Erasmus Mundus SpaceMaster - Joint European Master in Space Science and Technology INTRODUCTION TO SPACE PHYSICS Wolfgang Droege University of Wuerzburg 2017/2018
Prof. Dr. Wolfgang Dröge Lehrstuhl für Astronomie Campus Hubland Nord Emil-Fischer-Straße 31 D-97074 Würzburg Phone: 0931 31 83669 Fax: 0931 31 84603 droege@astro.uni-wuerzburg.de Office: 31.01.012 Exercise Groups: HS-P / Physik SE 3 Thu 15:00 16:00 17:00 18:00 tbd http://www.astro.uni-wuerzburg.de/en/teaching/winterterm-2016-17/spacephysics
registration in sb@home
exercise groups Thursdays 15:00 16:00 start: probably 10 Nov 16:00 17:00 17:00 18:00 tbd
Chair for Astronomy and Astrophysics Prof. Dr. K. Mannheim high-energy astrophysics astrophysical sources of high-energy neutrinos indirect signatures of dark matter observations with gammaray telescopes MAGIC and FACT Prof. Dr. M. Kadler multiwave-length astronomy radio astronomy / VLBI studies of black holes and relativistic plasma jets cosmic gamma-ray bursts Prof. Dr. W. Dröge space physics analysis of in-situ spacecraft measurements particle acceleration in cosmic sources transport simulations of solar particles in the heliosphere
SPACE PHYSICS Investigation of the natural plasma environments close enough to the Earth to be studied by in situ measurements: Solar Wind and Interplanetary Magnetic Field Sun Heliosphere Magnetospheres Ionospheres Topics: Energetic Particles Plasma Waves Auroras Space Weather Instruments ELECTRODYNAMICS PLASMA PHYSICS STATISTICAL PHYSICS GEOPHYSICS ASTROPHYSICS NUCLEAR / ELEMENTARY PARTICLE PHYSICS
ELECTRODYNAMICS: Maxwell s equations in vacuum SI CGS (Gauss) Coulomb s law no magnetic monopoles Faraday s law Ampere s law Field transformations Ohm s law Lorentz force
MOTION OF PARTICLES CONSISTS OF TWO COMPONENTS: REGULAR MOTION IN SMOOTH, LARGE SCALE MAGNETIC FIELD AND SCATTERING AT FLUCTUATIONS IN THE MAGNETIC FIELD
PLASMA: The state of matter in which neutral atoms are separated into charged components (ions and electrons) Plasma Physics treats the collective behaviour of charged particles in electromagnetic fields more than 99% of the visible matter in the universe is in the plasma state interplanetary space is a huge natural plasma laboratory accessible by spacecraft, which helps to develop a consistent picture of fundamental plasma physical processes distribution function, phase space density transport (Boltzmann-) equation force density SYSTEM OF COUPLED, NON-LINEAR DIFFERENTIAL EQUATIONS!
SOLAR CORONA LASCO C3 coronograph (NASA)
SOLAR WIND
COMETS HALE BOPP Photo: National Astronomical Observatory of Japan A comet generally has two tails, not one. Dust tail: points back along the comet path Ion Tail: electrically charged particles which originate from the nucleus as (neutral) gaseous particles. Because of the interaction with the Sun's magnetic field, this tail always points directly away from the Sun.
AURORAS Photo by Jan Curtis Aurora over Hancock, MI looking north, July 25, 2004, 2:18am Photos by Claudia Perko
COSMIC RAYS Electroscope Victor Hess before his 1912 balloon flight in Austria, during which he discovered cosmic rays ionisation increases with altitude (above 1.5 km) source located above the Earth s atmosphere
NEUTRON MONITORS source: http://neutronm.bartol.udel.edu/
MODULATION OF THE GALACTIC COSMIC RAY COMPONENT Solar modulation refers to the influence the Sun exerts upon the intensity of galactic cosmic rays. As solar activity rises (top panel), the count rate recorded by a neutron monitor in Thule, Greenland decreases (bottom panel). Modulation related to Variability of the Sun: Sun spots solar magnetic fields duration of full solar cycle ~ 22 years
Sources Of Energetic Particles Outside Of The Heliosphere Galactic Cosmic Rays Anomalous Cosmic Rays
WORLD-WIDE NEUTRON MONITOR NETWORK
THE BEGINNING OF THE SPACE AGE Sputnik Oct 4, 1957 Explorer 1 31 Jan 1958 discovery of radiation belts (van Allen belts)
RADIATION BELTS inner: mostly protons 700 6000 km outer: mostly electrons 15000-25000 km
SUN AND SOLAR WIND EXHIBIT VARIABILITY ON A LARGE RANGE OF TIMESCALES
Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). gamma-ray imaging of solar flares reconstruction of event geometry
SOHO EIT (Solar & Heliospheric Observatory) (Extreme Ultraviolet Imaging Telescope)
SHOCK WAVE surface where physical parameters (n, T, v, ) undergo discontinuous changes supersonic aircraft solid sphere placed in supersonic flow gun shot kitchen sink
SOHO observations of coronal mass ejections and energetic particles
THEORETICAL MODEL OF A CME-DRIVEN SHOCK WAVE source: University of Riverside
magnetospheric bow shock heliospheric bow shock
acceleration of energetic charged particles at astrophysical shocks super nova remnants radio galaxies, quasars
ACCELERATION OF ENERGETIC PARTICLES AT SHOCK WAVES
Advanced Composition Explorer (ACE) observations of energetic particles and solar wind plasma (Lario 2004) time-intensity profiles angular distributions energy spectra Wind / Step
Sources Of Energetic Particles In The Heliosphere Solar Flares Coronal Mass Ejections (CMEs) / Shocks Corotating Interaction Regions Magnetospheres (Jupiter)
Energy Spectra Of Heliospheric Particles
COSMIC RAYS ARE OBSERVED AT ENERGIES UP TO > 10 20 ev
Maxwellian velocity distribution function The general equilibrium VDF in a uniform thermal plasma is the Maxwellian (Gaussian) distribution. The average velocity spread (variance) is, <v> = (2k B T/m) 1/2, and the mean drift velocity, v 0.
What is the nature of the solar wind fluctuations? Plasma Waves: deterministic relation between frequency and wavenumber ω = ω (k) Turbulence: correlation between ω and k only statistical
What is the nature of the solar wind fluctuations? WAVE PICTURE: superposition of small-amplitude linear plasma waves deterministic correlation between frequency and wave number dispersion relation ω = ω(k) TURBULENCE PICTURE: only statistical correlation between frequency and wave number strong interaction between fluctuations with different wave numbers
POWER SPECTRA OF MAGNETIC FIELD TIME VARIATIONS FOURIER TRANSFORMS AUTOCORRELATION FUNCTION
modeling of the propagation of energetic solar particles in the solar wind with solutions of the transport equation (analytical and numerical) predictions from observed solar wind parameters possible? phase space density f(r,p,µ,t)
evolution of particle distributions in the inner heliosphere Fearless Forecasts University of Alaska and Exploration Physics International, Inc. http://gse.gi.alaska.edu/index.html realistic configurations of interplanetary magnetic field
impulsive injection Fearless Forecasts University of Alaska and Exploration Physics International, Inc. http://gse.gi.alaska.edu/index.html
Fearless Forecasts University of Alaska and Exploration Physics International, Inc. http://gse.gi.alaska.edu/index.html
STEREO Solar Terrestrial Relations Observatory Stereoscopic observations of Sun and of CMEs with 2 spacecraft launch: 26 October 2006 KSC / Florida
http://sdo.gsfc.nasa.gov/data/ Current solar activity and STEREO positions http://sohowww.nascom.nasa.gov/data/realtime/gif/ http://stereo-ssc.nascom.nasa.gov/index.shtml
What is Space Weather? (http://sohowww.nascom.nasa.gov/) "conditions on the Sun and in the solar wind, magnetosphere, ionosphere and thermosphere that can influence the performance and reliability of space-borne and ground-based technological systems and can endanger human life or health."
EFFECTS OF SPACE WEATHER
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-totip, 15 m tip-to-tip Axial antennas ~ 12 m tip-to-tip Booms 12 m each
WIND 3-D Plasma and Energetic Particle Experiment PI: R.P. LI http://sprg.ssl.berkeley.edu:80/wind3dp/ Ions and electrons 3 ev- 30 kev and 20 kev- 11 MeV
WIND ACE STEREO WIND 3DP SST 4 π angular coverage electrons: 42 600 kev protons: 60 kev 7 MeV ACE / EPAM / LEFS60 spin axis towards Sun 8 sectors electrons: 45 312 kev STEREO / IMPACT / SEPT 3-axis stabilized 4 viewing directions electrons: 30 400 kev protons: 60 kev 7 MeV
FUTURE MISSIONS SOLAR ORBITER ESA / NASA Start: 2018 Perihelion: ~ 0.28 AU (60 R S ) Cruise Phase: ~ 3.5 y Orbit: ~ 150 d Maximum latitude: ~ 30 instrument development: start 2010 SOLAR PROBE NASA Start: 2018 Closest approach ~ 10 R S What are the origins of the solar wind streams and the heliospheric magnetic field? What are the sources, acceleration mechanisms, and transport processes of solar energetic particles? How do coronal mass ejections evolve in the inner heliosphere
Интергелиозонд (INTERHELIOPROBE) launch ~ 2025 Determine the mechanisms of the solar corona heating and acceleration of the solar wind Investigate thin structure and dynamics of the solar atmosphere Define the nature and global dynamics of the solar flares and coronal mass ejections and their influence on the heliosphere and space weather Explore the Sun as the powerful and changeable accelerator of the particles Observe from high heliolatitude and to investigate the solar atmosphere and the corona in polar and equatorial regions Charged Particle Telescope
Introduction to Space Physics (4 SWS) 0922056 Wolfgang Dröge droege@astro.uni-wuerzburg.de http://www.physik.uni-wuerzburg.de/en/astro/people/ag_droege/ Lecture Tue 14:00-16:00 HS P / Physik Thu 14:00-15:00 HS P / Physik Exercise Thu tbd Groups Literature: May-Britt Kallenrode, Space Physics Springer Verlag George K. Parks, Physics Of Space Plasmas, Westview Press Malcom S. Longair, High-Energy Astrophysics, Cambridge University Press A.O. Benz, Plasma Astrophysics Kluwer, Dordrecht Margaret G. Kivelson & Christopher T. B. Rossi, Cosmic Rays, McGraw Hill Russel, Introduction to Space Physics, Englewood Cliffs, 1964 Cambridge University Press