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| Warnings and Alerts | |
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Issue Time: 2026 Jun 28 1041 UTC
WATCH: Geomagnetic Storm Category G1 Predicted Highest Storm Level Predicted by Day: Jun 28: None (Below G1) Jun 29: G1 (Minor) Jun 30: G1 (Minor) THIS SUPERSEDES ANY/ALL PRIOR WATCHES IN EFFECT 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 |
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| Current Condition and Alerts | |
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Issued: 2026 Jun 29 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 28 June follow. Solar flux 186 and estimated planetary A-index 5. The estimated planetary K-index at 1200 UTC on 29 June was 1.33. No space weather storms were observed for the past 24 hours. Space weather for the next 24 hours is predicted to be minor. Geomagnetic storms reaching the G1 level are likely. Radio blackouts reaching the R1 level are likely. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Jun 29 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. Despite showing decay and weakening throughout the period, Region 4475 (S07W43, Dai/beta-gamma) produced a C9.5 at 28/2117 UTC (the largest flare of the period), as well as a C3.0 flare at 29/0250 UTC. Region 4478 (S05E01, Fki/beta-gamma-delta) maintained its weak delta configuration as it observed minor decay and separation between its leading spots and trailing spots. this region only yielded a C4.1 flare at 29/0340 UTC. Region 4479 (N15W05, Eki/beta-gamma-delta) exhibited significant development, gaining a delta configuration and multiple intermediate spots, and was the primary contributor to the overall flare activity. The largest events from this region included: a C8.7 at 28/2159 UTC, a C6.5/Sf at 29/0758 UTC, and a C8.1/Sf at 29/0828 UTC. This region added multiple low and mid level C-class flares as well. The other regions on the visible disk continued to decay and were inactive. .Forecast... Solar activity is expected to continue at predominately low levels on 29-30 Jun and 01 Jul. Isolated M-flares (R1-R2/Minor-Moderate) are likely, with a slight chance for X-flares (R3/Strong or greater), primarily due to the potential of Regions 4475 and 4479. Energetic Particles .24 hr Summary... The greater than 2 MeV electron flux reached high levels, observing a maximum flux of 2,627 pfu at 28/1700 UTC. The greater than 10 MeV proton flux was at background levels. .Forecast... The greater than 2 MeV electron flux is expected to remain elevated to moderate to high levels over 29-30 Jun and 01 Jul. The greater than 10 MeV proton flux is expected to persist at background levels through 01 Jul. Solar Wind .24 hr Summary... Solar wind parameters returned to near background levels. Total magnetic field strength averaged around 4 nT, the Bz component experienced no significant southward deflections, and solar wind speeds decreased to settled under 400 km/s by the end of the period. Phi remained mostly in a negative (towards the Sun) orientation. .Forecast... The solar wind environment is expected to remain near background levels through most of 29 Jun. Enhanced conditions are anticipated to return by late 29 Jun to midday on 30 Jun with the predicted arrival of the CME that left the Sun late on 26 Jun. Additional enhancements are again likely on 01 Jul as the CME from 27 Jun is forecast to reach Earth. Geospace .24 hr Summary... The geomagnetic field was at quiet levels. .Forecast... Mostly quiet conditions are expected for most of 29 Jun. Unsettled to active levels are then expected, with isolated G1 (Minor) storm conditions likely, and a slight chance for G2 (Moderate) levels by early 30 Jun, due to the potential arrival of the 26 Jun CME. Quiet to unsettled levels, with isolated active periods, are expected on 01 Jul. There is also a chance for isolated periods of G1 (Minor) storming on 01 Jul with the anticipated arrival of the CME that left the Sun on 27 Jun, though confidence is low with this forecast. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Jun 29 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 1 (below NOAA Scale levels). The greatest expected 3 hr Kp for Jun 29-Jul 01 2026 is 5.00 (NOAA Scale G1). NOAA Kp index breakdown Jun 29-Jul 01 2026 Jun 29 Jun 30 Jul 01 00-03UT 1.00 4.67 (G1) 2.00 03-06UT 1.00 5.00 (G1) 1.67 06-09UT 0.33 4.00 1.67 09-12UT 1.33 4.00 1.67 12-15UT 1.33 3.67 2.00 15-18UT 1.33 3.33 2.33 18-21UT 1.67 3.00 3.67 21-00UT 4.67 (G1) 1.67 4.33 Rationale: Isolated G1 (Minor) storm conditions are likely, with a slight chance for G2 (Moderate) levels by early 30 Jun, due to the potential arrival of the 26 Jun CME. 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 29-Jul 01 2026 Jun 29 Jun 30 Jul 01 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 Jun 29-Jul 01 2026 Jun 29 Jun 30 Jul 01 R1-R2 55% 55% 55% R3 or greater 10% 10% 10% Rationale: Isolated R1-R2 (Minor-Moderate) radio blackouts are likely, with a slight chance for R3 (Strong or greater) events, primarily due to the potential of Regions 4475 and 4479. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Jun 22 0229 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 15 - 21 June 2026 Solar activity was at low levels on 15-19 Jun with a total of 19 C-class flares, moderate levels on 20-21 Jun with three M-class (M5 or below) flares, and high levels on 22 Jun with an isolated M6.8 flare. Three out of the four M-class flares originated from Region 4473 (S08, L=133, class/area=Eko/270 on 20 Jun). These included: an M1.0 at 20/1500 UTC, an M2.6 at 21/0246 UTC, and the M6.8/2b flare at 21/1929 UTC (the largest of the period). Region 4472 (S14, L=149, class/area=Dao/100 on 20 Jun) added the remaining M-flare, an M1.3 at 20/0151 UTC. Notable activity included a small filament eruption, a pair of type-II radio sweeps, and a couple of CMEs. The filament eruption was centered near S20E20 and began after 19/0300 UTC. A faint, slow-moving CME signature appeared in STEREO-A COR2 imagery but was not apparent in other available coronagraph imagery. Analysis and modeling of the event indicated most of the ejecta will likely miss behind Earth's orbit, with a slight possibility of a portion grazing Earth by mid to late on 23 Jun. Additional CMEs were observed early in the period, but none appeared to have an Earth-directed component. The aforementioned radio sweeps were relatively slow moving. The first was at 20/0407 UTC, with an estimated velocity of 300 km/s, likely associated with a C1.4 flare that occurred at 20/0307 UTC from Region 4470 (N06, L=188, class/area=Dao/90 on 19 Jun). The second was at 21/1932 UTC, with an estimated velocity of 380 km/s, likely associated with the M6.8/2b flare. A CME associated with the C1.4 flare was analyzed and determined to not have an Earth-directed component. A CME was also likely associated with the M6.8 flare, but analysis was pending as of this writing. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 15,16, and 18 Jun, with a peak flux of 2,043 pfu at 16/1525 UTC. Flux levels were at low to moderate levels on 17and 19-21 Jun. Geomagnetic field activity was at quiet to unsettled levels throughout the period (15-21 Jun) under near-background conditions. Forecast of Solar and Geomagnetic Activity 22 June - 18 July 2026 Solar activity is expected to continue at predominately low levels on 22 Jun- 24 Jun, with an increasing chance for M-class (R1-R2/Minor-Moderate) flares due primarily to the flare potential of Region 4473 (S08, L=133, class/area=Eko/270 on 20 Jun). Additional chances for M- and X- class flares are likely after 30 Jun with the anticipated return of Region 4463 (N16, L=339, class/area=Hsx/70 on 10 Jun). <div> Chances for an S1 or greater proton event increase after 24 Jun as additional magnetically complex active regions are snticipated to return to the visible disk.</div> The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at moderate levels on 22 Jun-03 Jul, 08-09 Jul, and 13-18 Jul. High levels are likely on 05-07 Jul and 10-13 Jul with elevated wind speeds associated with coronal hole high speed streams. Geomagnetic field activity is expected to be quiet to unsettled levels on 22-24 Jun, 27 Jun - 02 Jul, 04-07 Jul, 09-18 Jul. Isolated active periods are possible on 25-26 Jun, 03 Jul, and 15 Jul in response to recurrent, weak CH HSS influence. 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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