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Panorama from STEREO A & B imaging the
heliosphere from the Sun to Earth (JPL image)
Marco Velli1,2, Neil Murphy2
1UCLA 2JPL
Heliophysics
Understanding the Sun and its Interactions
with the Earth and the Solar System
2
Heliophysics Science Goals
2013 Heliophysics Decadal Report, “Solar and Space Physics: A Science for a
Technological Society”
• Determine the origins of the Sun’s activity and predict the resulting
variations of the space environment (Space Weather Forecasting)
• Determine the dynamics & coupling of Earth’s magnetosphere,
ionosphere & atmosphere and their response to solar and terrestrial
inputs (Geospace)
• Determine interaction of the Sun with the solar system & interstellar
medium
• Discover and characterize fundamental processes that occur both
within the heliosphere and throughout the universe (particle
acceleration, magnetic reconnection, shock heating, etc.)
Scales of interest
range from 10s of km
to 100s of AU
Measurable quantities
include
electromagnetic
radiation, (from
Gamma rays to long
wave radio), electrons,
protons, neutrons, ions
and neutral atoms
Structure of the outer heliosphere
Initial model
Actual measurement
ation
er
Heating the low solar atmosphere
5
Slit-Jaw images and Spectra from the IRIS mission

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Astronauts and Robots 2015: Marco Velli, UCLA

  • 1. 1 Panorama from STEREO A & B imaging the heliosphere from the Sun to Earth (JPL image) Marco Velli1,2, Neil Murphy2 1UCLA 2JPL Heliophysics Understanding the Sun and its Interactions with the Earth and the Solar System
  • 2. 2 Heliophysics Science Goals 2013 Heliophysics Decadal Report, “Solar and Space Physics: A Science for a Technological Society” • Determine the origins of the Sun’s activity and predict the resulting variations of the space environment (Space Weather Forecasting) • Determine the dynamics & coupling of Earth’s magnetosphere, ionosphere & atmosphere and their response to solar and terrestrial inputs (Geospace) • Determine interaction of the Sun with the solar system & interstellar medium • Discover and characterize fundamental processes that occur both within the heliosphere and throughout the universe (particle acceleration, magnetic reconnection, shock heating, etc.)
  • 3. Scales of interest range from 10s of km to 100s of AU Measurable quantities include electromagnetic radiation, (from Gamma rays to long wave radio), electrons, protons, neutrons, ions and neutral atoms
  • 4. Structure of the outer heliosphere Initial model Actual measurement ation er
  • 5. Heating the low solar atmosphere 5 Slit-Jaw images and Spectra from the IRIS mission