The Swarm Satellite Constellation Application and Research Facility (SCARF) and Swarm data products
- Nils Olsen1Email author,
- Eigil Friis-Christensen1,
- Rune Floberghagen2,
- Patrick Alken3, 4,
- Ciaran D. Beggan5,
- Arnaud Chulliat3,
- Eelco Doornbos6,
- João Teixeira da Encarnação6,
- Brian Hamilton5,
- Gauthier Hulot3,
- Jose van den IJssel6,
- Alexey Kuvshinov7,
- Vincent Lesur8,
- Hermann Lühr8,
- Susan Macmillan5,
- Stefan Maus4,
- Max Noja8,
- Poul Erik H. Olsen1,
- Jaeheung Park8,
- Gernot Plank9,
- Christoph Püthe7,
- Jan Rauberg8,
- Patricia Ritter8,
- Martin Rother8,
- Terence J. Sabaka10,
- Reyko Schachtschneider8,
- Olivier Sirol3,
- Claudia Stolle1, 8,
- Erwan Thébault3,
- Alan W. P. Thomson5,
- Lars Tøffner-Clausen1,
- Jakub Velímský11,
- Pierre Vigneron3 and
- Pieter N. Visser6
© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB. 2013
Received: 30 March 2013
Accepted: 1 July 2013
Published: 22 November 2013
Swarm, a three-satellite constellation to study the dynamics of the Earth’s magnetic field and its interactions with the Earth system, is expected to be launched in late 2013. The objective of the Swarm mission is to provide the best ever survey of the geomagnetic field and its temporal evolution, in order to gain new insights into the Earth system by improving our understanding of the Earth’s interior and environment. In order to derive advanced models of the geomagnetic field (and other higher-level data products) it is necessary to take explicit advantage of the constellation aspect of Swarm. The Swarm SCARF (SatelliteConstellationApplication andResearchFacility) has been established with the goal of deriving Level-2 products by combination of data from the three satellites, and of the various instruments. The present paper describes the Swarm input data products (Level-1b and auxiliary data) used by SCARF, the various processing chains of SCARF, and the Level-2 output data products determined by SCARF.
Key wordsEarth’s magnetic field core field lithosphere ionosphere magnetosphere electromagnetic induction comprehensive inversion Swarm satellites
Swarm, a constellation mission comprising three identical satellites to study the dynamics of the Earth’s magnetic field and its interactions with the Earth system (Friis-Christensen et al., 2006, 2008) is expected to be launched in late 2013. The objective of the Swarm mission is to provide the best ever survey of the geomagnetic field and its temporal evolution, in order to gain new insights into the Earth system by improving our understanding of the Earth’s interior and environment.
Each of the three Swarm satellites will make high-precision and high-resolution measurements of the strength, direction and variation of the magnetic field, complemented by precise navigation, accelerometer, plasma and electric field measurements. These observations will be provided as Level-1b data, which are the calibrated and formatted time series of e.g. the magnetic field measurements taken by each of the three Swarm satellites. These Level-1b data, as well as the higher-Level Swarm data products described in this paper, will be distributed by ESRIN (Frascati/I).
Swarm will simultaneously obtain a space-time characterisation of both the internal field sources in the Earth and the ionospheric-magnetospheric current systems. The research objectives assigned to the mission are: (a) studies of core dynamics, geodynamo processes, and core-mantle interaction; (b) mapping of the lithospheric magnetisation and its geological interpretation; (c) determination of the 3-D electrical conductivity of the mantle; and (d) investigation of electric currents flowing in the magnetosphere and ionosphere.
A challenging part, however, is the separation of the various sources (in the core, lithosphere, ionosphere, magne-tosphere etc.) which in total yields the measured magnetic field. A constellation consisting of several satellites, like Swarm, opens new possibilities for exploring the geomagnetic field from space beyond those achievable with single-satellites. At first glance one would expect that using simultaneous data from N satellites results in a reduction of the error of geomagnetic field models by , since the amount of data is increased by N compared to one single satellite. This error reduction by of course only holds if the data are statistically independent, which is highly idealistic and unrealistic since the main limiting factor for improved field modelling is not the measurement error but the dynamic behaviour of external sources. Treating data from a constellation of N satellites in a “single-satellite” approach thus typically results in an improvement of the model error by less than . However, if explicit advantage is taken of the constellation, there is some potential for model improvement better than . A constellation of three satellites can do more than three single satellites, and therefore a (SMART) combination of data from all three satellites, and of the various instruments, allows for taking full advantage of the Swarm constellation. Analysis of the Swarm data will greatly improve existing and provide new models of the near-Earth magnetic field of high resolution and authenticity compared to what is possible with single-satellite missions like Ørsted (Olsen, 2007) and CHAMP (Reigber et al., 2005).
In recognition of the large effort needed to extract the various types of scientific information from the complex set of observations a group of institutions and organisations have joined the SMART consortium (SwarmMagnetic andAtmosphericResearchTeam). The purpose of the consortium is to contribute to the optimal science return from the Swarm mission by a coordinated effort to exploit the constellation aspects of this unique mission. This effort is obviously in accordance with ESA’s aim of providing the scientific community with the best possible products from the Swarm mission, and it was decided to establish a SwarmSCARF (SatelliteConstellationApplication andResearchFacility), with the purpose of deriving commonly used scientific models and quantities, the so-called Level-2 products and make them available to the scientific community at large. Advanced Swarm-derived models of the geomagnetic field and other Level-2 data products are determined from the Level-1b data and auxiliary (i.e. non-Swarm) data and provide the prospect of investigating hitherto undetected features of the Earth’s interior.
SCARF (sometimes also called “Level-2 Processing S>ystem”, L2PS) comprises in its present form a joint effort between the six European partners: DTU (Lyngby/DK), TU Delft (Delft/NL), BGS (Edinburgh/GB), ETH (Zürich/CH), GFZ (Potsdam/D) and IPGP (Paris/F) with contributions from CUP (Prague/CZ), NOAA (Boul-der/USA) and GSFC/NASA (Greenbelt/USA). The team behind SCARF has designed and implemented algorithms to derive advanced models of the geomagnetic field describing sources in the core, lithosphere, ionosphere and mag-netosphere, models of the electrical conductivity of Earth’s mantle and time series of thermospheric wind and density at the positions of the Swarm satellites. These models, which are state-of-the-art implementations of current knowledge, are intended to facilitate and increase the use of the Swarm data by a much wider community than the one represented in the SMART consortium itself.
The work performed by SCARF is a major extension on the “End-To-End” mission simulation that has been performed during Phase A of the Swarm mission, the results of which have been published in a special issue (Vol. 58 No. 4, 2006) of Earth, Planets and Space (cf. Olsen et al., 2006 for an overview).
The present paper describes the Swarm input data products (Level-1b and auxiliary data) used by SCARF, the various processing chains of SCARF, and the Level-2 output data products determined by SCARF and distributed by ESA through the PDGS (Payload Data Ground Segment) at ESRIN.
The content of the paper is as follows: Section 2 summarizes the various Level-1b data, with emphasis on the 1 Hz time series of the magnetic field observations. Section 3 describes the various processing chains and resulting Level-2 data products. All processing chains have been tested using synthetic data from a full mission simulation; the creation of this synthetic data set is described in Section 4. Data processing time-line and data availability are discussed in Section 5.
2. Swarm Level-1b Products
Content of Swarm Level-1b Product MAGx_LR.
Time of observation
Time reference information
Latitude of observation in the International Terrestrial Reference Frame (ITRF)
Longitude of observation in the ITRF
Radius of observation in ITRF
Magnetic field intensity
Magnetic stray field correction intensity related to attitude control magneto-torquers
Magnetic stray field correction intensity of all other sources
Error estimate on magnetic field intensity
Magnetic field vector in the instrument frame of the VFM magnetometer
Magnetic field vector in the NEC (North, East, Center) frame
Magnetic stray field correction vector related to attitude control magneto-torquers (in VFM frame)
Magnetic stray field correction vector of all other sources (in VFM frame)
Error estimates on magnetic field vector BVFM (in VFM frame)
Rotation from NEC frame to STR Common Reference Frame (CRF), quaternion (NEC ← CRF)
Error estimate on attitude information
Flags characterizing the magnetic field intensity measurement: spikes or gap in data, discrepancy between ASM and VFM, etc.
Flags characterizing the magnetic field vector measurement BVFM and BNEC: spikes or gap in data, discrepancy between ASM and VFM, etc.
Flags characterizing the attitude information: identification of active heads, blinding, etc.
Flags characterizing the spacecraft platform information: thruster activation, lack of telemetry, etc.
ASM reference frequency calibration data deviation for ASM stability assessment
The quality of Level-1b magnetic and plasma products MAGx_LR and EFIx_PL can be inspected using quick-look products, essentially comprising various daily and mission-to-date plots designed to reveal a range of possible measurement problems (Beggan et al., 2013).
The positions provided in the Level-1b data are generated automatically as part of the Level-1b processing as “Medium Precise Orbits” (MOD) with an expected accuracy not exceeding a few meters. In case higher precision of the position is needed (or for periods where the MOD automatic calculation yields less optimal results) it is recommended to use the positions provided by the “Precise Orbit Determination” (POD) chain (Level-2 product SP3xCOM_2_) discussed in Section 3.2.
3. Swarm Level-2 Data Processing and Products
Depending on the complexity of the processing, there are two types of Level-2 products, which are called Cat-1 and Cat-2 products, respectively. Cat-1 data processing involves complex algorithms to derive Level-2 products describing specific sources of the Earth’s magnetic field like the lithospheric field or time series of the large-scale mag-netospheric signal. Cat-1 products are derived by SCARF since scientific expertise is required during processing. In contrast, processing of Cat-2 products is less demanding, and therefore these products are derived by ESA on a daily basis in ESA’s Swarm PDGS using algorithms designed by SCARF. The processing runs automatically, leading to product release with minimum delay; Cat-2 products are tested for their near real time capability with processing delays of less than 1 hour. Cat-2 products are therefore suitable e.g. for space weather applications (Stolle et al., 2013).
The Swarm Level-2 products.
(needed for Level-1b processing)
Time series of Euler angles describing transformation from STR-CRF to VFM frame for all three Swarm satellites (3 × 3 Euler angles)
Spherical harmonic model of the core field and its temporal variation
Spherical harmonic model of the lithospheric field
Electrical conductivity of the mantle
1D model of mantle conductivity
3D model of mantle conductivity
3D C-response maps
External current systems
Spherical harmonic model of the large-scale magnetospheric field and its Earth-induced counterpart
Spherical harmonic model of the daily geomagnetic variation at middle latitudes (Sq) and low latitudes (EEJ)
Precise Orbit Determination (POD)
Time series of position and velocity of the center of mass for satellite x (x = A, BorC)
Accelerometer calibration parameters for satellite x
Time series of non-gravitational accelerations estimated for satellite x
Magnetic Forcing of the Upper Atmosphere
Time series of calibrated and pre-processed accelerometer observations and of aerodynamic accelerations for satellite x
Time series of neutral thermospheric density and wind speed for satellite x
Earth environment and Space-Weather (Cat-2 products)
Ionospheric bubble index for satellite x
Time series of the ionospheric total electron content for satellite x
Time series of field-aligned currents determined from combination of Swarm A and Swarm B
Time series of field-aligned currents (single-satellite solution) for satellite x
Equatorial Electric Field for satellite x
3.1 Level-2 products related to main magnetic sources
In addition to auxiliary data, the processing also requires auxiliary models like the IGRF (AUX_IGR_2_) or more advanced models of the core field (AUX_COR_2_) and the lithospheric field (AUX_LIT_2_). Models of the electrical conductivity of the Earth’s mantle (AUX_MCM_2_) and of the surface conductance of oceans and sediments (AUX_OCM_2_) are used to account for secondary, Earth-induced contributions connected to the temporal variations of magnetospheric and ionospheric origin. Finally, a model of the magnetic signature of ocean tides (AUX_MTI_2_) is provided.
In the following we briefly discuss the various Level-2 products.
Spherical Harmonic Models of the core, lithospheric, ionospheric and magnetospheric field. Models of the core field and its time changes are provided as spherical harmonic expansion coefficients in the Level-2 product MCO_SHA_2_ (where “M” indicates that the product describes a Magnetic source, “CO” stands for COre field, “SHA” denotes that the model is given as an expansion of a Spherical Harmonic Analysis, and “2” refers to the fact that this is a Level-2 data product. The last character, in this example “_”, indicates the generic form of the Level-2 product; other values are “C” if the product is derived in the Comprehensive Inversion chain or “D” if the product is derived in one of the Dedicated Inversion chains.)
For the core field models these are chosen to be Nmin = 1, Nmax = 18 and the time dependence of the Gauss coefficients is parametrized using B-splines; however, the final product MCO_SHA_2_ contains a series of snapshot models (corresponding to order 6 splines and 6 months separation of the spline knots). Details of the data format, and how to transform back from the snapshot representation to the original spline representation, are given in the Level-2 Product Definition Document (Swarm Level 2 Processing System Consortium, 2013).
Core field model version MCO_SHA_2C is derived in the Comprehensive Inversion chain (see Sabaka et al. (2013) for details), while model version MCO_SHA_2D is derived in the Dedicated Inversion chain (Rother et al., 2013).
A proper determination of the Euler anglesα, β, γ describing the rotation between the instrument frames of the vector magnetometer and star tracker (see Eq. (2)) is only possible in-orbit. A pre-flight determination made on ground is limited e.g. by atmospheric turbulence to an accuracy of, say, 20 arc-seconds since global data coverage is required in order to obtain Euler angles within a few arc-seconds. This is only possible in-orbit. A determination of the Euler angles by co-estimation with all major contributions to the near-Earth magnetic field is made in the Comprehensive Inversion chain (Sabaka et al., 2013), and an independent determination is made in the Dedicated Core chain (Rother et al., 2013). The resulting Euler angles are provided as Level-2 data product MSW_EUL_2_ (MSW_EUL_2C and MSW_EUL_2F) and will be used in the re-processing of Level-1b data by the PDGS.
Spherical Harmonic Models of the lithospheric field are provided in the Level-2 product MLI_SHA_2_ (where “LI” stands for LIthospheric field). Similar to the core field products, model version MLI_SHA_2C is derived in the CI chain, while model MLI_SHA_2D is determined using the Revised Spherical Harmonic Cap method, as described in Thébault et al. (2013). The minimum, resp. maximum, spherical harmonic degree and order is Nmin = 16 and Nmax = 150.
A model of the non-polar daily geomagnetic variation caused by ionospheric currents, including their variability with season and solar flux, is given in the Level-2 product MIO_SHA_2_, where “IO” stands for IOnospheric field. Details of the dedicated chain leading to product version MIO_SHA_2D are given in Chulliat et al. (2013). Product version MIO_SHA_2C is derived in the CI chain.
Finally, time-series of spherical harmonic expansion coefficients of the large-scale magnetospheric field and its Earth-induced counterpart are provided in the Level-2 product of generic name MMA_SHA_2_. As part of the CI chain time series of the magnetospheric and induced expansion coefficients are provided with a sampling rate of 90 minutes (corresponding approximately to the orbital period of the satellites) for degree n = 1 and order m = 0, and with a sampling rate of 6 hours for degrees up to n = 3 and order m = 0, 1 for the magnetospheric field and up to n =m = 5 for the induced field. The name of the resulting product is MMA_SHA_2C. The dedicated chain (Hamilton, 2013) for deriving a related product called MMA_SHA_2F contains time series of magnetospheric and induced fields for degree n = 1 and order m = 0, 1 with sampling rate of 90 minutes. (The last character “F” in the product name indicates that this is a fast-track product which is provided without an independent regular validation as is the case for most other Level-2 products).
Level-2 data product MMA_SHA_2C of the large-scale magnetospheric field and its Earth-induced counterpart is used to determine models of electrical conductivity of the mantle, regarding both its 1-D structure (which means that conductivity is assumed to only vary with depth, resulting in Level-2 product MIN_1DM_2_, see Püthe and Kuvshinov (2013a) for details) and lateral variations of conductivity (3-D models, Level-2 product MIN_3DM_2_). The latter is derived using two independent chains, working in the frequency domain, leading to product version MIN_3DM_2a (Püthe and Kuvshinov, 2013b), or in the time domain, leading to product version MIN_3DM_2b (Velímsky, 2013). Electromagnetic transfer functions (C-responses) are also provided (Level-2 products MCR_1DM_2_ and MCR_3DM_2_).
3.2 Level-2 products related to acceleration, orbit determination and thermospheric wind and density
3.3 Level-2 products related to the Earth environment and space weather (Cat-2 products)
Figure 5 shows the processing chains that result in the Cat-2 Level-2 products (listed in the bottom part of Table 3). All Cat-2 products are provided as daily CDF files (similar to most of the Level-1b products) since they all contain time-series of a certain geophysical quantity.
Time series of an Ionospheric Bubble Index (IBI), derived using magnetic and plasma observations from each of the three satellites, are provided in IBIxTMS_2F. Details of the processing can be found in Park et al. (2013). Time series of the ionospheric and plasmaspheric Total Electron Content (TEC) as determined by each of the three satellites are provided in the product TECxTMS_2F. The implemented algorithm for TEC determination is identical to that described by Noja et al. (2013). The processing schemes resulting in time series of Field-Aligned Currents (FAC) as provided in FACxTMS_2F (single satellite solution), resp. FAC_TMS_2F (obtained by combining data from Swarm A and B) are described in Ritter et al. (2013).
Dayside Eastward Equatorial Electric Field (EEF) values are derived for each equatorial crossing of each satellite (x = A, B, or C) and are provided in the product EEFxTMS_2F. More details on that chain are given in Alken et al. (2013).
4. Development and Test of the SwarmSCARF
Difference in spectra, degree error, and accumulated error. The Mauersberger-Lowes spectrum (degree variance)of the differences between the true (i.e. input) and the estimated model coefficients, , in combination with the spectrum of the input model, has been used to evaluate an estimated model. Degree error is defined as , and accumulated error at degree N is defined as .(5)
Degree correlation(Langel and Hinze, 1998, eq. (4.23)), where and hm e are from the estimated model and and are from the input model, has also been used to evaluate a spherical harmonic model. Models are considered compatible up to that degree n where ρ n drops below 0.7.(6)
Sensitivity matrix is the relative error of each coefficient in a degree versus order matrix:S(n,m) represents the percentage degree-normalized error in a recovered coefficient of degree n and order m.(7)
Global maps of field differences (for instance of B r ) between the input and the estimated model are used to find geographically confined deficiencies in the estimated models, for instance in connection with the polar gaps.
Finally, the quality of time series (like those of the magnetospheric and induced spherical harmonic expansion coefficient) is assessed for various target periods using Squared Coherency coh2: If F (ω) and G (ω) are the Fourier transform of the two time series f (t) and g(t) and F (ω)* is the complex conjugate of F(ω) then squared coherency at frequency ω is defined aswith ⟨F(ω)G (ω)*⟩ and ⟨G(ω)F (ω)*⟩ as the cross-spectra and ⟨F(ω)F(ω)*⟩ and ⟨G(ω)G(ω)*⟩ as the auto-spectra of f(t),g(t) (e.g. eq. (20) of Olsen, 1998).(8)
Product requirements for magnetic Level-2 products.
Core field (MCO), first time derivative (secular variation) at ground, n = 2-16, averaged over time
Lithospheric field (MLI), accumulated error at ground, n = 16–150
Ionospheric field (MIO), average relative error on ground
10% at magnetic latitudes below ±55°
Magnetospheric field (MMA)
Squared coherency coh2 > 0.8, though > 0.95 for n = 1
Squared coherency coh2 > 0.8, though > 0.75 for n = 1
Mantle conductivity (MIN)
1/2 order of magnitude error, though 1/4 order of magnitude at depths 400–1500 km
1 order of magnitude error, though 1/2 order of magnitude at depths 400–1500 km
At the beginning of the SCARF activity the launch of the Swarm satellites was still scheduled for 2010. In order to have similar ambient conditions, but access to actual input values to parametrize e.g. atmospheric drag or Earth rotation variations, we simulated a launch on July 1, 1998, 00:00 UT, which is approximately one solar cycle (11 years) before the anticipated launch in 2010.
The performed simulation is described in more detail in Olsen et al. (2007), which is an extension of the work of Olsen et al. (2006). In a first step we calculated synthetic orbits. We assumed all three satellites to be in circular near-polar orbits with injection altitude of h0 = 450 km altitude and orbital inclination i = 87.4° for the lower pair (Swarm satellites A and B) and of h0 = 530 km altitude and orbital inclination i = 88° for the third satellite Swarm C. The two lower satellites were assumed separated in longitude by 1.4°. They are not exactly side-by-side (which would imply collision risk near the poles) but are shifted along-track by a time lag between 2 and 10 seconds. This simulates the requirement that “The maximum time difference between Swarm A and Swarm B when crossing the equator shall be 10 seconds”. The chosen orbital configuration is similar (though not identical) to the one that is presently foreseen for Swarm (h0 = 460 km and i = 87.35° for Swarm A and B; h0 = 530 km and i = 87.95° for Swarm C, and a Local Time of the Ascending Node of about 14:30).
Magnetic field data generation follows mainly the approach described in Olsen et al. (2006) with updates given in Olsen et al. (2007). The various input models have been designed in the following way: The core field is taken from the GRIMM model (Lesur et al., 2010) for the years 2003 to 2008, but shifted by 5 years (i.e. to 1998.0 to 2003.0) in order to be compatible with the simulation period. The lithospheric input model contains spherical harmonic expansion coefficients up to degree and order 250. Degrees n = 14 and 15 are taken from model POMME-6.1, degrees n = 16 to 90 are taken from model MF7, and degrees 91 to 250 are taken from model NGDC-720 (version 3p1) scaled by factor 1.1. See http://geomag.org/models/index.html for more information on these models. The magnetospheric field contribution is simulated using an hour-by-hour spherical harmonic analysis of world-wide distributed observatory hourly mean values of the years 1997-2002 in dipole-latitude and magnetic local time. Expansion coefficients of degrees n = 1,…, 3 and order m = 0,…, 1 have been determined. Secondary, Earth-induced fields are determined (up to n = 15) from those primary coefficients using the 3D mantle conductivity model, including oceans, discussed in Kuvshinov et al. (2006). The input model describing the ionospheric primary field is taken from CM4 (Sabaka et al., 2004) while the secondary, induced, field is calculated from those primary coefficients using the same 3D mantle conductivity model as for the magnetospheric induced field. Finally, we added synthetic noise based on CHAMP experience. We assumed correlated random noise of standard deviation (0.1 0.07, 0.07) nT for (Bn, BE, BC), in agreement with the Swarm performance requirements.
The magnetic field vector in the Level-1b CDF files is given both in the NEC coordinate frame and in the VFM frame of the vector magnetometer. In order to transform the synthetic data to the VFM frame we have arbitrarily chosen the (input) Euler angles (α = −1724, β = 3488,γ = −6184) arcsecs for Swarm A, (α = 808,β = −434,γ = −1234) arcsecs for Swarm B and (α = 2222,β = 2991,γ = 3115) arcsecs for Swarm C.
The various input (reference) models are available at ftp.space.dtu.dk/data/ magnetic- satellites / Swarm/ SCARF/TDS- 1/ Reference/ while the synthetic 1 Hz Level-1b data product MAGx_LR files can be found at ftp.space. dtu.dk/ data /magnetic-satellites/Swarm/ SCARF/TDS- 1/Level1b/Mag/. Further details of the results of the closed-loop modelling tests to check each chain meets the performance requirements can be found in the respective references and papers in this volume.
5. Swarm Processing Time-line and Data Availability
Three days (72 hours) after downlink
Swarm Level-1b data are processed
Next working day
Swarm Level-2 Quick-Look (MAGx_QL_2_ and EFIx_QL_2_), Fast-Track Magnetospheric (MMA_SHA_2F) and all Cat-2 data products (which require up to 2 hours of processing time) are processed
Up to three weeks later
Swarm Level-2 Products regarding Precise Orbit Determination (SP3xCOM_2_), Accelerometer data (ACCxCAL_2_, ACCxPOD_2_, ACCx_AE_2_), and Thermospheric (Neutral) Density and Winds (DNSxWND_2_), are processed
Every three months
Swarm Level-2 Fast-Track core field and Euler angles products (MCO_SHA_2F and MSW_EUL_2F) are processed
Every yearEvery year-plus a few extra times in reduced form during the first year of the mission—the Swarm Level-2 magnetic models are estimated and evaluated. The estimations are performed in two parallel processing chains:
The Comprehensive Inversion (MSW_EUL_2C, MCO_SHA_2C, MLI_SHA_2C, MMA_SHA_2C, MIO_SHA_2C) and Mantle Conductivity estimations (MIN_1DM, MIN_3DM, MCR_1DM, MCR_3DM) each with a processing time of one month
The Dedicated Inversions consisting of (in sequence, each step with a processing time of one month)
* Core field inversion (MCO_SHA_2D)
* Lithospheric field inversion (MLI_SHA_2D)
* Ionospheric field inversion (MIO_SHA_2D).
All estimated models are subject to an evaluation and- when parallel models are available—cross-comparisons which will be documented in the Swarm Level-2 Validation Products (Myy_VAL_2 _) with a processing time of up to one month.
Level-1b and Level-2 data are available at http://earth.esa.int/Swarm.
The Swarm mission is devoted to provide the best ever absolute measurements of the geomagnetic field. Its various instruments have been selected in order to optimize the scientific interpretation of the measurements in terms of the various sources of the magnetic field. In recognition of the large effort needed to extract the various types of scientific information from the complex set of observations a group of institutions and organisations have joined the SMART consortium (SwarmMagnetic andAtmosphericResearchTeam). The consortium has decided to contribute to the optimal science return from the mission by supporting the creation of a SwarmSCARF (SatelliteConstellationApplication andResearchFacility), with the purpose of deriving commonly used scientific models and parameters, the so-called Level-2 products and make them available to the scientific community at large.
During the 3-year long development phase of SCARF the various processing chains have been optimized and thoroughly tested, demonstrating that the facility is ready to enter the data exploitation phase and process real Swarm data. It is believed that some of the results of the SCARF exercise may also be of relevance for future Earth Science constellation missions that undoubtedly will be implemented.
List of Acronyms
Absolute Scalar Magnetometer (instrument)
Common Data Format (Goucher and Mathews, 1994)
Common Reference Frame (of Star Tracker)
Electric Field Instrument (LP and TII)
Global Position System (Receiver)
International Terrestrial Reference Frame
Langmuir Probe (instrument)
North, East, Center coordinate frame
Medium Precise Orbit Determination
Precise Orbit Determination
Payload Data Ground Segment
Receiver Independent Exchange Format (Gurtner and Estery, 2007)
National Geodetic Survey Standard GPS Format (Hilla, 2007)
Star Tracker (instrument)
Total Electron Content of ionosphere
Thermal Ion Imager (instrument)
Vector Field Magnetometer (instrument)
The Development of Swarm SCARF has been funded by ESA through contract No. 4000102140/10/NL/JA.
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