NOAA GOES and POES Data: Contributions to

Radiation Belt Storm Probes’ Science

Howard J. Singer and Janet Green NOAA Space Weather Prediction Center

RBSP Science Working Group Meetng Boulder, CO

August 31, 2010

AF-Geospace, Courtesy of Greg Ginet, AFRL

Acknowledgments: Terry Onsager, Juan Rodriguez, and Paul Loto’aniu

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Presentation Outline:   Introduction  GOES Observations During

the RBSP Mission  POES Observations  Science Challenges  Summary

NOAA GOES and POES Data: Contributions to Radiation Belt Storm Probes’ Science

Structure

Effects Dynamics

AF-Geospace

Singer, Bouwer, and Onsager

1993 2002 2

7

L Va

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Dst

-40

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SAMPEX: EL0/Electrons, 2-6 MeV

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The locations of the GOES-R fleet. Two operational satellites positioned at 137 degrees West longitude for the Western Operational station, And at 75 degrees West longitude for the Eastern Operational station. During the on-orbit storage period, the satellites will be positioned at 105 degrees West longitude and a Launch/Check-out position is reserved at 90 degrees West longitude. (Currently, GOES West is at 135 degrees west, but this will be changing to 137 degrees west.)

GOES Locations

On-orbit GOES storage Operational

Calendar Year 2027 2026 2025 2024 2023 2022 2021 2020 2019 2018 2017 2016 2015

GOES 14

GOES 15

GOES R

2014 2013 2012 2011 2010 2009

GOES 13

GOES 12

GOES 11

2007 2008

GOES 10 Backup

GOES East

GOES West

On-orbit Spare

Continuity of GOES Operational Satellite Program

GOES S

Satellite is operational beyond design life

9/4/2008

2028

This chart is updated frequently depending on factors such as satellite and instrument condition. Chart has been modified to show GOES NOP (13,14,15) have been launched.

5/24/06

6/27/09

3/4/10

GOES NOP Magnetometer Specifications

Multipoint Investigations of Magnetic Storms and Radiation Belts 6

Multipoint Investigations of Magnetic Storms and Radiation Belts 7

Geosynchronous Satellite Particle Data

 3 Satellite Series  GOES (I-M) 11  GOES (NOP) 13-15  GOES-R

NOP

NOP NOP

GOES NOP (13, 14, 15) Energetic Particle Sensors

Magnetospheric Electron Detector (MAGED): 9 look directions for (5 azimuth and 5 elevation with shared center) 5 energy channels in each look direction: 30 keV – 600 keV

Magnetospheric Proton Detector (MAGPD): 9 look directions for (5 azimuth and 5 elevation with shared center) 5 energy channels in each look direction: 80 keV – 800 keV

Energetic Proton Electron and Alpha Detector (EPEAD): 2 look directions (East and West) 3 electron energy channels: > 0.8 MeV, > 2 MeV, > 4 MeV 7 proton energy channels: 0.7 – 900 MeV 6 alpha particle energy channels: 4 – 500 MeV

High Energy Proton and Alpha Detector (HEPAD): 1 look direction 4 proton energy channels: 330 – >700 MeV 2 alpha particle channels: 2560 – >3400 MeV

NEW

NEW

NEW

Electron energy coverage of GOES I-M, GOES NOP, and GOES R+.

Adapted from J. E. Mazur, Summary Report, Workshop on Energetic Particle Measurements for the GOES R+ Satellites, Held at NOAA SEC, October 28-29, 2002

MAGED EPEAD

EPS

MPS-Lo MPS-Hi

NOP

Proton energy coverage of GOES I-M, GOES NOP, and GOES R+.

Adapted from J. E. Mazur, Summary Report, Workshop on Energetic Particle Measurements for the GOES R+ Satellites, Held at NOAA SEC, October 28-29, 2002

MAGPD EPEAD

EPS

MPS-Lo MPS-Hi SGPS

NOP

EP

EA

D

Ele

ctro

n fl

ux

MA

GE

D

Ele

ctro

n fl

ux

MA

GP

D

Pro

ton

flux

Mag

netic

Fi

eld

>.8, >2,4 MeV electrons

Thick lines are telescopes nearest loss cone

Observations 1)Proton pitch angle distribution flattens 2)Followed by electron flux increase 3)Little change in magnetic field

12 LT 10 LT

80-110 keV protons

30-50 keV electrons

New Data: MAGED/MAGPD

Explanation 1)Substorms inject electrons & protons 2)Particles drift in opposite directions 3)80 keV protons reach noon first

Questions Is proton injection isotropic or are they isotropized as they drift?

J. Green, COSPAR, 2010

Magnetic waves in the azimuthal and radial components with a few second period and about 0.5 nT p-p amplitude observed between 1800 and 1805 UT, corresponding to the second injection of protons and electrons shown in the previous figure.

Demonstrates capabilities of GOES 13, 14, 15 magnetic observations to observe high-frequency ion cyclotron waves.

GOES-14 Magnetometer Observations Aug 27, 2009 1800-1805 UT

GOES R+ Energetic Particle Sensors (All New)

Energetic Heavy Ion Sensor (EHIS): 1 look direction 10-200 MeV/nucleon in 5 bands 5 mass groups (H, He, CNO, Ne-S, Fe group)

Solar and Galactic Proton Sensors (SGPS): 2 look directions (East and West) 10 proton energy channels (1-500 MeV) + >500 MeV integral 10 alpha energy channels (4-500 MeV)

Magnetospheric Particle Sensor-Hi (MPS-Hi): 5 look directions 10 electron energy channels (50 keV – 4 MeV)+ >2 MeV integral 7 proton energy channels (80 keV – 10 MeV)

Magnetospheric Particle Sensor-Lo (MPS-Lo): 14 look directions 30 eV – 30 keV, 15 bands, electrons and protons (ions)

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GOES 13,14, 15 Contribute Solar as well as in-situ Observations for RBSP

GOES 13, 14, 15 Enhancements Magnetometer (MAG)

•  Two instruments operating simultaneously

Energetic Particle Sensors (EPS) •  Lower energy electron (30 keV) and

proton (80 keV) bands •  More look-directions

X-Ray Sensor (XRS) •  Eliminate electronic range-changing

EUV Sensor (EUVS) •  New instrument, five wavelength

bands 10 - 125 nm Solar X-Ray Imager (SXI)

•  Improved sensitivity and resolution •  Autonomous event response

Polar Satellite Particle Data  POES/METOP

 SEM2  NOAA-15,16,17,18,19  METOP-1, METOP-2 (launch

2012)  NPOESS (SEM-N instruments prior

to split into NOAA JPSS and DOD DWS-likely delaying any new sensors until 2018)

Total Energy Detector (TED) - electrons and ions 50 eV – 20 keV; zenith and 30 deg to zenith

- 4 energy bands telemetered, selected from 16, at a low duty cycle - 2 s data rate

- Flux in energy band containing max flux together with energy band number

- Integrated (50 eV to 20 keV) directional energy flux, electrons and ions at each of the two viewing directions

Medium Energy Proton and Electron Detector (MEPED) - electrons: 30 keV – 2.5 MeV; zenith and 90 deg to zenith;

3 energy channels (proton contamination significant in field aligned direction) - ions: 30 keV – 6.9 MeV; zenith and 90 deg to zenith; 6 energy channels (P6 channel detects ~ 1 MeV electrons) - omni-directional detector, nearly one hemisphere, protons 16 MeV - >140 MeV; 4 energy channels

- 2 s data rate except for two highest energy omni-directional channels

POES Space Environment Monitor 2 (SEM 2)

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Radiation Belt Structure and Dynamics: A Balance of Sources and Losses

Acceleration Processes   Adiabatic   VLF chorus: pitch angle and energy diffusion   ULF waves: radial diffusion   Interplanetary shocks

Loss Processes   Adiabatic   Magnetopause   Plasmaspheric hiss   Electromagnetic Ion

Cyclotron waves   Dayside VLF chorus

(Reeves, SWJ 2007; adapted from Summers et al. JGR 1998) (see also Liemohn and Chan, EOS, Oct 2007)

GOES magnetic field and particle observations, just beyond the RBSP apogee, provide additional multipoint observations needed to characterize most of these processes (except for VLF and hiss).

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Magnetospheric Activity for 1995 Stream Interfaces

Solar Wind Drivers and Magnetospheric Response •  Large fluctuations in Ey at the interface, and following, responsible for intense activity that weakens with time as shown by quartiles of ap and Sym-H •  Pc 5 ULF wave activity enhanced at and following the interface and may contribute to acceleration of relativistic electrons shown by a 2-order of magnitude flux increase after drop out at the interface • It appears that the combination that produces relativistic electrons is prolonged high solar wind velocity, continuous geomagnetic activity, and prolonged ULF wave activity. Maybe other factors not considered here.

McPherron and Weygand (2005) AGU Monograph

Velocity

Ey

ap

Sym-H Pc5

Geo MeV e

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Multisatellite Observations Examine the Energization of Relativistic Electrons

Chen, Reeves, and Friedel, Nature, July 2007

•  Utilize GPS, LANL, and Polar spacecraft to distinguish between acceleration by radial diffusion or gyro-resonant wave-particle interactions •  Construct phase space density (PSD) at fixed adiabatic invariants •  Examine the shape of the PSD profile to differentiate between diffusive and local acceleration

GOES needed for L values beyond RBSP

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Why do we need multiple spacecraft in LWS and RBSP to reach science closure?

The two RBSP spacecraft will address several “local” acceleration questions

The third spacecraft—ORBITALS—will give the global local time, radial, and latitude separation to answer key questions fully!

Courtesy Ian Mann

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The ‘Great Debate’

Harlow Shapley Heber D. Curtis

April 26, 1920: Shapley and Curtis on “The Scale of the Universe” What is the size of our galaxy and the nature of spiral nebula?

Andromeda Galaxy

Shapley correct about position of sun in the Milky Way galaxy Curtis correct about spiral nebula being separate galaxies In the end, each supported both correct and incorrect views.

Partial resolution in mid-20’s using the 100” Hooker Telescope at Mt. Wilson when Hubble identified Cepheid variables in Andromeda that could be used to determine distance.

Like this debate, our community is engaged in a major scientific debate with competing ideas about the processes responsible for the acceleration and loss of relativistic electrons. Who is right? Are there aspects of different views that are correct/incorrect? Will the NASA Radiation Belt Storm Probes and other multipoint observations help to resolve the controversies?

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Conclusions

•  GOES and POES satellites will contribute to RBSP science •  GOES, at multiple geosynchronous locations, offers in situ observations of Earth’s magnetic field and energetic particle environment, as well as solar observations •  GOES will make measurements of the background field and particle environment at the outer boundary of the RBSP satellites. These observations will include such features as PSD, ULF waves, ring current, substorms, storms… •  Radiation Belt Storm Probes, together with existing GOES, POES, and other satellite and ground-based observations, and modeling, provide the opportunity to solve long-standing and ‘great problems’ about the radiation belt acceleration and loss processes.