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| Warnings and Alerts | |
| No Current Warnings Space Weather Scales | |
| Current Condition and Alerts | |
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Issued: 2026 May 01 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 30 April follow. Solar flux 143 and estimated planetary A-index 15. The estimated planetary K-index at 1200 UTC on 01 May was 1.67. Space weather for the past 24 hours has been minor. Geomagnetic storms reaching the G1 level occurred. 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 01 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 with isolated to occasional C-class flaring observed primarily from Region 4420 (N16W76, Fkc/beta-gamma-delta), though Region 4424 (N17W42, Eai/beta-gamma) produced the largest flare of the period, a C5.1 at 30/0031 UTC. There are six numbered regions on the visible disk. Region 4420 continued to show a slight decline in extent along with fragmentation and spreading of the intermediate spots and an overall decrease in spot count despite some new flux emergence. Region 4424 underwent growth with in the intermediate spots and consolidation in the leading group, developing a mixed polarity gamma configuration. Region 4425 (N05W03, Ekc/beta) showed loss of penumbra in the trailing spots with increased separation and consolidation of the bipoles. Region 4423 (S10W60, Bxo/beta) showed consolidation of its trailing pole with slight spreading between the bipoles. Region 4428 (S24W20, Cro/beta) showed flux emergence in the intermediate area along with consolidation of, and separation between, the leading and trailing regions. New Region 4429 (S04E28, Cro/beta) was numbered this period. Analysis is ongoing following the observation of CME to the southeast first seen in STEREO-A COR2 imagery beginning at 30/1253 UTC and to the south-southwest in SOHO LASCO C2 imagery beginning at 30/1326 UTC. .Forecast... Solar activity is expected to be at low levels with a chance for moderate (R1-R2, Minor-Moderate) flare activity over 01-03 May. A slight chance for X-class flares (R3-Strong or greater) also exists, due primarily to the flare potential of Regions 4420 and 4425. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux at geosynchronous orbit was at normal to moderate levels with a peak of 421 pfu observed at 30/1415 UTC. The greater than 10 MeV proton flux at geosynchronous orbit was at background levels. .Forecast... The greater than 2 MeV electron flux is expected to increase to high levels 01-02 May in response to anticipated negative polarity CH HSS (-CH HSS) influences before returning to low to moderate levels on 03 May. The greater than 10 MeV proton flux is expected to remain at background levels, though a slight chance for S1 (Minor) solar radiation storm levels or greater exists through 03 May due to the complexity and location of Region 4420. Solar Wind .24 hr Summary... Solar wind parameters were enhanced during the period. Solar wind speeds started the period ranging around 350 km/s, before increasing more significantly late in the period to approximately 500 km/s. Total magnetic field strength (Bt) increased from around 6-8 nT early in the period to a peak near 13-14 nT around 30/1500-1600 UTC before decreasing toward 10 nT late in the period. The North-South component (Bz) was variable with several sustained southward deflections later in the period, deviating as far south as -12 nT at around 30/1930 UTC. A rise in solar wind temperature late in the period, coinciding with the speed increase, is consistent with HSS arrival. The phi angle was predominantly in the negative (towards the Sun) orientation throughout the period. .Forecast... Enhanced solar wind conditions are expected to persist through 01 May under continued -CH HSS influences. A gradual return to near nominal levels is anticipated on 02 May as HSS influences wane, before a new negative polarity CH HSS is anticipated to become geoeffective by late 03 May. Geospace .24 hr Summary... The geomagnetic field ranged from quiet to G1 (Minor) geomagnetic storm levels. .Forecast... Unsettled to G1 (Minor) conditions are expected through 01 May under continued -CH HSS influences. A return to mostly quiet levels is anticipated on 02 May as HSS influences wane. Quiet to unsettled conditions are expected on 03 May with the anticipated onset of a new negative polarity CH HSS late in the day. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 May 01 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 5 (NOAA Scale G1). The greatest expected 3 hr Kp for May 01-May 03 2026 is 4.33 (below NOAA Scale levels). NOAA Kp index breakdown May 01-May 03 2026 May 01 May 02 May 03 00-03UT 4.00 2.33 2.33 03-06UT 4.33 2.33 1.67 06-09UT 3.00 2.33 1.33 09-12UT 2.67 2.33 2.33 12-15UT 3.67 2.00 2.67 15-18UT 2.00 2.00 3.00 18-21UT 2.00 2.00 3.33 21-00UT 1.67 2.00 3.33 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 01-May 03 2026 May 01 May 02 May 03 S1 or greater 10% 10% 10% Rationale: There exists a slight chance for S1 (Minor) or greater solar radiation storms over 01-03 May. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for May 01-May 03 2026 May 01 May 02 May 03 R1-R2 50% 50% 50% R3 or greater 10% 10% 10% Rationale: A chance exists for R1-R2 (Minor-Moderate) radio blackouts, with a slight chance for R3 (Strong), over 01-03 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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