outflow jets, ion heating, and 3d structure in ssx
DESCRIPTION
Outflow jets, ion heating, and 3D structure in SSX. Michael Brown Swarthmore College, NSF Center for Magnetic Self-Organization Tim Gray, Ed Dewey ’10, Bevan Gerber-Siff ’10, Kevin Labe ‘11 Vernon Chaplin ’07, Lake Bookman `08 M. J. Schaffer E. V. Belova - PowerPoint PPT PresentationTRANSCRIPT
Michael Brown
Swarthmore College, NSF Center for Magnetic Self-Organization
Tim Gray, Ed Dewey ’10, Bevan Gerber-Siff ’10, Kevin Labe ‘11Vernon Chaplin ’07, Lake Bookman `08
M. J. Schaffer
E. V. Belova
Research supported by US DOE and NSF
Outflow jets, ion heating, and 3D structure in SSX
SSX parametersIon Density (protons) 1014 -1015 cm-3
Temperature (Te,Ti) 20 - 80 eV
Magnetic Field 0.1 Tesla
Ion gyroradius 0.5 cm
Alfvén speed 100 km/s
S (Lundquist number) >1000
Plasma 10-100%
Poloidal flux 3-4 mWb
Spheromak formation
2D MHD simulation
Tangled 3D magnetic lines (lab and solar)
one foot tall 5 earth diameters tall
Ele
ctro
n D
iffus
ion
Reg
ion
Reconnection geometry (2D model)
Sepa
ratr
ix
Inflow (slow)
Outflow (fast, Alfvenic)
Current flow (out)Electron flow (in)
3D hybrid simulation (Y. Lin)
Kinetic ions (5x108 ions), fluid electrons
Simulation results: 3D resistive MHD (E. Belova, PPPL)
SSX device (distributed probe array)
•Opposing magnetized plasma guns•Close fitting copper flux conserver•Midplane IDS access for flow studies
Local 3D probe measurements
Right-handedSpheromak
Left-handedspheromak Reconnected
poloidal flux
Merging studies in prolate geometry(2003-2007)
• 0.4 meter diameter, 0.6 meter length • reconnection at midplane
• formation of prolate FRC object • ultimately unstable with slow growth rate
Counter-helicity merging (prolate)
3D probe measurements in SSX
3D probe measurements in SSX
3D probe measurements in SSX
Bi-directional outflows in SSXHigh resolution ion Doppler spectroscopy
(Cothran, et al, PRL to be submittedJ. Fung thesis ‘06)
Ion Doppler Spectroscopy (1.33m)
Ion Doppler Spectroscopy (1.33m)
Ion Doppler spectrometer layout
IDS line shapes (high resolution)
Observation of bi-directional outflow
Data is effectively f(v_r)… one pixel is 10 km/s
Stills from IDS movie
Dynamics of the flow (bursts, turbulence) encoded in the lineshape
Bi-directional outflows on the sun
D. Innes (SOHO SUMER chromosphere)Innes, Nature, 1997
Innes, Solar Physics, 1997
Location of SUMER slit on solar disk
SiIV light dispersed along slit
Velocity resolution 10 km/s
Spatial resolution1000 km
Spatially localizedevents
Hot ions in SSX
Cothran, et al (SSX)
(low density discharges,after glow discharge conditioning, short gas delay)
Hot ions in SSX (merging)
IDS hot ion temperature measurement (one shot, 1014
density)
IDS hot ion flow measurement
IDS hot ion temperature measurement (average, 5x1014
density)
Scaling of Ti with density
Scaling of Ti with density (single sph)
Dipole-trapped, Gaussian fit, early in formation (30-40 s)
IDS ion temperature measurement HeII 468.57 nm (THe > TC)
Te from CIII (97.7 nm) to CIV (155 nm) ratio
Te from CIII (97.7 nm) to CIV (155 nm) ratio (single spheromak)
Te from SXR array fitting
Observe electron heating with SXR during 30-40 s reconnection period
Hot ions in the extended corona
Cranmer, Space Science Rev, 2002 (UVCS)
UVCS line of sight
Greater than mass ratio ion temperatures
Quadrupole measurement in SSX
Mattheaus, et al, GRL (2005)Landreman, (2003)
Cothran, et al, GRL (2003)
Driven magnetic reconnection experiments
Cothran et al GRL 30, 1213 (2003)Brown et al ApJL 577, 63 (2002)Brown et al Phys. Plasmas 9, 2077 (2002)Brown et al Phys. Plasmas 6, 1717 (1999)Kornack et al Phys. Rev. E 58, R36 (1998)
Magnetic probe array
RGEAs
Large slots cut into FC rear walls define the reconnection region
3D magnetic structureEnergetic particles
3D magnetic probe array
600 coils, 558 array
~2 cm spacing
25 three channel 8:1multiplexer/integratorboards
10 eight channel 8-bitCAMAC digitizers
Full probe readoutevery 0.8 s
Quadrupole out-of-plane field
Ion inertial scale 2 cm
Trajectory of Polar spacecraft
Path of tiny Polar
Trajectory of POLAR spacecraft
Polar trajectory
Mozer, et al, PRL (2002)
POLAR SUB-SOLAR OBSERVATION OF THE ION SCALE
Merging studies in oblate geometry(2007-2008+)
• 0.5 meter diameter, 0.4 meter length • turbulent merging process
• formation of oblate FRC object (sometimes)•Ti higher, Te lower than prolate
• often unstable with Alfvenic growth rate
Trapezoidal flux conserver in SSX
Trapezoidal flux conserver in SSX
Trapezoidal flux conserver in SSX
FRC equilibrium with trapezoidal FC
2D merging simulation (N. Murphy)
Stable Oblate FRC in SSX (sometimes)
Ti and Te in oblate merging in SSX
Ti higher, Te lower than prolate
Density at midplane with merging
Dynamic merging events in SSX
Unstable! Turbulent?
Summary (1)
Bi-directional sub-Alfvenic outflowmeasured with ion Doppler spectroscopy on SSX
Hot ions and warm electrons also observed in the laboratoryusing spectroscopy/soft x-rays
Summary (2)
Measurement of Ti for different ion mass(Carbon, Helium, Silicon)
Electron heating observed during mergingevents using soft x-ray array…
less heating for single spheromak
Summary (3)
3D structure measured at the ion inertial scale in SSX merging experiments
First laboratory measurement ofout of plane quadrupole field observed onlength scale similar to Polar observations
at the magnetopause
Summary (prolate)
Bi-directional sub-Alfvenic outflowmeasured with ion Doppler spectroscopy on SSX
Both ions/electrons heated by reconnection
Spheromak merging createsunstable prolate FRC object
with reconnection at midplane
Summary (oblate)
Merging in oblate geometry in SSX
Hot ions and warm electrons also observed in the laboratoryusing spectroscopy/soft x-rays
Future studies (fall 2008)
Measurement of Ti for different ion mass(Carbon, Helium, Xenon)
Continue search for stable mergingin oblate geometry
Future studies (fall 2008)
High resolution, high frequency mag probe(Tobin Munsat collaboration)
Mach and retarding grid ion probes