|
|
| Warnings and Alerts | |
|
Issue Time: 2026 Jun 06 2211 UTC
WATCH: Geomagnetic Storm Category G3 Predicted Highest Storm Level Predicted by Day: Jun 07: None (Below G1) Jun 08: G3 (Strong) Jun 09: G2 (Moderate) THIS SUPERSEDES ANY/ALL PRIOR WATCHES IN EFFECT Space Weather Scales |
|
| Current Condition and Alerts | |
|
Issued: 2026 Jun 07 1850 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 06 June follow. Solar flux 138 and estimated planetary A-index 17. The estimated planetary K-index at 1800 UTC on 07 June was 2.00. No space weather storms were observed for the past 24 hours. Space weather for the next 24 hours is predicted to be strong. Geomagnetic storms reaching the G3 level are likely. Radio blackouts reaching the R1 level are likely. Space Weather Scales |
|
| Forecast Discussion | |
|
Issued: 2026 Jun 07 1250 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity reached moderate levels due to an M1.8/2n flare at 06/1401 UTC from Region 4461 (S21E12, Cro/beta), which was the largest of the period. Region 4456 (N17W41, Dai/beta-gamma-delta) was responsible for a C8.8/Sf flare at 06/1318 UTC as it continued to undergo evolution, gaining additional spots with asymmetric penumbra and a relatively weak delta signature in its intermediate area. Low-level C-class flares were observed just behind the E limb at about at about N06. The aforementioned M1.9/2N flare resulted in a F10.7 cm radio burst measuring 190 sfu, an approximately 11 degree-long filament eruption centered near S25E28, and a Type II sweep with an estimated speed of 838 km/s. The resulting partial halo CME, first seen in LASCO C2 coronagraph imagery at 06/1401 UTC, is anticipated to arrive around midday on 08 June. .Forecast... A chance for isolated M-class flare activity (55%) will persist through 09 June primarily due to the flare potential exhibited by Regions 4456, 4458 and 4462 alongside the flare history of Region 4455. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux at geosynchronous orbit reached high levels with a peak flux of 1,280 pfu at 06/1710 UTC. The greater than 10 MeV proton flux became enhanced just after 06/1515 UTC due to the eruption from the M1.8 flare event. .Forecast... The greater than 2 MeV electron flux at geosynchronous orbit is expected to remain at high levels through 07 June before returning to normal to moderate levels on 08 June with the arrival of the 06 June CME. 2 MeV electron flux levels are likely to return to high levels by the close of 09 June. The greater than 10 MeV proton flux is expected to remain at background levels with a chance for an S1 (Minor) event on 08 June with the shock arrival of the 06 June CME. Solar Wind .24 hr Summary... Solar wind parameters reflected waning CME and possible weak positive polarity CH HSS influences. Total field ranged 3-5 nT and the Bz component was mostly benign with no significant southward deflections. Solar wind speeds gradually declined to primarily below 550 km/s and phi was predominantly positive. .Forecast... Current solar wind conditions are expected to continue to wane over the course of 07 June. A disturbed solar wind environment is expected to return by early to mid UTC-day on 08 June with the shock arrival from the 06 June CME bringing enhanced magnetic field and faster solar wind. These enhancements are anticipated to continue into 09 June with a waning trend beginning by mid UTC-day. Geospace .24 hr Summary... Geomagnetic field activity was at quiet to unsettled levels. .Forecast... Quiet to unsettled levels are expected on 07 June under the current solar wind regime. G1-G2 (Minor-Moderate), with isolated periods of G3 (Strong), geomagnetic storming are likely to begin by mid UTC-day on 08 June with the arrival of the CME that left the Sun on 06 June. G1-G2 (Minor-Moderate) geomagnetic storming is likely to linger into the early portions of 09 June before giving way to unsettled to active conditions. Space Weather Scales |
|
| Three Day Forecast | |
|
Issued: 2026 Jun 07 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 Jun 07-Jun 09 2026 is 7.00 (NOAA Scale G3). NOAA Kp index breakdown Jun 07-Jun 09 2026 Jun 07 Jun 08 Jun 09 00-03UT 2.67 2.33 6.33 (G2) 03-06UT 2.00 2.00 5.33 (G1) 06-09UT 2.00 3.00 5.00 (G1) 09-12UT 2.67 4.33 4.33 12-15UT 2.00 5.33 (G1) 3.00 15-18UT 2.00 5.67 (G2) 3.33 18-21UT 2.33 7.00 (G3) 3.33 21-00UT 2.33 6.33 (G2) 3.67 Rationale: Periods of G1-G3 (Minor-Strong) geomagnetic storming are likely on 08 Jun, with G1-G2 (Minor-Moderate) storm periods likely on 09 Jun, following the anticipated arrival of a CME that left the Sun on 06 Jun. 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 Jun 07-Jun 09 2026 Jun 07 Jun 08 Jun 09 S1 or greater 15% 25% 10% Rationale: There is a slight chance for S1 (Minor) solar radiation storms on 07 and 09 Jun, with a chance for S1 levels on 08 Jun following the anticipated shock arrival of the 06 June CME. C. NOAA Radio Blackout Activity and Forecast Radio blackouts reaching the R1 levels were observed over the past 24 hours. The largest was at Jun 06 2026 1401 UTC. Radio Blackout Forecast for Jun 07-Jun 09 2026 Jun 07 Jun 08 Jun 09 R1-R2 55% 55% 55% R3 or greater 10% 10% 10% Rationale: R1-R2 (Minor-Moderate) radio blackouts are likely, with a slight chance for R3 (Strong) or greater events, over 07-09 Jun. Space Weather Scales |
|
| Weekly Highlights and Forecasts | |
|
Issued: 2026 Jun 01 0157 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 25 - 31 May 2026 Solar activity reached moderate levels on 29 May when Region 4455 (N15, L=83, class/area=Eko/370 on 29 May) produced an M1.1/Sf flare at 29/0704 UTC; the largest flare of the period. Solar activiy was low with C-flare activity observed throughout the remainder of the week. The greater than 10 MeV proton flux became enhanced late on 25 May following an eruption from beyond the NW limb. The greater than 10 MeV proton flux exceeded S1 (Minor) levels at 26/0010 UTC, and reached a peak flux of 2,380 pfu at 26/0110 UTC before decreasing below S1 levels by 26/0540 UTC. The greater than 100 MeV proton flux also became enhanced following this event, but did not exceed alert threshold. The greater than 2 MeV electron flux at geosynchronous orbit was at normal to moderate levels throughout the period. Geomagnetic field activity reached unsettled levels on 25 and 27 May, with active levels observed on 26, and 28-31 May, as negative polarity CH HSS influences prevailed throughout the period. Forecast of Solar and Geomagnetic Activity 01 June - 27 June 2026 Solar activity is expected to be at predominately low levels throughout the outlook period, with a chance for M-class (R1-R2/Minor-Moderate) flare activity. No proton events are expected at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 12-20 Jun, with normal to moderate levels likely throughout the remainder of the period. Geomagnetic field activity is likely to reach G2 (Moderate) storm levels on 11 Jun, with G1 (Minor) storming likely on 12 Jun, due to negative polarity CH HSS influences. Active conditions are likely on 01, 03-05, 13-14, and 23-27 Jun due to multiple recurrent CH HSSs. Quiet and quiet to unsettled conditions are expected to prevail throughout the remainder of the outlook period. 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 | |
 |
|
| Log Polar View C2 C3 and AIA 304 | |
 |
|
| Combined C2 C3 and AIA 304 Video | |
 |
|
| Log Polar View C2 C3 and AIA 304 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)