PUI Distribution Determined by Ionization & Cooling: Along Inflow Axis Use  = 1.5 & 1.2 Assume  = 1 AU (SolMax) Assume  = 0.3 AU (SolMin) Requires Pickup Ion Data Over Full Solar Cycle Available from ACE SWICS!

11 Influence of Ionization & Cooling PUI Distribution Determined by Ionization & Cooling ACE SWICS PUI PSDs June 2001 & 2007 - Along Inflow Axis - 2001  = 0.85 AU (SolMax) - 2007  = 0.34 AU (SolMin) Use  = 2.0, 1.5 & 1.2 in Model Looks Tantalizing! Acceptable V/V sw To Do PSD Integration!! PUI Distribution Determined by Ionization & Cooling ACE SWICS PUI PSDs June 2001 & 2007 - Along Inflow Axis - 2001  = 0.85 AU (SolMax) - 2007  = 0.34 AU (SolMin) Use  = 2.0, 1.5 & 1.2 in Model Looks Tantalizing! Acceptable V/V sw To Do PSD Integration!!

12 Summary & Conclusions Interstellar He Cone Traversals with STEREO A & B Show remarkable substructure aligned with SW density enhancements, but neither SW density, flux, ionization and IMF variations explain all PUI variations Potential Culprits: a) Deviations from adiabatic cooling b) Transport effects not aligned with SW a) First attempt to separate effects of ionization rates and cooling behavior on PUI spectra appear to suggest a deviation from plain adiabatic dependence (w 3/2 ), but so far only pseudo phase space density evaluated b) ACE & STEREO Spring 2007 at 0.01AU along Interstellar He Cone Traversals with STEREO A & B Show remarkable substructure aligned with SW density enhancements, but neither SW density, flux, ionization and IMF variations explain all PUI variations Potential Culprits: a) Deviations from adiabatic cooling b) Transport effects not aligned with SW a) First attempt to separate effects of ionization rates and cooling behavior on PUI spectra appear to suggest a deviation from plain adiabatic dependence (w 3/2 ), but so far only pseudo phase space density evaluated b) ACE & STEREO Spring 2007 at 0.01AU along

13 Thank You! Support for this Project: - NASA SR&T - NASA ACE - NASA Solar Terrestrial Probes - PRODEX & Swiss National Foundation - DLR in Germany

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