Rosenvinge

The GGS/WIND Mission: 

The GGS/WIND Mission Tycho von Rosenvinge ACE/RHESSI/WIND Workshop Taos, New Mexico October 7, 2003

WIND Mission: 

WIND Mission Kluwer Academic Publishers ISBN 0-7923-3384-5 Reprinted from Space Science Reviews, Vol. 71, 1995 http://pwg.gsfc.nasa.gov/wind.shtml

Global Geospace Science Program: 

Global Geospace Science Program US Contribution to International Solar Terrestrial Physics Program USA: WIND and POLAR (GGS) ESA: SOHO and Cluster ISAS: Geotail

WIND Mission: 

WIND Mission WIND and ACE complement each other: WIND has a very sensitive radio/plasma WAVES instrument (S/C has very low EMI/EMC) WIND has spin-axis perpendicular to ecliptic (permits far better measurements of anisotropies) EPACT/LEMT fills gap between ACE/ULEIS and ACE/SIS 3DP fills gap between ACE/SWEPAM and ACE/EPAM (external surface of WIND is conducting, allowing SW core electron temperatures <1 eV to be observed) WIND teams have brought additional talent and competing viewpoints

WIND Spacecraft: 

WIND Spacecraft Launched November 1, 1994 Spin-axis perpendicular to ecliptic Spin-rate 20 RPM Launch weight ~ 1150 kg Orbits controlled by lunar swingbys and on-board hydrazine system Wire antennas: 100 m tip-to-tip, 15 m tip-to-tip Axial antennas ~ 12 m tip-to-tip Booms 12 m each

WIND Instruments: 

WIND Instruments

WIND Instruments, cont.: 

WIND Instruments, cont.

WIND Orbit: 

WIND Orbit Sun Coordinate System: earth at origin, earth-sun line fixed; projection of orbit onto ecliptic plane.

WIND Orbit, cont: 

WIND Orbit, cont

WIND Orbit, cont: 

WIND Orbit, cont

WIND Orbit, cont: 

WIND Orbit, cont

WIND Orbit, cont: 

WIND Orbit, cont

WIND Orbit, cont: 

WIND Orbit, cont

Small-Scale Gradients in B: 

Small-Scale Gradients in B Comparison of Wind (orange) and ACE (black) magnetic field data for an interplanetary shock at about 0438. Even when both spacecraft are near L1, in this case about 30 Re apart in Ygse, significant differences can exist between different observing points -- seen here between the ACE and Wind detection of a very non-planar shock with considerable variation in the Bz component.

WAVES Daily Plot : 

WAVES Daily Plot

WAVES: 

WAVES Type II burst shows evidence of CME/ IP shock; this CME was observed by SOHO

WAVES: 

WAVES Second Type II burst shows evidence of another CME which was not observed by SOHO

WAVES: 

WAVES Up-to-date WAVES data is readily available at http://lep694.gsfc.nasa.gov/waves/waves.html

Haggerty and Roelof, ApJ 579, 841,2002: 

Haggerty and Roelof, ApJ 579, 841,2002 Interpretation: There are 2 different populations of electrons: the first (prompt) is associated with the Type-III radio burst, the second (delayed, observed at 1 AU by EPAM) is accelerated and subsequently released by a CME-driven shock.

Slide20: 

Plasma frequency line emitted local to S/C at 1 AU Two sample electron events, one with a short e delay to 1 AU and a short radio drift time, one with a long e delay and a long radio drift time: Top panel = ACE/EPAM electrons, Bottom Panel = Type III observed by WIND/WAVES

Slide21: 

CANE, 2003 Suggests that there is only one electron population and that electron delays are due to interplanetary scattering. This will be the subject of considerable discussion in Working Group 1.

WIND/3DP Daily Plot: 

WIND/3DP Daily Plot

WIND/3DP Daily Plot: 

WIND/3DP Daily Plot Up-to-date plots available from http://sprg.ssl.berkeley.edu/wind3dp/esahome.html

Collisionless Magnetic Reconnection Diffusion Region: 

Collisionless Magnetic Reconnection Diffusion Region Oierset, et al., Nature, 412, 414, 2001

Observations (3DP): 

Observations (3DP) Oierset, et al., Nature, 412, 414, 2001

Solar Wind Experiment (SWE): 

Solar Wind Experiment (SWE) Two Faraday Cups The response of each Faraday cup to an internal calibration current has changed less than 0.3% over 8 years Solar Wind flow angle measured to better than 1 degree Withstands high intensity, high energy particles well Data available at http://web.mit.edu/afs/athena/org/s/space/www/wind.html

Bastille Day Event, 2000: 

Bastille Day Event, 2000 Three-day overview of Wind spacecraft observations of the July 2000 Bastille Day event. Top to bottom illustrates energetic particle flux (EPACT/LEMT), magnetic field data (MFI) and plasma data from SWE. A large halo CME occurred at the time of the vertical dashed line. S1 and S2 designate interplanetary shocks. MC2 and possibly MC1 are magnetic clouds. Eight hours of Geotail solar wind speed data are shown just before S2.

EPACT/LEMT: 

EPACT/LEMT 48 front detectors, each 2 cm2 x 18 microns thick, scan whole sky every spacecraft rotation (every 3 seconds). On-board particle identification bins particles according to energy, element, and arrival direction up to ~ 40,000 events per second. Total GF ~ 51 cm2-sr.

EPACT/LEMT: 

EPACT/LEMT

EPACT/LEMT-Discovery of Trans-Fe Events: 

EPACT/LEMT-Discovery of Trans-Fe Events

EPACT/LEMT- Anomalous Cosmic Rays: 

EPACT/LEMT- Anomalous Cosmic Rays The color assigned to the magnetic field azimuth in the middle panel is used to mark the ACR intensity in the lower panel. ACR intensities rise during outward (green) field polarity and fall during inward (red) polarity [Reames and Ng, 2001].

EPACT/LEMT- Anomalous Cosmic Rays, cont: 

EPACT/LEMT- Anomalous Cosmic Rays, cont Previous slide showed rising intensities during periods of outward directed fields (from the northern solar hemisphere) and falling intensities during periods of inward (southern) field. This behavior is consistent with the latitude field migration of the Fisk model during the 6-month interval when the Earth is on one side of the solar equator. However, the phase of the variation should reverse when Earth moves across the solar equator. The lack of a phase change is a severe challenge to the global field model.

SMS-STICS: Posner, Galvin, Schwadron, GRL, submitted: 

SMS-STICS: Posner, Galvin, Schwadron, GRL, submitted Note precursor ions well ahead of approaching IP shock

SMS-STICS: Posner, Galvin, Schwadron, GRL, submitted: 

SMS-STICS: Posner, Galvin, Schwadron, GRL, submitted 2nd example