11 mccaffrey eve epo -...
TRANSCRIPT
-
Page 1SDO EPO- DRAFTFEB2008
EVEEPO
-
Page 2SDO EPO- DRAFTFEB2008
EVE EPO Toolkit1.EUV FAQ2.Google Earth Ionosphere3.UV Activities4.Space Weather Monitors5.EVE EPO Website6.GEMS Science Kits (LHS)7.All About EVE DVD8.SDO EPO Slidedeck9.Tips for EPO10.Discussion
-
Page 3SDO EPO- DRAFTFEB2008
EPO Tips1. Know Your Audience2. Keep it Simple3. Minimize Text - Maximize Images4. Be a storyteller5. Use Humor6. Use Repetition7. Use Repetition8. Be Interactive9. Emphasize just a few key points (- less is
MORE!)10.Smile!!
-
Page 4SDO EPO- DRAFTFEB2008
NAS
-
Page 5SDO EPO- DRAFTFEB2008
-
Page 6SDO EPO- DRAFTFEB2008
-
Page 7SDO EPO- DRAFTFEB2008
The very high energy radiations are absorbed in the upper atmosphere and do not penetrate to the earth’s surface.
-
Page 8SDO EPO- DRAFTFEB2008
The visible and infrared radiations reach the earth and determine our climate, create our weather, warm the earth’s surface, and, through re-radiation, warm its atmosphere.
-
Page 9SDO EPO- DRAFTFEB2008
But this portion of the spectrum remains unchanged year after year, varying at most only by fractions of one percent.
-
Page 10SDO EPO- DRAFTFEB2008
The portion we cannot see-- the radio waves, X rays, and otherhigh frequency and particle radiations-- do change markedly, according to solar activity.
-
Page 11SDO EPO- DRAFTFEB2008
By observing these changes, scientists learn much about the sun and earthand their relationships.
-
Page 12SDO EPO- DRAFTFEB2008
Putting a satellite into orbit is simply an extension of rocketry…
-
Page 13SDO EPO- DRAFTFEB2008
It may say aloft for years instead of only a few minutes, and it covers a wide range of latitudes or longitudes, or both.
-
Page 14SDO EPO- DRAFTFEB2008
Within less than an hour it can obtain data on both the day and night sides of the earth and the summer and winter regions.
-
Page 15SDO EPO- DRAFTFEB2008
…Satellites have already helped us make more precise measurements of the density of “empty”space.
-
Page 16SDO EPO- DRAFTFEB2008
They have encountered a band of intense solar radiation that appears to double every 60 miles above 250 miles to the greatest height yet reached.
-
Page 17SDO EPO- DRAFTFEB2008
So far, it appears that the radiation is trapped in this region by the earth’s magnetic field.
-
Page 18SDO EPO- DRAFTFEB2008
EVE EPOPast
•Pilot Project with MESA St. Vrain School District,Skyline High Cchool, Longmont, CO•Semester-long space-weather program for English Second Language Learners•Include the use of Sudden Ionospheric Disturbance (SID) Monitor
-
Page 19SDO EPO- DRAFTFEB2008
EVE EPOPresent
•Expanding into other MESA Schools (after and during school)•Developing and testing a space weather education kit•Materials available online•DVD with tour of LASP, interviews with scientists, overview of space weather
-
Page 20SDO EPO- DRAFTFEB2008
EVE EPOFuture
•Sharing EPO materials with other SDO programs on and after launch•Collaborating with LASP on Space Science Education Summit (June 08) and Journalist Workshop (Pre-launch)•Expand the network andemphasize best practices
-
Page 21SDO EPO- DRAFTFEB2008
SOLAR DYNAMICOBSERVATORY
-
Page 22SDO EPO- DRAFTFEB2008
The Solar Dynamics Observatory (SDO) is the first Living With a Star NASA mission.http://lws.gsfc.nasa.gov/
-
Page 23SDO EPO- DRAFTFEB2008
It will use telescopes to study the Sun’s magnetic field
-
Page 24SDO EPO- DRAFTFEB2008
The interior of the Sun
-
Page 25SDO EPO- DRAFTFEB2008
And changes in solar activity.
-
Page 26SDO EPO- DRAFTFEB2008
The primary goal of the SDO mission is to understand the solar variations that influence life on Earth
-
Page 27SDO EPO- DRAFTFEB2008
And humanity’s technological systems.
-
Page 28SDO EPO- DRAFTFEB2008
RESEARCH QUESTIONS
How is the Sun’smagnetic fieldgenerated andstructured?
-
Page 29SDO EPO- DRAFTFEB2008
RESEARCH QUESTIONS
How is the sun’s stored magnetic energyconverted and released into space?
-
Page 30SDO EPO- DRAFTFEB2008
RESEARCH QUESTIONSHow are solar wind, energetic particles, and variations in the solar irradiance formed?
-
Page 31SDO EPO- DRAFTFEB2008
SDO Provides HD Resolution Information
What information can you obtain from this image?
-
Page 32SDO EPO- DRAFTFEB2008
Versus this image?
• 50 times better spatial resolution
-
Page 33SDO EPO- DRAFTFEB2008
SDO Team
• NASA and three Instrument Teams are building SDO
– NASA/ Goddard Space Flight Center: build spacecraft, integrate the instruments, provide launch and mission operations
– Lockheed Martin & Stanford University: AIA & HMI
– LASP/University of Colorado: EVEAtlas V carries Rainbow 1 into orbit, July 2003.
-
Page 34SDO EPO- DRAFTFEB2008
SDO Data and Science
Images of Sun’s surface (photosphere)
-measuring magnetic field and probing the interior
Chromospheric & Coronal Imaging-pictures of the sun’s corona (outer layer)
Spectral Irradiance- -measuring specific intensity of Extreme
Ultraviolet (EUV)
-
Page 35SDO EPO- DRAFTFEB2008
• Mass: 3000 kg• Power: 1000 W• Width: 6 m• Height: 4.7 m
HMI
EVE
Instrument Module
S/C Bus & Prop. Modules
Solar Arrays
Antenna Booms
AIA SUITE
SDO Observatory
-
Page 36SDO EPO- DRAFTFEB2008
SDO Investigations:• Extreme Ultraviolet
Variability Experiment (EVE)
EVE
Solar Arrays
Antenna Booms
SDO Observatory
Measures the solar extreme ultraviolet (EUV) irradiance to understand variations, such as flares, that impact Earth.
-
Extreme Ultraviolet Radiation Extreme Ultraviolet Radiation
http://umbra.nascom.nasa.gov/http://sohowww.nascom.nasa.gov/
31JAN0316JAN03
Heliosphere
Corona
Chromosphere-TR
Surface Magnetic Field
Photosphere
2×106 K
8×104 K
6×103 K
11-year solar cycle
… varies continuously,by 50% to
100X
… emerges from the Sun’s outer layers (chromosphere, transition region, and corona)
EVE
From Judith Lean
-
Page 38SDO EPO- DRAFTFEB2008
EVE
-
Page 39SDO EPO- DRAFTFEB2008
EVE Data & Research
Measure Changes in Extreme Ultraviolet
EUV &X Rays Create Earth’s
Ionosphere
-
Page 40SDO EPO- DRAFTFEB2008
EVE Data & Research
All of the radiation measured by EVE is absorbed above 75 km, most above 100 km.
-
Page 41SDO EPO- DRAFTFEB2008
SDO Investigations:Helioseismic Magnetic
Imager (HMI)HMI
Solar Arrays
Antenna Booms
SDO Observatory
Images the Sun’s magnetic fields to understand the Sun’s interior and magnetic activity.
-
Page 42SDO EPO- DRAFTFEB2008
SOHO/MDI, January 14, 2004
HMI: “Seeing” Magnetic Fields
The Sun’s magnetic field.
One ‘day’ in the life of the Sun’s magnetic field (January 2004.)
-
Page 43SDO EPO- DRAFTFEB2008
Solar Cycle at the Poles
Potential to observe the solar polar field reversal
-
Page 44SDO EPO- DRAFTFEB2008
HMI: An Ultrasound of the Sun
Measuring Velocities Inside
the Sun
-
Page 45SDO EPO- DRAFTFEB2008
HMI: An Ultrasound of the Sun
Observing Solar Weather!
-
Page 46SDO EPO- DRAFTFEB2008
SDO Investigations:Atmospheric Imaging
Assembly (AIA)
Solar Arrays
Antenna Booms
AIA SUITE
SDO Observatory
High-resolution images of the corona over a wide range of temperatures.
-
Page 47SDO EPO- DRAFTFEB2008
AIA: It’s the Time Dependence
• HD images of the corona
• High-resolution & high-cadence views of solar activity and flares.
-
Page 48SDO EPO- DRAFTFEB2008
Summary
• Launch Date:January 2010
• Possible option : June 2009
HMI
EVE
Instrument Module
S/C Bus & Prop. Modules
Solar Arrays
Antenna Booms
AIA SUITE
-
Page 49SDO EPO- DRAFTFEB2008
http://sdo.gsfc.nasa.gov/
-
Page 50SDO EPO- DRAFTFEB2008
http://lasp.colorado.edu/eve/