MESSENGER observations of Mercury’s northern cusp

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Presentation transcript:

MESSENGER observations of Mercury’s northern cusp Jim M. Raines University of Michigan Patrick J. Tracy, Daniel J. Gershman, Gang Kai Poh, James A. Slavin, Thomas H. Zurbuchen, Haje Korth, Brian J. Anderson, and Sean C. Solomon MESSENGER-BepiColombo Joint Meeting 16 June 2015 Add co-authors

First orbital observations Magnetospheric Cusps Updated version from Zurbuchen et al., 2011 Enhanced plasma flux observed on >90% orbits LAT: 30-80; LT 6-14 h. Consistent with analysis of magnetic depressions [Winslow et al., 2012] Na+-group ions dominate planetary species, but He+ and O+ group ions observed. 2 16 June 2015 Jim M. Raines, Univ. of Michigan

Three sources for cusp plasma identified Raines et al., 2014 1. Solar wind H+ enter on newly reconnected field lines, loss cone shows some will precipitate onto surface. 2. Upwelling Na+ ions observed down to 70 km altitude may be from surface sputtering. Energy: 100-300 eV. 3. Na+ are ionized near the magnetopause and driven into the cusp by reconnection. Energy: 2.7 keV (ave) 16 June 2015 Jim M. Raines, Univ. of Michigan

Jim M. Raines, Univ. of Michigan Energy dispersion curve Typical case 3: Active Cusp Dayside Na+-group ions 16 June 2015 Jim M. Raines, Univ. of Michigan

Precipitating protons H+ in cusp Clean, 140° cut-off angle evidence of 50° loss cone evident. Consistent with 59° average loss cone [Winslow et al., 2014] Very narrow (~15°) beam directed toward surface is <10 s in duration 6.2 x 107 (cm2 s)-1 PPT flux α=180 α=0 surface  50-60° Loss cone Flow into cusp down to surface Reflectometry: 56-62° Winslow et al., 2014 5 16 June 2015 Jim M. Raines, Univ. of Michigan

Upwellng Na+ Pitch angles for Na+ in cusp α=180 α=0 Surface Very little flux directed at surface Upwelling component 16 June 2015 Jim M. Raines, Univ. of Michigan

Jim M. Raines, Univ. of Michigan North-flowing beam on dayside consistent with freshly-reconnected field lines sweeping over the cusp Cusp Cusp Dayside Dayside 16 June 2015 Jim M. Raines, Univ. of Michigan

Statistical results (1) Proton precipitation (PPT) flux varies over 4 orders of magnitude, likely due to changing solar wind conditions. 16 June 2015 Jim M. Raines, Univ. of Michigan

Statistical results (2) Variation due to solar wind conditions dominates variations due to altitude. (PPT rate calculated assuming circular cusp of measured length.) 16 June 2015 Jim M. Raines, Univ. of Michigan

Jim M. Raines, Univ. of Michigan Summary and Beyond Studies in progress now Detailed examination very low altitude data (< 100 km) Identification of reconnection site through energy dispersion analysis Very high time resolution (150 ms) analysis of cusp dynamics Search for new species m/q > 30 via laboratory measurements Summary Proton precipitation observed at all altitudes substantial. Fluxes range 104 – 108 cm-2 s-1. >50° loss cone observed as <130° cutoff angle High-energy (> 1 keV) Na+ is swept in by reconnection and is evident at all altitudes Low-energy (100-300 keV), upwelling is Na+ evident at all altitudes, though not directly coupled to observed proton precipitation flux. Variation due to solar wind conditions dominates those due to altitude. Change! 16 June 2015 Jim M. Raines, Univ. of Michigan