Geomagnetic Field Modeling Lessons learned from Ørsted and CHAMP and prospects for Swarm Nils Olsen RAS Discussion Meeting on Swarm October 9 th 2009 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 1 / 43
Outline of Talk 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 2 / 43
Outline of Talk Exploring Earth s Magnetic Field from Space 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 3 / 43
Exploring Earth s Magnetic Field from Space Why should we measure magnetic field from space? Global coverage with ground observatories... and with 3 days of satellite data Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 4 / 43
Exploring Earth s Magnetic Field from Space Magnetic Field Model From Satellite Data B = grad V V = N n a + V ext n=1 m=0 r, θ, φ are spherical coordinates ( a ) n+1 [gn m cos mφ + hn m sin mφ] P m r n (cos θ) a is Earth s radius g m n and h m n are the spherical harmonic expansion coefficients of the internal magnetic field Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 5 / 43
Exploring Earth s Magnetic Field from Space Expansion Coefficients g m n, h m n of the Internal Field Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 6 / 43
Exploring Earth s Magnetic Field from Space Expansion Coefficients g m n, h m n of the Internal Field Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 6 / 43
Exploring Earth s Magnetic Field from Space Expansion Coefficients g m n, h m n of the Internal Field Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 6 / 43
Exploring Earth s Magnetic Field from Space Expansion Coefficients g m n, h m n of the Internal Field Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 6 / 43
Exploring Earth s Magnetic Field from Space Model Resolution Vector data 10,000 observations No external field Static internal field Perfectly polar orbit (inclination = 90 ) Vector data at all latitudes Ideal case: Perfect satellite, perfect environment,... Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 7 / 43
Outline of Talk Previous Missions: POGO and Magsat 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 8 / 43
Previous Missions: POGO and Magsat Satellite Missions: POGO Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 9 / 43
Previous Missions: POGO and Magsat Model Resolution Scalar data 10,000 observations No external field Static internal field Perfectly polar orbit (inclination = 90 ) Only intensity data strong Backus effect! Sectorial coefficients g n n, h n n are poorly determined Example: data from POGO satellite series (1965-72) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 10 / 43
Previous Missions: POGO and Magsat Model Resolution Scalar data 10,000 observations No external field Static internal field Perfectly polar orbit (inclination = 90 ) Only intensity data strong Backus effect! Sectorial coefficients g n n, h n n are poorly determined Example: data from POGO satellite series (1965-72) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 10 / 43
Previous Missions: POGO and Magsat Model Resolution Vector and scalar data 10,000 observations No external field Static internal field Perfectly polar orbit (inclination = 90 ) Vector data at non-polar latitudes (below ±60 ), else intensity data Vector data only needed at low latitudes to avoid Backus effect Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 11 / 43
Previous Missions: POGO and Magsat Satellite Missions: Magsat Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 12 / 43
Previous Missions: POGO and Magsat Model Resolution Vector and scalar data 10,000 observations No external field Static internal field Near polar orbit (inclination = 97 ) Vector data at non-polar latitudes (below ±60 ), else intensity data Zonal coefficients poorly determined due to polar gap Example: data from Magsat satellite (1979-80) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 13 / 43
Outline of Talk Present Missions: Ørsted, CHAMP and SAC-C 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 14 / 43
Present Missions: Ørsted, CHAMP and SAC-C Satellite Missions: Ørsted, CHAMP and SAC-C Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 15 / 43
Present Missions: Ørsted, CHAMP and SAC-C Present Satellites Satellites of the International Decade of Geopotential Research Ørsted Launched on 23th February 1999 Polar orbit, 650-850 km altitude all local times within 790 days (2.2 years) CHAMP Launched on 15th July 2000 low altitude (350-450 km) all local times within 130 days SAC-C Copy of Ørsted experiment Launched on 21th November 2000 700 km altitude, fixed local time 1030/2230 (no high-precision vector data due to payload failure) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 16 / 43
Present Missions: Ørsted, CHAMP and SAC-C Single satellites: Space-Time Ambiguity A low-earth-orbiting satellite moves with 8 km/s. It is difficult to distinguish whether an observed field change is due to a temporal field change or due to the movement of the satellite. Multi-point observations in space can resolve this ambiguity Satellite Constellation Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 17 / 43
Present Missions: Ørsted, CHAMP and SAC-C N Single Satellites vs. Constellation of N Satellites Data treated as multiple single-satellite observations Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 18 / 43
Present Missions: Ørsted, CHAMP and SAC-C N Single Satellites vs. Constellation of N Satellites Data treated as multiple single-satellite observations N satellites increase of number of data by N reduction of model error by N (if data are independent) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 18 / 43
Present Missions: Ørsted, CHAMP and SAC-C N Single Satellites vs. Constellation of N Satellites Data treated as multiple single-satellite observations N satellites increase of number of data by N reduction of model error by N (if data are independent) improvement less than N if data are not independent Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 18 / 43
Present Missions: Ørsted, CHAMP and SAC-C N Single Satellites vs. Constellation of N Satellites Data treated as multiple single-satellite observations N satellites increase of number of data by N reduction of model error by N (if data are independent) improvement less than N if data are not independent Take advantage of constellation: potential of improvement better than N Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 18 / 43
Outline of Talk Near Future: Swarm 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 19 / 43
Near Future: Swarm After Ørsted and CHAMP: Swarm Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 20 / 43
Near Future: Swarm The Swarm Concept ESA mission, to be launched in 2010 3 satellites: 2 side-by-side in low orbit 1 in higher orbit Three orbital planes with two different near-polar inclinations Science objectives Monitoring of core field changes after Ørsted and CHAMP Improved determination of the small-scale crustal field 3D mantle conductivity Magnetospheric and ionospheric current systems Magnetic forcing of the upper atmosphere Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 21 / 43
Near Future: Swarm The Swarm Concept ESA mission, to be launched in 2010 3 satellites: 2 side-by-side in low orbit 1 in higher orbit Three orbital planes with two different near-polar inclinations Science objectives Monitoring of core field changes after Ørsted and CHAMP Improved determination of the small-scale crustal field 3D mantle conductivity Magnetospheric and ionospheric current systems Magnetic forcing of the upper atmosphere Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 21 / 43
Near Future: Swarm Lower Pair of Swarm Satellites Measures Magnetic Field Gradient Pair of Swarm Satellites Measures Magnetic Field Gradient B r B θ B φ Swarm allows to measure the East-West Gradient, which is more sensitive to the small-scale lithospheric field Magnetic field East-West Gradient of Magnetic field 02.11.2007 Geophysical Colloquium, ETH Zurich page 32 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 22 / 43
Near Future: Swarm Advantage of two satellites flying side-by-side Quasi-complex representation of crustal field: B = Re{grad V } V = a ( a ) n+1 γ m r n Pn m e imφ n,m γ m n = g m n ih m n Difference of B at two satellites separated by φ in longitude: B = B(r, θ, φ) B(r, θ, φ + φ) 0 0 50 100 150 order m = Re{grad V } γn m = γn m ( 1 e im φ ) 1 e im φ m φ Sensitive to higher order m Filter gain 1 exp(i m φ) 2 1.8 1.6 1.4 1.2 1 0.8 0.6 0.4 0.2 φ = 1 o φ = 1.4 o φ = 2 o Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 23 / 43
Near Future: Swarm Model Resolution East-West gradient data 10,000 observations No external field Static internal field Near polar orbit (inclination = 97 ) East-West gradient data Zonal coefficients undetermined Enhanced resolution of sectorial coefficients Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 24 / 43
Near Future: Swarm End-To-End Mission Simulation Generation of synthetic orbits simulation starts on July 1, 1998 (one solar cycle before anticipated launch) simulation length of 4.5 years 24 18 Swarm A Swarm C Swarm C Swarm A 550 500 450 Local Time [hrs] 12 altitude [km] 400 350 6 300 Swarm C Swarm A 0 1998.5 1999 1999.5 2000 2000.5 2001 2001.5 2002 2002.5 2003 year 250 1998.5 1999 1999.5 2000 2000.5 2001 2001.5 2002 2002.5 2003 year 24 Swarm A Swarm C Swarm C Swarm A 18 Local Time [hrs] 12 6 0 1998.5 1999 1999.5 2000 2000.5 2001 2001.5 2002 2002.5 2003 year Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 25 / 43
Near Future: Swarm End-To-End Mission Simulation Magnetic Field Generation Core field time changes up to n = 19 Crustal field (static) up to n = 250 Ionospheric field, daily + seasonal periodicity Amplitude modulated by daily values of F10.7 Induced field by means of 1D conductivity model Magnetospheric field Time dependence of external coefficients up to n = 3, m = 0, 1 given by observatory data (hourly mean values) Induced field (up to n = 45) calculated using 3D mantle conductivity, including oceans Toroidal (non-potential) field daily + seasonal periodicity Instrument noise Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 26 / 43
Near Future: Swarm Crustal Field Recovery from B alone Single satellite approach degree error at ground 1 degree correlation 10 1 0.99 0.98 0.97 [nt] 10 0 degree correlation ρ n 0.96 0.95 0.94 10 1 0.93 0.92 10 2 signal Field only 20 40 60 80 100 120 140 degree n 0.91 0.9 20 40 60 80 100 120 140 degree n Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 27 / 43
Near Future: Swarm Crustal Field Recovery from B and [ B] EW Constellation approach degree error at ground 1 degree correlation 10 1 0.99 0.98 0.97 [nt] 10 0 degree correlation ρ n 0.96 0.95 0.94 10 1 0.93 0.92 10 2 signal Field only Field + Gradient 20 40 60 80 100 120 140 degree n 0.91 0.9 20 40 60 80 100 120 140 degree n Same observations in both cases, but different arrangement of data subsets Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 27 / 43
Crustal Field Recovery Near Future: Swarm Sensitivity matrix: relative error in %, normalized by mean power at that degree n Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 28 / 43
Near Future: Swarm Map of Crustal Field Difference using B only B r at surface, in nt Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 29 / 43
Near Future: Swarm Map of Crustal Field Difference using B and [ B] EW B r at surface, in nt Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 30 / 43
Near Future: Swarm Improvement of Lithospheric Field Model POGO and Magsat... n 30, resolution: 1330 km Magnetic field of Earths crust radial component at 10 km altitude Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 31 / 43
Near Future: Swarm Improvement of Lithospheric Field Model POGO and Magsat... n 30, resolution: 1330 km... with present satellites Ørsted and CHAMP... n 60, resolution: 670 km Magnetic field of Earths crust radial component at 10 km altitude Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 31 / 43
Near Future: Swarm Improvement of Lithospheric Field Model POGO and Magsat... n 30, resolution: 1330 km... with present satellites Ørsted and CHAMP... n 60, resolution: 670 km... and with Swarm n 130, resolution: 300 km Magnetic field of Earths crust radial component at 10 km altitude Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 31 / 43
Outline of Talk Recent Core Field Changes 1 Exploring Earth s Magnetic Field from Space 2 Previous Missions: POGO and Magsat 3 Present Missions: Ørsted, CHAMP and SAC-C 4 Near Future: Swarm 5 Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 32 / 43
Core field changes Recent Core Field Changes Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 33 / 43
Recent Core Field Changes Core field changes Ground observatory data monitor field change in time at a fixed location in space The role of observatory data: help in separating spatial and temporal variations when analyzing satellite data help in bridging the gap between satellite missions Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 33 / 43
Recent Core Field Changes Observatory monthly means monitor field change at fixed locations but: contain internal and external field contribution challenge: extraction of core field signal Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 34 / 43
Recent Core Field Changes Observatory monthly means monitor field change at fixed locations but: contain internal and external field contribution challenge: extraction of core field signal dy/dt [nt/yr] dy /dt at Niemegk/Germany 20 15 10 5 0 5 10 15 observed 20 1950 1960 1970 1980 1990 2000 annual differences of monthly means Scatter (partly) due to magnetospheric ring-current contributions Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 34 / 43
Revised monthly means Recent Core Field Changes 50 years (1958-2007) of hourly mean values from Niemegk Traditional way: arithmetic mean (all days, all local times) σ = 13.3 nt/yr σ = 4.7 nt/yr 40 15 NGK 20 30 10 15 20 5 10 σ = 11.6 nt/yr dx/dt [nt/yr] 10 0 10 20 dy/dt [nt/yr] 0 5 10 15 20 dz/dt [nt/yr] 5 0 5 10 15 20 30 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 35 / 43
Revised monthly means Recent Core Field Changes 50 years (1958-2007) of hourly mean values from Niemegk Traditional way: arithmetic mean (all days, all local times) σ = 13.3 nt/yr σ = 4.7 nt/yr 40 15 NGK 20 30 10 15 20 5 10 σ = 11.6 nt/yr dx/dt [nt/yr] 10 0 10 20 dy/dt [nt/yr] 0 5 10 15 20 dz/dt [nt/yr] 5 0 5 10 15 20 30 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year New: robust (Huber) average of data after correction for ionospheric and magnetospheric contributions 40 30 20 σ = 4.9 nt/yr NGK 15 10 5 σ = 1.9 nt/yr 20 15 10 1960 1970 1980 1990 2000 year σ = 3.3 nt/yr dx/dt [nt/yr] 10 0 10 20 dy/dt [nt/yr] 0 5 10 15 20 dz/dt [nt/yr] 5 0 5 10 15 20 30 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 35 / 43
Revised monthly means Recent Core Field Changes 50 years (1958-2007) of hourly mean values from Niemegk Traditional way: arithmetic mean (all days, all local times) σ = 13.3 nt/yr σ = 4.7 nt/yr 40 15 NGK 20 30 10 15 20 5 10 σ = 11.6 nt/yr dx/dt [nt/yr] 10 0 10 20 dy/dt [nt/yr] 0 5 10 15 20 dz/dt [nt/yr] 5 0 5 10 15 20 30 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year New: robust (Huber) average of data after correction for ionospheric and magnetospheric contributions 40 30 20 σ = 4.9 nt/yr NGK 15 10 5 σ = 1.9 nt/yr 20 15 10 1960 1970 1980 1990 2000 year σ = 3.3 nt/yr dx/dt [nt/yr] 10 0 10 20 dy/dt [nt/yr] 0 5 10 15 20 dz/dt [nt/yr] 5 0 5 10 15 20 30 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year 1960 1970 1980 1990 2000 year Standard deviation σ (wrt a GCV spline fit) is reduced by a factor of 3 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 35 / 43
Recent Core Field Changes The CHAOS Field Model Series CHAOS 6.5 years of satellite data (March 1999 and December 2005) Order 4 splines up to spherical harmonic degree n = 14, static up to n = 50 Regularization of < B 2 > at Earth s surface CHAOS-2 10 years of satellite data (March 1999 and March 2009) Observatory monthly means (1997-2006) Order 6 splines up to n = 20, static for n = 21 60 Regularization of < B 2 > at Core-Mantle Boundary (CMB) CHAOS-3 10.5 years of satellite data (March 1999 and August 2009) Revised observatory monthly means (1997-2009) Order 6 splines up to n = 20, static for n = 21 60 Regularization of < d 3 B/dt 3 2 > at CMB Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 36 / 43
Recent Core Field Changes CHAOS-3 Data Selection Distribution of non-polar data 16000 14000 CHAMP scalar CHAMP vector Oersted scalar Oersted vector SAC C scalar total number of data points per month 12000 10000 8000 6000 4000 2000 0 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 year stacked histogram Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 37 / 43
Recent Core Field Changes Spectrum of first and second time derivative at t = 2005.0 10 4 10 3 CHAOS 2 CHAOS 3 [(nt/yr) 2 or (nt/yr 2 ) 2 10 2 10 1 10 0 first time derivative 10 1 second time derivative 10 2 10 3 0 2 4 6 8 10 12 14 16 18 20 degree n CHAOS-3 shows less secular acceleration power at n = 1, more power at n > 6 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 38 / 43
Fit to observatory data Recent Core Field Changes CHAOS-2 CHAOS-3 component mean rms mean rms Ẋ [nt/yr] -2.74 13.42 0.02 7.35 Ẏ [nt/yr] 0.17 11.41-0.02 5.02 Ż [nt/yr] 0.92 9.91-0.10 7.02 CHAOS-3 rms misfit reduced by factor 2 for X and Y, and by 30% for Z The non-zero mean values of CHAOS-2 are not present in CHAOS-3 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 39 / 43
Fit to observatory data Recent Core Field Changes CHAOS-2 CHAOS-3 component mean rms mean rms Ẋ [nt/yr] -2.74 13.42 0.02 7.35 Ẏ [nt/yr] 0.17 11.41-0.02 5.02 Ż [nt/yr] 0.92 9.91-0.10 7.02 CHAOS-3 rms misfit reduced by factor 2 for X and Y, and by 30% for Z The non-zero mean values of CHAOS-2 are not present in CHAOS-3 Also satellite rms misfit data is slightly lower for CHAOS-3 compared to CHAOS-2 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 39 / 43
Recent Core Field Changes Fit to observatory data dx/dt [nt/yr] 5 0 5 10 15 20 25 KAK X 1998 2000 2002 2004 2006 2008 2010 dy/dt [nt/yr] 0 5 10 15 KAK Y CHAOS 2 CHAOS 3 1998 2000 2002 2004 2006 2008 2010 dz/dt [nt/yr] 35 KAK Z 30 25 20 15 10 5 0 5 1998 2000 2002 2004 2006 2008 2010 dx/dt [nt/yr] 0 5 10 15 20 25 HER X 1998 2000 2002 2004 2006 2008 2010 dy/dt [nt/yr] 8 10 12 14 16 18 20 22 24 HER Y 26 1998 2000 2002 2004 2006 2008 2010 dz/dt [nt/yr] HER Z 80 70 60 50 40 1998 2000 2002 2004 2006 2008 2010 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 40 / 43
Conclusions Conclusions Bright future for space magnetometry (until 2015?) Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 41 / 43
Conclusions Conclusions Bright future for space magnetometry (until 2015?) Constellation aspect: 1+1+1 is sometimes more than 3 Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 41 / 43
Conclusions Conclusions Bright future for space magnetometry (until 2015?) Constellation aspect: 1+1+1 is sometimes more than 3 changed role of ground observatory data Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 41 / 43
Conclusions Nils Olsen (DTU Space) Ørsted, CHAMP, and Swarm 42 / 43