SpaceMaster - Joint European Master in Space Science and Technology INTRODUCTION TO SPACE PHYSICS

Transcription

1 Erasmus Mundus SpaceMaster - Joint European Master in Space Science and Technology INTRODUCTION TO SPACE PHYSICS Wolfgang Droege University of Wuerzburg 2017/2018

2 Prof. Dr. Wolfgang Dröge Lehrstuhl für Astronomie Campus Hubland Nord Emil-Fischer-Straße 31 D Würzburg Phone: Fax: Office: Exercise Groups: HS-P / Physik SE 3 Thu 15:00 16:00 17:00 18:00 tbd

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4 registration in

5 exercise groups Thursdays 15:00 16:00 start: probably 10 Nov 16:00 17:00 17:00 18:00 tbd

6 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

7 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

8 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

9 MOTION OF PARTICLES CONSISTS OF TWO COMPONENTS: REGULAR MOTION IN SMOOTH, LARGE SCALE MAGNETIC FIELD AND SCATTERING AT FLUCTUATIONS IN THE MAGNETIC FIELD

10 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!

11 SOLAR CORONA LASCO C3 coronograph (NASA)

12 SOLAR WIND

13 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.

14 AURORAS Photo by Jan Curtis Aurora over Hancock, MI looking north, July 25, 2004, 2:18am Photos by Claudia Perko

15 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

16 NEUTRON MONITORS source:

17 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

18 Sources Of Energetic Particles Outside Of The Heliosphere Galactic Cosmic Rays Anomalous Cosmic Rays

19 WORLD-WIDE NEUTRON MONITOR NETWORK

20 THE BEGINNING OF THE SPACE AGE Sputnik Oct 4, 1957 Explorer 1 31 Jan 1958 discovery of radiation belts (van Allen belts)

21 RADIATION BELTS inner: mostly protons km outer: mostly electrons km

22 SUN AND SOLAR WIND EXHIBIT VARIABILITY ON A LARGE RANGE OF TIMESCALES

23 Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). gamma-ray imaging of solar flares reconstruction of event geometry

24 SOHO EIT (Solar & Heliospheric Observatory) (Extreme Ultraviolet Imaging Telescope)

25 SHOCK WAVE surface where physical parameters (n, T, v, ) undergo discontinuous changes supersonic aircraft solid sphere placed in supersonic flow gun shot kitchen sink

26 SOHO observations of coronal mass ejections and energetic particles

27 THEORETICAL MODEL OF A CME-DRIVEN SHOCK WAVE source: University of Riverside

28 magnetospheric bow shock heliospheric bow shock

29 acceleration of energetic charged particles at astrophysical shocks super nova remnants radio galaxies, quasars

30 ACCELERATION OF ENERGETIC PARTICLES AT SHOCK WAVES

31 Advanced Composition Explorer (ACE) observations of energetic particles and solar wind plasma (Lario 2004) time-intensity profiles angular distributions energy spectra Wind / Step

32 Sources Of Energetic Particles In The Heliosphere Solar Flares Coronal Mass Ejections (CMEs) / Shocks Corotating Interaction Regions Magnetospheres (Jupiter)

33 Energy Spectra Of Heliospheric Particles

34 COSMIC RAYS ARE OBSERVED AT ENERGIES UP TO > ev

35 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.

36 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

37 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

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39 POWER SPECTRA OF MAGNETIC FIELD TIME VARIATIONS FOURIER TRANSFORMS AUTOCORRELATION FUNCTION

40 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)

41 evolution of particle distributions in the inner heliosphere Fearless Forecasts University of Alaska and Exploration Physics International, Inc. realistic configurations of interplanetary magnetic field

42 impulsive injection Fearless Forecasts University of Alaska and Exploration Physics International, Inc.

43 Fearless Forecasts University of Alaska and Exploration Physics International, Inc.

44 STEREO Solar Terrestrial Relations Observatory Stereoscopic observations of Sun and of CMEs with 2 spacecraft launch: 26 October 2006 KSC / Florida

45 Current solar activity and STEREO positions

46 What is Space Weather? ( "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."

47 EFFECTS OF SPACE WEATHER

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49 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

50 WIND 3-D Plasma and Energetic Particle Experiment PI: R.P. LI Ions and electrons 3 ev- 30 kev and 20 kev- 11 MeV

51 WIND ACE STEREO WIND 3DP SST 4 π angular coverage electrons: kev protons: 60 kev 7 MeV ACE / EPAM / LEFS60 spin axis towards Sun 8 sectors electrons: kev STEREO / IMPACT / SEPT 3-axis stabilized 4 viewing directions electrons: kev protons: 60 kev 7 MeV

52 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

53 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

54 Introduction to Space Physics (4 SWS) Wolfgang Dröge 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