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☀️ GOES X-Ray Flux Monitor

Real-time solar X-ray flux monitoring from NOAA GOES satellites in geostationary orbit

Data Source: GOES-16 (GOES-East, 75.2°W) & GOES-18 (GOES-West, 137.2°W) • Wavelengths: 0.5-4.0 Å & 1.0-8.0 Å • Update Frequency: Real-time, 1-minute averages
Current X-Ray Level
B2.4
Background Level
24-Hour Peak
C5.1
at 08:42 UTC
Solar Activity Status
● QUIET
No major events detected
🌍 Sunspot Number: 87 ☀️ Solar Wind Speed: 425 km/s 🧲 Kp Index: 2 (Quiet)

☀️ Solar Flare Classification

X-Class
Major flares
≥ 10⁻⁴ W/m²
Radio blackouts, radiation storms
M-Class
Medium flares
10⁻⁵ to 10⁻⁴ W/m²
Brief radio blackouts
C-Class
Small flares
10⁻⁶ to 10⁻⁵ W/m²
Minor effects
B-Class
Background
10⁻⁷ to 10⁻⁶ W/m²
No noticeable effects
A-Class
Quiet
< 10⁻⁷ W/m²
Normal background level

🛰️ GOES X-Ray Detection System

🛰️

GOES-16 (GOES-East)

Launched: November 19, 2016

Position: 75.2°W Geostationary Orbit

Altitude: 35,786 km (22,236 mi)

Instrument: EXIS (Extreme Ultraviolet and X-ray Irradiance Sensors)

Coverage: Eastern Americas, Atlantic Ocean

X-Ray Bands:

  • • XRS-A: 0.05-0.4 nm (soft X-rays)
  • • XRS-B: 0.1-0.8 nm (hard X-rays)
🛰️

GOES-18 (GOES-West)

Launched: March 1, 2022

Position: 137.2°W Geostationary Orbit

Altitude: 35,786 km (22,236 mi)

Instrument: EXIS (Extreme Ultraviolet and X-ray Irradiance Sensors)

Coverage: Western Americas, Pacific Ocean

X-Ray Bands:

  • • XRS-A: 0.05-0.4 nm (soft X-rays)
  • • XRS-B: 0.1-0.8 nm (hard X-rays)

How X-Rays Are Detected: The EXIS sensors measure solar X-ray irradiance in two wavelength bands. When a solar flare occurs, the sudden increase in X-ray flux is detected within seconds. Data is transmitted continuously to NOAA's Space Weather Prediction Center, where it's processed and classified (A, B, C, M, or X class) based on peak flux intensity in the 0.1-0.8 nm band.

📊 GOES X-Ray Flux - 6-Hour Real-Time (NOAA Data)

Loading X-ray flux data...
Data Source: NOAA SWPC • Update: Every minute • Red Line: 0.1-0.8 nm (classification band) • Blue Line: 0.05-0.4 nm

🧲 Solar Magnetic Field (HMI Continuum)

Solar Magnetic Field
Observatory: NASA Solar Dynamics Observatory (SDO) • Instrument: Helioseismic and Magnetic Imager (HMI) • Shows sunspot regions where X-rays originate

☀️ Solar Corona (94 Å EUV)

Solar X-Ray Image
Observatory: NASA SDO • Instrument: Atmospheric Imaging Assembly (AIA) • Wavelength: 94 Å (6.3 million K plasma) • Shows flaring regions and coronal structures

🔬 How Solar X-Rays Are Detected

1. X-Ray Generation at the Sun

Solar flares occur when magnetic energy in the Sun's atmosphere is suddenly released. This heats plasma to 10-40 million K, emitting intense X-rays that travel at light speed (8 minutes to Earth).

2. Satellite Detection

GOES satellites orbit at 35,786 km altitude, outside Earth's atmosphere which blocks X-rays. The EXIS instrument uses ionization chambers and photodiodes to measure X-ray intensity in real-time.

3. Data Transmission & Processing

X-ray flux data is transmitted every second to NOAA's Wallops Command and Data Acquisition Station in Virginia, then relayed to the Space Weather Prediction Center in Boulder, Colorado.

4. Classification & Alerts

Flares are classified by peak flux in the 0.1-0.8 nm band: A (10⁻⁸ W/m²), B (10⁻⁷), C (10⁻⁶), M (10⁻⁵), X (≥10⁻⁴). Automated alerts notify operators of power grids, airlines, and GPS systems.

🎯 Solar Flare Probability Forecast (Next 24 Hours)

M-Class Flare Probability
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Medium flares (R1-R2 radio blackouts)
X-Class Flare Probability
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Major flares (R3+ radio blackouts)
Proton Event (S1+) Probability
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Radiation storm forecast
Data Source: NOAA Space Weather Prediction Center • Method: Probabilities derived from current sunspot complexity, magnetic field configuration (McIntosh classification), and recent flare history • Updated every 6-12 hours by SWPC forecasters