SPACE WEATHER INTERPRETING THE WIND Petra Vanlommel & Luciano Rodriguez
THE SUN LOSES ENERGY Radiation Mass Particles
THE SUN LOSES ENERGY PHYSICAL REPHRASING Total Solar Irradiance Solar Wind Fast Particles
SPACE WEATHER Flares Plasma wolken Snelle zonnewind Proton storm
SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
SPACE WEATHER Space weather describes the conditions in space that affect Earth and its technological systems. Space weather storms originate from the Sun and occur in space near Earth or in the Earth's atmosphere. These storms generally occur due to eruptions on the Sun known as solar flares, proton storms and the solar wind.
TIME TO ARRIVE ON EARTH Plasma wolken 8 minutes Flares Days Proton Hour storm Snelle zonnewind
FORECAST Flare Flares probability Perturbations Plasma wolken of the Geomagnetic Snelle zonnewind field Proton Probability storm
RELAX AND WATCH
OUR PROTECTION
Total Solar Irradiance Solar Wind Fast Particles
GEOMAGNETIC STORMS 4x 100x 200x 600x 1700x
CONSEQUENCES GIC Satellite operations, e.g. GNSS, drag, surface charging Radio communication Electrical power plants Aurora Malmö Blackout - Oct 30, 2004 About 50 000 customer were without electricity in Malmö, Sweden for 20-50 minutes First known power grid blackout due to GIC in Europe An overcurrent relay was too sensitive to the third harmonic of 50 hz. It has been replaced by a less sensitive relay later.
GLOBAL SOLAR DIPOLE Snelle wind Open magneetveld lijnen Snelle wind Gesloten veldlijnen Heliosferisch stroomvlak Trage wind Trage wind Snelle wind
LOCAL MAGNETIC FIELDS
LOCAL MAGNETIC FIELDS
SOLAR WIND
SLOW VERSUS FAST 250-400 High: ~10 Low: ~10 4 K, ~1eV Variable km/s Density, cm -3 Temperature Behavior 400-800 Low: ~3 High: ~10 5 K, ~10eV Stationary
SOLAR WIND - IN SITU
COORDINATE SYSTEM
IMF POLARITY for 400 km/s ϕ ~ 135 for 400 km/s ϕ ~ 315
EXTREME FAST ϕ = 90
EXTREME FAST ϕ = 0 ϕ = 360
RADIAL
RADIAL
RADIAL
RADIAL
VARIATIONS Non-eruptive Eruptive Coronal Hole Coronal Mass Ejection Sector Boundary Crossing
SECTOR BOUNDARY CROSSING
HELIOSPHERIC CURRENT SHEET Snelle wind Open magneetveld lijnen Snelle wind Gesloten veldlijnen Heliosferisch stroomvlak Trage wind Trage wind Snelle wind
BALLERINA SKIRT
MAGNETIC SECTORS Cravens, 1997
SEPT 10 - IN SITU: PHI
SEPT 10 - IN SITU - DENSITY
SEPT 10 - IN SITU - BZ
GEO EFFECTIVENESS
CORONAL HOLE
WHEN SLOW AND FAST MEET
Top View
IN SITU - CH IN A SCHEME
CORONAL HOLE Co-rotating structure Shock is present, usually behind 1AU Radial! No extra mass-flux
IN SITU
IN REAL LIFE
CME A new, discrete, bright white light feature in the coronograph field-of-view with a predominantly, radial outward velocity.
TRANSIENT - EXTRA MASS
STRUCTURE 1.Shock, if ICME is fast enough 2.Shocked sheath plasma compressed - heated - strong B - varying direction of B 3.Driver gas, i.e. ICME cool - steady strong B - large scale smooth field rotation - decreasing speed
PATH
Shock Short sheath High B Smooth rotation in Bz Decreasing speed
Shock Sheath High B Smooth rotation in Phi Decreasing speed Low T
THE WIND YESTERDAY
SOLAR SOURCE
CONTACT SIDC: sidc.be STCE News letter: stce.be petra.vanlommel@oma.be
INTERESTING stce.be/esww10
MI : SPACE WEATHER FOR ENGINEERS Focus on HF communication, Trans-ionospheric propagation, effects on GNSS signal precision http://www.stce.be/sw4e/, Nov 12-15, 2013, Leuven, Belgium