11 mccaffrey eve epo -...

SDO EPO- DRAFTFEB2008

EVEEPO


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


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!!


NAS


The very high energy radiations are absorbed in the upper atmosphere and do not penetrate to the earth’s surface.


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.


But this portion of the spectrum remains unchanged year after year, varying at most only by fractions of one percent.


The portion we cannot see-- the radio waves, X rays, and otherhigh frequency and particle radiations-- do change markedly, according to solar activity.


By observing these changes, scientists learn much about the sun and earthand their relationships.


Putting a satellite into orbit is simply an extension of rocketry…


It may say aloft for years instead of only a few minutes, and it covers a wide range of latitudes or longitudes, or both.


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.


…Satellites have already helped us make more precise measurements of the density of “empty”space.


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.


So far, it appears that the radiation is trapped in this region by the earth’s magnetic field.


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


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


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


SOLAR DYNAMICOBSERVATORY


The Solar Dynamics Observatory (SDO) is the first Living With a Star NASA mission.http://lws.gsfc.nasa.gov/


It will use telescopes to study the Sun’s magnetic field


The interior of the Sun


And changes in solar activity.


The primary goal of the SDO mission is to understand the solar variations that influence life on Earth


And humanity’s technological systems.


RESEARCH QUESTIONS

How is the Sun’smagnetic fieldgenerated andstructured?


RESEARCH QUESTIONS

How is the sun’s stored magnetic energyconverted and released into space?


RESEARCH QUESTIONSHow are solar wind, energetic particles, and variations in the solar irradiance formed?


SDO Provides HD Resolution Information

What information can you obtain from this image?


Versus this image?

• 50 times better spatial resolution


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.


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)


• 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


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


EVE


EVE Data & Research

Measure Changes in Extreme Ultraviolet

EUV &X Rays Create Earth’s

Ionosphere


EVE Data & Research

All of the radiation measured by EVE is absorbed above 75 km, most above 100 km.


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.


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.)


Solar Cycle at the Poles

Potential to observe the solar polar field reversal


HMI: An Ultrasound of the Sun

Measuring Velocities Inside

the Sun


HMI: An Ultrasound of the Sun

Observing Solar Weather!


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.


AIA: It’s the Time Dependence

• HD images of the corona

• High-resolution & high-cadence views of solar activity and flares.


Summary

• Launch Date:January 2010

• Possible option : June 2009

HMI

EVE

Instrument Module

S/C Bus & Prop. Modules

Solar Arrays

Antenna Booms

AIA SUITE


http://sdo.gsfc.nasa.gov/


http://lasp.colorado.edu/eve/

11 mccaffrey eve epo -...

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