|
|
| Warnings and Alerts | |
|
Issue Time: 2026 Apr 02 0753 UTC
EXTENDED WARNING: Geomagnetic K-index of 5 expected Extension to Serial Number: 2218 Valid From: 2026 Apr 02 0230 UTC Now Valid Until: 2026 Apr 02 1800 UTC Warning Condition: Persistence Potential Impacts: Area of impact primarily poleward of 60 degrees Geomagnetic Latitude. Induced Currents - Weak power grid fluctuations can occur. Spacecraft - Minor impact on satellite operations possible. Aurora - Aurora may be visible at high latitudes, i.e., northern tier of the U.S. such as northern Michigan and Maine. Space Weather Scales |
|
| Current Condition and Alerts | |
|
Issued: 2026 Apr 02 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 01 April follow. Solar flux 142 and estimated planetary A-index 8. The estimated planetary K-index at 1200 UTC on 02 April was 5.00. Space weather for the past 24 hours has been minor. Geomagnetic storms reaching the G1 level occurred. Space weather for the next 24 hours is predicted to be moderate. Geomagnetic storms reaching the G2 level are expected. Radio blackouts reaching the R2 level are likely. Space Weather Scales |
|
| Forecast Discussion | |
|
Issued: 2026 Apr 02 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. C-class flaring was observed from Regions 4401 (N25W77, Hax/alpha), 4403 (N15W32, Hax/alpha), and 4409 (N02E19, Dri/beta-gamma). The largest flare was a C8.1 at 01/1958 UTC from Region 4409. Slight growth was observed in Region 4409. The rest of the spotted regions were stable or in decay. Other activity included several filament eruptions. The first was an approximate 30 degree filament eruption, centered near S23W57, that began at 01/1800 UTC. An associated CME was observed off the W limb in SOHO/LASCO C2 imagery at 01/1900 UTC. Modeling indicated no Earth-directed component. The second was an approximate 25 degree filament eruption in association with a C6.1 flare at 01/2328 UTC from Region 4403. The bulk of the ejecta appeared NNW is SUVI 304 imagery. An associated asymmetric halo CME was observed in GOES CCOR1 imagery at 01/2345 UTC. Initial model estimates show a glancing blow early on 04 Apr. Confidence is lower in the arrival time due to imagery gaps. .Forecast... Solar activity is likely to reach moderate (R1/R2-Minor/Moderate) levels, with slight chance for X-class (R3-Strong) flares through 04 Apr, due primarily to the flare potential of Regions 4404, 4405 and 4409. Energetic Particle .24 hr Summary... Electrons greater than 2 MeV at geosynchronous orbit reached high levels with a peak flux of 2,587 pfu at 01/1345 UTC before decreasing to normal to moderate levels at 01/1900 UTC. The greater than 10 MeV proton flux at geosynchronous orbit became slightly enhanced to around 1 pfu after 02/0130 UTC, possibly associated with a filament eruption in the NW quadrant around 01/2228 UTC. .Forecast... The greater than 2 MeV electron flux is expected to be at normal to moderate levels on 02 Apr and return to high levels 03 and 04 Apr due to HSS influence. There is a slight chance for the greater than 10 MeV proton flux to exceed S1 (Minor) solar radiation storm levels through 03 Apr increasing to a chance on 04 Apr due to possible CME enhancement. Solar Wind .24 hr Summary... Solar wind parameters began the period under CME influence from the 30 Mar CME. Following the IP shock arrival at 01/1130 UTC, weak enhancements in total field were observed ranging from 3-16 nT coupled with solar wind speeds initially reaching 500 km/s before calming to around 415 km/s. At 01/2005 UTC, a boundary crossing occurred exhibiting a shift into a negative sector. After 01/2300 UTC, total field began to increase reaching a maximum of 17 nT at 02/0729 UTC with Bz reaching a maximum southward deflection of -16 nT. Solar wind speed began to show an increase after 02/0300 UTC indicating the transition into a negative polarity CH HSS. .Forecast... Solar wind parameters are expected to continue to be enhanced under HSS conditions through 04 Apr. Additional enhancements from a glancing blow from the 01 Apr CME are expected late on 03 Apr to early on 04 Apr. Geospace .24 hr Summary... The geomagnetic field was at quiet to unsettled levels through 02/0000 UTC followed by active to G1 (Minor) storm conditions due to CME influence combined with the onset of CH HSS activity. .Forecast... The geomagnetic field is expected to be at unsettled to G1-G2 (Minor-Moderate) levels through the rest of the UTC day on 02 Apr due to combined CME/CH HSS activity. Unsettled to active levels are expected on 03 Apr as HSS activity persists. Glancing CME activity is expected early on 04 Apr causing unsettled to G1 (Minor) storming with a chance for G2 (Moderate) levels. Space Weather Scales |
|
| Three Day Forecast | |
|
Issued: 2026 Apr 02 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 Apr 02-Apr 04 2026 is 5.67 (NOAA Scale G2). NOAA Kp index breakdown Apr 02-Apr 04 2026 Apr 02 Apr 03 Apr 04 00-03UT 4.67 (G1) 4.33 5.33 (G1) 03-06UT 4.00 4.00 4.67 (G1) 06-09UT 5.33 (G1) 3.33 4.00 09-12UT 5.00 (G1) 3.33 3.67 12-15UT 5.67 (G2) 2.67 3.33 15-18UT 3.33 2.33 3.00 18-21UT 3.33 2.33 3.67 21-00UT 4.33 3.67 4.00 Rationale: The geomagnetic field is expected to be at unsettled to G1-G2 (Minor-Moderate) levels through the rest of the UTC day on 02 Apr due to combined CME/CH HSS activity. Glancing CME activity is expected early on 04 Apr causing unsettled to G1 (Minor) storming with a chance for G2 (Moderate) levels. 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 Apr 02-Apr 04 2026 Apr 02 Apr 03 Apr 04 S1 or greater 10% 10% 25% Rationale: There is a slight chance for the greater than 10 MeV proton flux to exceed S1 (Minor) solar radiation storm levels through 03 Apr increasing to a chance on 04 Apr due to possible CME enhancement. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for Apr 02-Apr 04 2026 Apr 02 Apr 03 Apr 04 R1-R2 55% 55% 55% R3 or greater 15% 15% 15% Rationale: Solar activity is likely to reach moderate (R1/R2-Minor/Moderate) levels, with slight chance for X-class (R3-Strong) flares through 04 Apr, due primarily to the flare potential of Regions 4404, 4405 and 4409. Space Weather Scales |
|
| Weekly Highlights and Forecasts | |
|
Issued: 2026 Mar 30 0230 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 23 - 29 March 2026 Solar activity reached moderate levels on 26 and 28 Mar with low levels observed on 23-25, 27, and 29 Mar. Region 4405 (N26, L=178, class/area=Ehi/330 on 28 Mar) was the most active of the period, producing nine C-class flares and a long-duration M1.3 flare at 28/0416 UTC that was accompanied by a Type II radio sweep (estimated velocity 868 km/s) and a CME first seen in LASCO C2 imagery at 28/0336 UTC. Region 4403 (N16, L=206, class/area=Hsx/120 on 28 Mar) was responsible for the most powerful event of the period, an M3.9/1n flare at 26/0623 UTC, which was associated with a Type II radio sweep (estimated velocity 607 km/s), a 1,600 sfu radio burst at 245 MHz, and a CME first visible in LASCO C2 imagery at 26/0648 UTC. Neither CME was determined to have 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 throughout the period 23-29 Mar with peak of 12,800 pfu observed at 27/1515 UTC. Geomagnetic field activity ranged from quiet to G1 (Minor) storm levels. G1 storm conditions were observed 23 Mar due to negative polarity coronal hole high speed stream (-CH HSS) influences. Active levels were observed on 24 Mar under the continuing -CH HSS. On 25 Mar, G1 storming levels were reached again; while residual -CH HSS effects were present, the activity was primarily driven by the arrival of a CME likely associated with a filament eruption on 22 Mar. Conditions waned to unsettled levels on 26 Mar and quiet levels on 27 Mar as HSS influences subsided. Activity remained quiet to unsettled on 28 Mar. On 29 Mar, the field returned to active levels preceding a solar sector boundary crossing (SSBC) and the onset of a positive polarity CH HSS (+CH HSS). Forecast of Solar and Geomagnetic Activity 30 March - 25 April 2026 Solar activity is expected to be is expected to be at low levels, with a varying chance for M-class (R1-R2/Minor-Moderate) flares through 25 Apr. No proton events are expected at geosynchronous orbit, barring any significant, non-recurrent solar activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 30-31 Mar, 04-09 Apr, 11-16 Apr, and 18-25 Apr. Normal to moderate flux levels are expected to prevail throughout the remainder of the period. Geomagnetic field activity is expected to reach G1 (Minor) geomagnetic storm levels on 30 March due to the influence of a positive polarity CH HSS (+CH HSS). Periods of G1 storming are likely on 04 April in response to a negative polarity CH HSS (-CH HSS). Further G1 storm periods are anticipated on 09 and 11 Apr, with likely G2 (Moderate) storm levels on 10 April, due to + CH HSS influences. The field is expected to reach G2 storm levels again on 18 Apr, followed by G1 storm periods on 19 Apr, due to -CH HSS influences. Unsettled to active conditions are likely during the onset and waning phases of these streams. Space Weather Scales |
|
| 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 | |
 |
|
| Daily Image AIA 171 PFSS Model | |
 |
|
| Daily Image AIA 193 | |
 |
|
| Daily Image AIA 304 | |
 |
|
| Daily Video AIA 171 | |
 |
|
| Daily Video AIA 171 PFSS Model | |
 |
|
| Daily Video AIA 193 | |
 |
|
| Daily Video AIA 304 | |
 |
|
| 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 | |
 |
|
| Daily Image HMI Magnetogram | |
 |
|
| Daily Video HMI Continuum | |
 |
|
| Daily Video HMI Magnetogram | |
 |
|
| 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 | |
| NO CURRENT DATA Insert LASCO | |
| Log Polar View C2 C3 and AIA 304 | |
| NO CURRENT DATA Insert Log Polar | |
| Combined C2 C3 and AIA 304 Video | |
| NO CURRENT DATA Insert LASCO Video | |
| Log Polar View C2 C3 and AIA 304 Video | |
| NO CURRENT DATA Insert Log Polar Video | |
| Space Weather Videos | |
|
|
|
| Space Weather Information | |
|
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. |
.jpg)