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Table 1 Comparison of the CHAOS-4 and CHAOS-5 geomagnetic field models

From: DTU candidate field models for IGRF-12 and the CHAOS-5 geomagnetic field model

 

CHAOS-4

CHAOS-5

Data sources

  

Observatory monthly means

June 1997 - June 2013

June 1997 - Sept 2014

Ørsted vector

March 1999 - Dec 2004

March 1999 - Dec 2004

Ørsted scalar

March 1999 - June 2013

March 1999 - June 2013

SAC-C scalar

Jan 2001 - Dec 2004

Jan 2001 - Dec 2004

CHAMP vector and scalar

Aug 2000 - Sept 2010

Aug 2000 - Sept 2010

Swarm A vector and scalar

Nov 2013 - Sept 2014

Swarm B vector and scalar

Nov 2013 - Sept 2014

Swarm C vector and scalar

Nov 2013 - Sept 2014

Time-dependent internal field

  

Model time span

1997.0–2013.5

1997.0–2015.0

Spherical harmonic degree

n=1–20

n=1–20

Spline basis

6th order, 0.5 year knots

6th order, 0.5 year knots

Based on

CHAOS-4l

CHAOS-5l

Static internal field

  

Spherical harmonic degree

n=21–90

n=21–90

Based on

CHAOS-4l (n=21–24)

CHAOS-5l (n=21–24)

 

and CHAOS-4h (n=25–90)

and CHAOS-4h (n=25–90)

External field

  

SM

n=1: 1 h, RC int + ext

n=1: 1 h, RC int + ext

 

5 day \(\Delta {q^{0}_{1}}\), 30 day \(\Delta {q^{1}_{1}}\), \(\Delta {s^{1}_{1}}\)

5 day \(\Delta {q^{0}_{1}}\), 30 day \(\Delta {q^{1}_{1}}\), \(\Delta {s^{1}_{1}}\)

 

n=2: static

n=2: static

GSM

n=1–2, m=0: static

n=1–2, m=0: static

Euler angles

  

Ørsted

Before and after Jan 24 2000

Before and after Jan 24 2000

CHAMP

10 day bins

10 day bins

Swarm

10 day bins

Regularization

  

Spatial

Static field n>85, \(<{B_{r}^{2}}>\)

Static field n>85, \(<{B_{r}^{2}}>\)

 

λ 0=1 nT−2

λ 0=1 nT−2

Temporal, interior

\(<(d{B^{3}_{r}}/dt^{3})^{2}>\)

\(<(d{B^{3}_{r}}/dt^{3})^{2}>\)

 

λ 3=0.33 (nT/year−3)−2

λ 3=0.33 (nT/year−3)−2

 

except \({g^{0}_{1}}\), λ 3=10 (nT/year−3)−2

except m=0, λ 3=100 (nT/year −3)−2

Temporal, endpoints

\(<(d{B^{2}_{r}}/dt^{2})^{2}>\)

\(<(d{B^{2}_{r}}/dt^{2})^{2}>\)

 

λ 2=10 (nT/year−2)−2

λ 2=100 (nT/year −2)−2

  1. Contributing data, model parameterization and model regularization are presented. Improvements of CHAOS-5 compared to CHAOS-4 are shown in bold. <> indicates integration over the core-mantle boundary