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MAG

Created by Andrew Walsh, last modified on 14 Apr, 2016

Note that all data volumes & rates are based on powers of 10, i.e. 1Gbit = 10⁹ bits.

TM Figures

Allocated TM	1.3 kbits/s
Download capacity per orbit (168 Days)	2.359 GB	= 18.870Gbits
SSMM allocation

Power Consumption

Source: MAG EM User Manual Issue 1, rev 0

Unit	Nominal (worst case 5 minute average) Power (Watts)
Electronics box and fluxgate electronics	6.86
Primary (outboard) sensor	0.36
Secondary (inboard) sensor	0.36
Sensor Heaters	5 Note: Heaters will be on when instrument is switched off (survival heaters)

Operational Modes

Source: MAG User Manual Issue 2, Rev 0

Mode	Data Rate (bps)	Duty Cycle (%)	Duty Cycle (hrs / orbit)	Orbital Volume (Gbits)
MAG Normal Mode	1000	100%	4032	14.515
MAG Burst Mode	6892	4.35%	175.526	4.355

Engineering Modes

Mode	Data Rate (bps)
SAFE	46
CONFIG	46
STANDBY	46
DEBUG	13924

Currently Implemented in MAG MAPPS/EPS EDF (For MTP/STP)

Objectives for MAG

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1.1.1.1 Low FIP fast wind origins
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1.1.2.1 Does slow wind originate from the over-expanded edges of coronal holes?
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1.1.2.2 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes?
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1.1.2.4 Study of density fluctuations in the extended corona as a function of the outflow velocity of the solar wind while evolving in the heliosphere
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1.1.2.5 Structure and evolution of streamers
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1.1.2.6 Disentangle the spatial and temporal variability of the slow wind
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1.1.2.7 Trace streamer blobs and other structures through the outer corona and the heliosphere.
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1.1.2.8 Determine the velocity, acceleration profile and the mass of the transient slow wind flows
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1.1.3.2.1 How does the Sun's magnetic field change over time?
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1.1.3.2.2 How is the heliospheric current sheet (HCS) related to coronal structure?
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1.1.3.3 What is the distribution of the open magnetic flux?
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1.1.4.1.3 Identify reconnection exhausts in the solar wind
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1.1.4.1.5 Identify and characterise the solar wind reconnection physics in current sheets with thickness down to the ion scales and smaller
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1.2.1.2 Energy and mass flux in the corona.
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1.2.1.9 Multi-temperature diagnostics of flaring coronal loops
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1.2.2.1 Determine where energy is deposited in the solar wind
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1.2.2.2 What drives the evolution of the solar wind distribution functions in situ?
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1.2.2.3 What is the nature and origin of waves, turbulence and small-scale structures?
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1.2.2.4 Solar wind reconnection physics
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1.2.2.6 Study fast plasma flows from the edges of solar active regions discovered with Hinode/EIS
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1.2.2.7 Study the correlation degree between velocity and magnetic field fluctuations in the interplanetary space
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1.3.1 Solar and local origin of Alfvénic fluctuations
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1.3.2 How is turbulent energy dissipated and how does turbulence evolve within the heliosphere?
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1.3.3 Plasma turbulence variability
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1.3.4 Plasma turbulence anisotropy
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2.1.1.2 CME structure
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2.1.1.3 CME evolution
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2.2.1 How do CMEs contribute to the global evolution of magnetic flux in the heliosphere?
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2.2.2 What is the role of ICMEs in the Sun’s magnetic cycle?
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2.3.2.1 Understand coronal conditions under which the shocks form and determine the interplanetary conditions where they evolve
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2.3.2.2 Identify interplanetary shocks and characterise their spatial and temporal evolution
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2.3.2.3 Study heating and dissipation mechanisms at shocks with radial distance
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2.3.2.4 Identify mechanisms that heat the thermal solar wind particle populations near shocks and determine their energy partition
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2.3.3 Resolve the interplanetary shock field and plasma structure down to the spatial and temporal scales comparable and smaller than the typical ion scales.
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2.3.4 Shock-surfing acceleration mechanism
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2.3.5 Understand the radio emissions from the ICME driven shocks
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2.3.6 Identify shock accelerated particles
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3.1.1.1 Where and when are shocks most efficient in accelerating particles?
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3.1.1.2.2 Composition variations
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3.1.1.2.3 Warped shock fronts
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3.1.1.2.4 Turbulence and inhomogeneities
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3.1.1.3 How are superhalo particles accelerated continuously in the corona and solar wind?
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3.1.1.4 How can SEPs be accelerated to high energies so rapidly?
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3.1.1.5 Do proton-amplified Alfvén waves play a role in accelerating particles at shocks?
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3.1.1.6 What causes SEPs' spectral breaks?
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3.1.1.7 Are there favourable environments for particle acceleration?
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3.1.2.0.1 Measure the enhancements of trans-iron elements in impulsive SEPs (to be deleted - trans-iron SEPs cannot be detected by EPD)
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3.1.2.3 Flare seed particles
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3.1.2.4 Explore the fact that only some of the hard X-ray peaks are related to escaping electrons, while others are not
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3.1.2.5 X-ray prompt events
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3.1.2.6 Delayed events (between X-ray peak and electron release time)
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3.1.2.8 Explore the type III radio bursts delays
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3.1.3.1 How shocks can accelerate electrons to relativistic energies (never observed for shocks near 1 AU)?
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3.1.3.2 Double-power law spectra
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3.1.4.1 Hard X-ray emission of escaping electron beams (thin-target emission)
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3.1.4.2 X-ray emission from electrons accelerated at CME shocks
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3.2.1.1 Map the power spectrum of the turbulent magnetic field as a function of heliocentric distance in order to provide ground-truth for transport models
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3.2.1.2 Measurements of SEP events time profiles and anisotropy in order to probe solar wind turbulence
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3.2.2 Latitudinal and longitudinal transport of SEPs
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3.2.3 Properties and distribution of near-Sun shocks, their fluctuations and particle acceleration
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3.2.4 How do large and small-scale structures modulate particle fluxes?
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3.2.5 Shock-surfing acceleration mechanism
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3.3 What are the seed populations for energetic particles?
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4.2.1 Probability density function (PDF) of solar high-latitude magnetic field structures.
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4.2.2 Basic properties of solar high-latitude magnetic field structures
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5.10.1 What is the temporal variability of 3D thermal particle distributions?
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5.10.2 How are proton and helium temperatures related to their relative drift, is there any evidence for resonant heating?
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5.10.3 How common are proton beams, where do they come from and what impact do they have on ambient conditions (wave generation, heating)?
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5.10.4 Identify and characterise the various forms of free energy in the particle distribution functions
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5.10.6 Electron halo population
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5.10.7 How do the combined electron strahl and composition signatures vary across reconnecting solar wind current sheets?
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5.4.2.1 Understand cometary properties and evolution by mapping the hydrogen Ly-α emission, proportional to the outgassing rate, along its trajectory close to the Sun

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