Integral protonspfu = cm⁻² s⁻¹ sr⁻¹
Dashed lines: NOAA solar radiation storm levels S1–S5, defined on the ≥10 MeV channel. Drag across a plot to zoom all time axes; double-click to reset.
provided by ESA and NOAA
Data: NOAA SWPC, GOES primary satellite for protons (SGPS integral and differential proton fluxes, real-time products)
Dashed lines: NOAA solar radiation storm levels S1–S5, defined on the ≥10 MeV channel. Drag across a plot to zoom all time axes; double-click to reset.
Black line, right axis: magnetic local time of the GOES satellite, from the longitude SWPC lists for it and a tilted dipole (IGRF-2025).
Points at the geometric centre of each channel. Zero fluxes are left out.
Data: NOAA SWPC, GOES primary satellite for electrons (≥2 MeV integral and MPS-HI differential electron fluxes, real-time products)
Dashed line: NOAA alert threshold, 1000 pfu. Values at geostationary orbit swing with local time each day.
Black line, right axis: magnetic local time of the GOES satellite, from the longitude SWPC lists for it and a tilted dipole (IGRF-2025).
NOAA gives one nominal energy per channel; the spectrogram bands run between the geometric midpoints of these energies.
Data: ESA Space Weather Service Network (SWESNET), NGRM Level-1 fluxes of MTG-I1 and MTG-S1 (GEO), MetOp-SG-A1, Sentinel-6 MF and Sentinel-6B (LEO). Orbit view also: GOES (NOAA SWPC) and, in the local build only, GK2A/KSEM (KMA, via ESA SWESNET). To choose satellites and follow their orbits and measurements over the last 24 h, open the satellite tracker.
Earth-fixed view, lit by the Sun at build time; samples behind the Earth are left out. LEO tracks: last 6 h; GEO units: last 24 h; dot = latest sample. Diamonds: other GEO monitors at the energies selected for NGRM (latest value): GOES from NOAA (integral flux above the NGRM threshold, >0.15, >0.4 or >1 MeV, summed from the MPS-HI differential channels; protons: SGPS P3, 3.4–6.5 MeV) and, in the local build only, GK2A/KSEM from swesnet (no redistribution allowed; 0.1–3.8 MeV bins; protons 3.1–6 MeV, near its background). Units are not inter-calibrated. Drag to turn, scroll or pinch to zoom. The faint ring marks geostationary distance. White: magnetic field line through each spacecraft's latest position, from an eccentric dipole fitted to IGRF-2025 (no external field), with dots where it reaches 100 km; cut at 14 RE. Its L can differ by up to ~10 % from the UNILIB L in the labels.
5-min means of the 90-s fluxes; the buttons choose the GEO unit for each species. At geostationary orbit the flux follows magnetic local time each day; L from UNILIB.
Median flux per 2-h and 0.25-L bin, all longitudes, both hemispheres; bins with fewer than 3 samples are empty. The colour scale is shared by the three units, so switching compares them directly. Below L ≈ 2 the LEO electron channels respond mostly to protons in the South Atlantic Anomaly.
As in the MetOp-SG-A1/NGRM newsletter: median fluxes per 2° × 3° geographic bin (latitude × longitude) over the 7-day window (≥ 3 samples). Empty bins with at least 4 of their 8 neighbours valued are interpolated (inverse-distance mean of the neighbours in log flux, one pass; the readout marks them); other empty bins show the Earth. Each bin is assigned by its median UNILIB L: protons where L < 3 (inner belt, the SAA), electrons where L ≥ 3 (outer belt, the horns at 50–75° latitude), each above its display level. Low-energy proton channels also count outer-belt electrons, which this split keeps out of the SAA picture. Colour scales run from the display level to the 98th percentile. Display levels: 10 × the quiet level far from the SAA (|lat| < 30°, 60–140° E), at least 0.2 for protons and 50 for electrons. LEO altitudes: MetOp-SG-A1 830 km, Sentinel-6 MF and 6B 1336 km, where the SAA is larger.
B/B₀: field strength at the spacecraft over its minimum on the same field line (UNILIB, IGRF + Olson–Pfitzer quiet). B/B₀ = 1 is the magnetic equator; the LEO units sample high B/B₀, close to where field lines enter the atmosphere (dashed line: dipole estimate at 100 km). GEO units are not shown here (they sit at B/B₀ ≈ 1; see the GEO time series). Median per 0.1-L × 0.05-decade bin (≥ 3 samples). Grey bins: median flux 0 (no counts above background, e.g. protons outside the inner belt). Electron channels: proton-contaminated samples in the SAA are masked (Sentinel-6 MF and 6B quality flag), so those bins stay empty. Proton channels: differential flux; MetOp-SG-A1 4.5 and 47 MeV, Sentinel-6 MF and 6B 5 and 50 MeV. Units are not inter-calibrated.
Data: NOAA SWPC: GOES XRS X-rays and flare list, real-time solar wind at L1 (the active spacecraft), planetary Kp
Flare class from the 0.1–0.8 nm channel (letters at right). Dots mark flare peaks of class C and above; M and X peaks are labelled.
NOAA's real-time solar-wind files hold only the last 24 hours; this page keeps them for 7 days (saved every hour), so the 3- and 7-day windows show the full span. Only the source NOAA marks as active is shown.
3-hour Kp. G1–G5 storm levels at Kp 5–9.
Data: NOAA SWPC alerts, warnings and watches; latest values of the GOES channels above