Solar Wind Transients and SEPs CSI 662 / ASTR 769 Lect. 06, March 20 Spring 2007 Solar Wind Transients and SEPs References: Lecture Gombosi: Chap. 12.5 – 12.7, P248 – P252 (supplement) Tascione: Chap. 3, P31-P40 (supplement) Prolss: 6.2, P300-P314 (supplement)

Solar Wind: Bimodal Fast and Slow Wind Fast wind originates from coronal hole, Slow wind originates from regions close to streamer belts or heliospheric current sheet SW heliographic latitudinal Distribution (Ulysses observation) Fast and Slow Wind

Solar Wind: Bimodal Fast and Slow Wind slow wind is denser and cooler fast wind is thinner and hotter Fast Solar Wind: originates in coronal holes Has flow speeds between 400-800km/s; average density is low ~ 3 ions/cm3 (1AU) The proton temperature is about 2x105 K The electron temperature is about 1x105K Slow Solar Wind: Speeds between 250-400km/s Average density is ~ 8 ions/cm3 (1AU) Solar Minimum -slow wind originates from regions close to the heliospheric current sheet Solar Maxima - slow wind originates above the active regions in the streamer belt Fast and Slow Wind

Heliospheric Current Sheet In a global sense, there is a huge current system flowing in a circumsolar disk, separating the two magnetic polarities The current sheet is inclined with respect to the ecliptic plan Solar rotation axis is 7° tilted Solar magnetic dipole axis is tilted from the rotation axis

Magnetic Sector The earth at one time above the current sheet, but at other times below the current sheet During solar minima, current sheet is rather simple, resulting two magnetic sectors as seen from the Earth During solar maximum, current sheet is complicated and highly distorted (warped), resulting in multiple magnetic sectors

Solar Wind Transients The normal or background solar wind generally follows the Archimedean spiral, characterized by the large scale sector magnetic structures and heliospheric current sheet They are usually steady and thus “quiet”; do not cause space weather disturbances Space weather is caused by solar wind transients, or highly disturbed solar wind. Solar wind transients are in two forms Interplanetary CME (ICMEs) Corotating interaction region (CIR) Solar wind transients are responsible for geomagnetic storms Increased IMF strength Increased solar wind speed Most importantly, the presence of southern IMF

Corotating Interaction Region (CIR) When a low latitude coronal hole appears (across the heliographic equator), fast wind exists in the ecliptic plane.

Corotating Interaction Region (CIR) The jetline of fast wind is less curved than that of slow wind Fast streams “catching up” with slow streams, compressing the preceding stream and produce a high pressure region. The interaction region is at the leading edge of the fast stream Since low-latitude coronal holes can live over several solar rotations, this structure can recur several times This is commonly called “corotating interaction region” or CIR A pair of forward and reverse shocks forms

Interplanetary CME (ICME) CME propagates into the interplanetary space, plowing through the ambient solar wind The magnetic structure of ICME at 1 AU is similar to that in its solar origin, which is highly helical (called flux rope) At 1 AU, it is called magnetic cloud highly organized magnetic field is observed, e.g., smooth rotation Large scale, crossing the Earth for ~ 24 hours Magnetic Cloud

Interplanetary CME (ICME) A Fast ICME pushes the interplanetary plasma, and produces a shock wave ahead of it. A CME driven shock is efficient in accelerating energy particles In addition to geomagnetic storms, CMEs are also responsible for energetic particle storms. ICME driven shock

SW Observations Direct solar wind observations are routine now ACE (Advanced Composition Explorer) (1997-present) spacecraft at Lagrangian point 1 WIND (1994-present) spacecraft (complicated orbit, sampling different parts of space) Measuring Magnetic field, 3-D Plasma velocity, density, temperature Particle energy, abundance, charge state, composition

Example Dst B/Bz Vel Np Tp Texp β Sun #75 2004/07/27 storm (-182 nT) Shock Front: discontinuity ICME (ejecta): B enhance Bz rotation Low Plasma β Low Tp High QFe ----- SH (Shock Sheath) Solar Sources

Example

Shock A Shock is a discontinuity separating two different regimes in otherwise continuous medium. It is associated with a disturbance moving faster than the signal speed in the medium (in a gas the signal speed is the speed of sounds; in space plasma: alfven speed) At the shock front the properties of the medium change abruptly. In a hydrodynamic shock, temperature and density increase- in a magnetohydrodynamic shock, magnetic field strength also increase.

Example of IP Shock

Shock Signal speed in the medium (Prolss Chap 6.3, P317-323) Sound speed or acoustic wave speed, caused by thermal pressure γ=5/3 for ideal gas Alfven speed in magnetized plasma, caused by magnetic pressure

Shock The Rankine-Hugoniot relations (Gombosi Chap 6.1, P103-106): 1: upper stream; 2: downsstream M: Mach number (flow speed/sound speed)

Time-variation of SEP fluxes Solar Energetic Particles (SEPs) SEPs with energies ranging from a few Kev to several Gev Because traveling close to speed of light, they reach the Earth in tens of minutes of the eruption Small SEPs are caused by flare related acceleration, lasting short (minutes) Large SEPs from CMEs Time-variation of SEP fluxes

Solar Energetic Particles (SEPs) Large SEPs are accelerated by CME-related IP shocks. They can last for several days because of the continuing driving of the shock Particle energy is gained from the kinetic energy of the shock front. Microscopic processes are complicated:

The End