WMO OSCAR | Gap analyses by variable, type of mission or WIGOS subcomponent

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Gap analyses by variable, type of mission or WIGOS subcomponent

Select gap analysis type

Select analysis type

Expert system, based on instrument properties Help icon

Simplified, based on mission objectives Help icon

In "Simplified" mode, the results in the analysis are calculated by looking at each instrument's mission objectives: for each instrument we keep track of what the primary, secondary, and opportunity mission objectives are. These mission objectives indicate that an instrument is primarily envisioned to measure variable X, Y and Z, that variables A, B and C are its secondary objective, and that it may offer the opportunity to measure variables I and II although it is not optimized for that. The simplified Gap analysis produces a timeline based on this information. The simplified Gap analysis is only available for analyzing variables, not for missions.

In "Expert system" mode, the results in the analysis are calculated with an expert system. Internally, OSCAR works with a large set of 1700 rules that determine whether or not an instrument is capable of measuring a given variable, and to what degree. When you select "Expert system", the Gap analysis is performed based on this large set of rules.

Measurement timeline for Solar magnetic field Help icon

Hint: Move around in the timeline by scrolling up, down, left or right.

Found 14 results

This table has a large number of results.

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Instrument	Relevance	Satellite	Orbit	1980	1981	1982	1983	1984	1985	1986	1987	1988	1989	1995	1996	1997	1998	1999	2000	2001	2002	2003	2004	2005	2006	2007	2008	2009	2010	2011	2012	2013	2014	2015	2016	2017	2018	2019	2020	2021	2022	2023	2024	2025	2026	2027	2028	2029	2030	2031	2032	2033	2034	2035
MDI	1 - primary	SOHO												X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X
PHI	1 - primary	Solar Orbiter	25 °																																				X	X	X	X	X	X	X	X	X	X	X
PMI	1 - primary	Vigil-L5																																										X	X	X	X	X	X	X	X	X	X	X
SOT	1 - primary	Solar-B (Hinode)	06:00 asc																						X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X
HMI	2 - very high	SDO	29.6 °																										X	X	X	X	X	X	X	X	X	X	X	X	X
VELC	4 - fair	Aditya-1																																							X	X	X	X	X	X
CP	4 - fair	SMM	28.5 °	X	X	X	X	X	X	X	X	X	X
METIS	4 - fair	Solar Orbiter	25 °																																				X	X	X	X	X	X	X	X	X	X	X
SECCHI/COR-1	4 - fair	STEREO-B	23.44 °																						X	X	X	X	X	X	X	X	X
SECCHI/COR-1	4 - fair	STEREO-A	23.44 °																						X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X
SECCHI/COR-2	4 - fair	STEREO-B	23.44 °																						X	X	X	X	X	X	X	X	X
SECCHI/COR-2	4 - fair	STEREO-A	23.44 °																						X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X	X
FIELDS	5 - marginal	Parker Solar Probe	3.4 °																																		X	X	X	X	X	X	X	X
MAG (Solar Orbiter)	5 - marginal	Solar Orbiter	25 °																																				X	X	X	X	X	X	X	X	X	X	X

All instruments for measuring Solar magnetic field

Instruments	Relevance	Operational limitations
MDI	1 - primary
PHI	1 - primary
PMI	1 - primary
SOT	1 - primary
HMI	2 - very high
VELC	4 - fair
CP	4 - fair
METIS	4 - fair
SECCHI/COR-1	4 - fair
SECCHI/COR-2	4 - fair
FIELDS	5 - marginal
MAG (Solar Orbiter)	5 - marginal

Instrument Types Select
ECT Range Select
Orbit Types Select Select	Inclination Range Edit
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	Each instrument is assigned with an up-to-5-step rating, evaluated as a blend of several elements. For this particular Variable, the rating is driven by: the observed solar area (disk only or disk + corona or corona only); the spatial resolution; whether measuring flux or spectrum. RATING CRITERIA:
1	VIS spectrometer with polarisation and Doppler capability
2	Disk + corona, VIS fluxmeter with polarisation and possibly Doppler capability, high spatial resolution Disk only, VIS fluxmeter with polarisation and possibly Doppler capability, high spatial resolution
3	Disk + corona, VIS fluxmeter with polarisation and possibly Doppler capability, coarse spatial resolution Disk only, VIS fluxmeter with polarisation and possibly Doppler capability, coarse spatial resolution
4	Occultation coronagraph with polarisation capability
5	Close-to-Sun viewing, measurement by magnetic and electric fields oscillation Close-to-Sun viewing, measurement by vector magnetometer

OSCAR

Gap analyses by variable, type of mission or WIGOS subcomponent

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