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| Warnings and Alerts | |
| No Current Warnings Space Weather Scales | |
| Current Condition and Alerts | |
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Issued: 2026 May 03 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 02 May follow. Solar flux 159 and estimated planetary A-index 7. The estimated planetary K-index at 1200 UTC on 03 May was 1.00. No space weather storms were observed for the past 24 hours. No space weather storms are predicted for the next 24 hours. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 May 03 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity was at low levels. An impulsive C8.7 flare at 02/1838 UTC from Region 4420 (N16, L=229), now beyond the northwest limb, was the largest of the period. Minor growth was observed in Regions 4428 (S24W44, Dai/beta-gamma), 4429 (S04E01, Dai/beta), and 4431 (S16E31, Dso/beta) and Region 4433 (S16E65, Dso/beta) was numbered as it rotated into view on the eastern limb. USAF SOON observatories reported a 20 degree long disappearing filament eruption beginning at approximately 02/1658 UTC that was centered near S31E08. This was corroborated by GOES SUVI 304 imagery, however, no discernible CME was observed in either CCOR-1, LASCO or STEREO-A coronagraph imagery indicating this event was likely mostly reabsorbed. .Forecast... Solar activity is expected to be at low levels with a chance for M-flares (R1-R2/Minor-Moderate) on 03-05 May. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux was at normal to moderate levels. The greater than 10 MeV proton flux was at background levels. .Forecast... The greater than 2 MeV electron flux is expected to be at normal to moderate levels on 03-05 May. The greater than 10 MeV proton flux is expected to remain at background levels through 05 May. Solar Wind .24 hr Summary... Solar wind parameters, as measured by the ACE spacecraft, remained consistent with ongoing negative polarity CH HSS influences. Total field strength reached a peak of 6 nT, and the Bz component briefly reached -6 nT. Solar wind speeds ranged between ~400-450 km/s throughout the period. .Forecast... The solar wind environment is expected to remain enhanced under negative polarity CH HSS influences over 03-05 May. Geospace .24 hr Summary... The geomagnetic field was at quiet to unsettled levels in response to negative polarity CH HSS influences. .Forecast... The geomagnetic field is expected to remain at quiet to unsettled levels 03-05 May as negative polarity CH HSS influences slowly wane. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 May 03 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
A. NOAA Geomagnetic Activity Observation and Forecast The greatest observed 3 hr Kp over the past 24 hours was 3 (below NOAA Scale levels). The greatest expected 3 hr Kp for May 03-May 05 2026 is 3.33 (below NOAA Scale levels). NOAA Kp index breakdown May 03-May 05 2026 May 03 May 04 May 05 00-03UT 3.33 2.67 2.67 03-06UT 2.33 3.00 2.67 06-09UT 2.67 2.67 2.00 09-12UT 2.67 2.67 2.00 12-15UT 2.33 1.67 1.67 15-18UT 1.67 1.67 1.67 18-21UT 1.67 0.67 1.67 21-00UT 2.67 2.67 2.00 Rationale: No G1 (Minor) or greater geomagnetic storms are expected. No significant transient or recurrent solar wind features are forecast. B. NOAA Solar Radiation Activity Observation and Forecast Solar radiation, as observed by NOAA GOES-18 over the past 24 hours, was below S-scale storm level thresholds. Solar Radiation Storm Forecast for May 03-May 05 2026 May 03 May 04 May 05 S1 or greater 5% 5% 5% Rationale: No S1 (Minor) or greater solar radiation storms are expected. No significant active region activity favorable for radiation storm production is forecast. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for May 03-May 05 2026 May 03 May 04 May 05 R1-R2 45% 45% 45% R3 or greater 5% 5% 5% Rationale: A chance for isolated R1-R2 (Minor-Moderate) radio blackouts due to M-class flares will persist through 05 May. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Apr 27 0538 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 20 - 26 April 2026 Solar activity ranged from low to high levels. The strongest events of the period were an X2.4 flare (R3-Strong) at 24/0107 UTC and an X2.5/2B (R3) at 24/0813 UTC from Region 4419 (N14, L=314, class/area=Eki/360 on 17 Apr). The X2.4 flare had as associated Tenflare and CME signature. Modeling of the CME indicated possible influence from the far periphery of the event on 26 Apr. The X2.5 flare had an associated Type II (est 1,293 km/s), Type IV, and Tenflare (570sfu) as well as a CME signature in coronagraph imagery. Modeling of this event suggested the primary bulk of the plasma was not on the Sun-Earth line. Other major X-ray events included an M6.4/1F (R2-Moderate) at 24/1815 UTC from Region 4419. The resulting CME was off the Sun-Earth line. An M6.0 (R2) flare 26/2257 UTC from Region 4420 (N16, L=225, class/area=Fki/400 on 25 Apr). As associated Type II (est 834 km/s) was reported with this event as well as a 30,000sfu burst on 245MHz. No CME signature was identified in subsequent coronagraph imagery. 13 other M-class (R1-Minor) events were observed over the past week with many producing radio and CME signatures. However, those events that were associated with CMEs did not contain an Earth-directed component. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 20-24 Apr and remained at normal background to moderate levels for the remainder of the report reporting period. Geomagnetic field activity reached G1 (Minor) storm levels on 20-21 Apr due to influence from a negative polarity CH HSS. Solar wind speeds peaked around 550 km/s and total magnetic field strength increased to a brief peak of 10 nT on 20 Apr. The Bz component reached as far south as -8 nT during the HSS. Quiet to unsettled conditions were observed over 22-25 Apr. A negative polarity coronal hole, with possible weak embedded influence from a CME that left the Sun on 24 Apr, caused isolated active levels on 26 Apr. Solar wind speeds remained below 500 km/s with this coronal hole. Forecast of Solar and Geomagnetic Activity 27 April - 23 May 2026 Solar activity is expected to reach moderate levels (R1-R2/Minor-Moderate), with a slight chance for high (R3/Strong), from 27 Apr - 04 May due to the flare potential from multiple active regions on the solar disk. The remainder of the outlook period is likely to be at low levels, with a slight chance for M-class (R1-R2). No proton events are expected at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit is expected reach high levels on 12 Apr, 29 Apr - 05 May, 08-14 May, and 17-21 May due to the anticipated influence from multiple, recurrent, CH HSS. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity is expected to reach G1 (Minor) geomagnetic storm levels on 07 May and 15-16 May. Active conditions are likely on 27 Apr, 30 Apr, 08 May, 17-18 May, and 23 May. Unsettled conditions are likely on 29 Apr, 01 May, 03-04 May, 09 May, and 21-22 May. All enhancement in geomagnetic activity are due to the anticipated influence of multiple, recurrent, CH HSSs. The remainder of the outlook period is expected to be at mostly quiet levels. Space Weather Scales |
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| About AIA Images | |
| The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) is designed to provide an unprecedented view of the solar corona, taking images that span at least 1.3 solar diameters in multiple wavelengths nearly simultaneously, at a resolution of ~ 1 arcsec and at a cadence of 10 s or better. The primary goal of the AIA Science Investigation is to use these data, together with data from other SDO instruments and from other observatories, to significantly improve our understanding of the physics behind the activity displayed by the Sun's atmosphere, which drives space weather in the heliosphere and in planetary environments. The AIA will produce data required for quantitative studies of the evolving coronal magnetic field, and the plasma that it holds, both in quiescent phases and during flares and eruptions; the AIA science investigation aims to utilize these data in a comprehensive research program to provide new understanding of the observed processes Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Daily Image AIA 171 | |
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| Daily Image AIA 171 PFSS Model | |
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| Daily Image AIA 193 | |
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| Daily Image AIA 304 | |
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| Daily Video AIA 171 | |
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| Daily Video AIA 171 PFSS Model | |
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| Daily Video AIA 193 | |
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| Daily Video AIA 304 | |
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| About the HMI Images | |
| (Helioseismic and Magnetic Imager) HMI is an instrument designed to study oscillations and the magnetic field at the solar surface, or photosphere. HMI is one of three instruments on the Solar Dynamics Observatory; together, the suite of instruments observes the Sun nearly continuously and takes a terabyte of data a day. HMI observes the full solar disk at 6173 Å with a resolution of 1 arcsecond. HMI is a successor to the Michelson Doppler Imager on the Solar and Heliospheric Observatory. This is very much how the Sun looks like in the visible range of the spectrum (for example, looking at it using special 'eclipse' glasses: Remember, do not ever look directly at the Sun!). The magnetogram image shows the magnetic field in the solar photosphere, with black and white indicating opposite polarities. Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Daily Image HMI Continuum | |
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| Daily Image HMI Magnetogram | |
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| Daily Video HMI Continuum | |
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| Daily Video HMI Magnetogram | |
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| About LASCO Images | |
| LASCO (Large Angle Spectrometric Coronagraph) is able to take images of the solar corona by blocking the light coming directly from the Sun with an occulter disk, creating an artificial eclipse within the instrument itself. The position of the solar disk is indicated in the images by the white circle. The most prominent feature of the corona are usually the coronal streamers, those nearly radial bands that can be seen both in C2 and C3. Occasionally, a coronal mass ejection can be seen being expelled away from the Sun and crossing the fields of view of both coronagraphs. The shadow crossing from the lower left corner to the center of the image is the support for the occulter disk. C2 images show the inner solar corona up to 8.4 million kilometers (5.25 million miles) away from the Sun. C3 images have a larger field of view: They encompass 32 diameters of the Sun. To put this in perspective, the diameter of the images is 45 million kilometers (about 30 million miles) at the distance of the Sun, or half of the diameter of the orbit of Mercury. Many bright stars can be seen behind the Sun. Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Combined C2 C3 and AIA 304 | |
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| Log Polar View C2 C3 and AIA 304 | |
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| Combined C2 C3 and AIA 304 Video | |
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| Log Polar View C2 C3 and AIA 304 Video | |
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| Space Weather Videos | |
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| Space Weather Information | |
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Demystifying Space Weather An article by Scientific Frontline Informative information and glossary about “Space Weather” Space weather has become increasingly important in our modern world due to our growing reliance on technology. It can impact various aspects of our daily lives, from communication and navigation systems to power grids and even astronaut safety. In this deep dive, we'll explore the intricacies of space weather, its causes, its effects, and why understanding it is crucial in our technology-dependent society. |
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