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| Warnings and Alerts | |
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Issue Time: 2026 Jan 26 0906 UTC
WATCH: Geomagnetic Storm Category G1 Predicted Highest Storm Level Predicted by Day: Jan 27: None (Below G1) Jan 28: G1 (Minor) Jan 29: None (Below G1) THIS SUPERSEDES ANY/ALL PRIOR WATCHES IN EFFECT Comment: Negative polarity CH influences will likely lead to isolated G1 (Minor) geomanetic storming periods on 28 Jan. 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 Jan 26 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 25 January follow. Solar flux 165 and estimated planetary A-index 15. The estimated planetary K-index at 1200 UTC on 26 January was 2.33. 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 Jan 26 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. Region 4342 (N16W78, Dso/beta) produced a C7.9 flare that peaked at 25/2143 UTC, which was the largest of the period. CMEs associated with this event were first observed in LASCO C2 coronagraph imagery beginning at approximately 25/2012 UTC. However, these CMEs are not expected to have an Earth-directed component given their source location on the western limb. New simple spots were observed near N17E12, but remain unnumbered at this time given a lack of substantial growth or activity in their few hours of existence. The remaining numbered active regions were relatively stable and quiet, or were in decay. .Forecast... Solar activity is expected to be low with a chance for M-class flares (R1/R2, Minor/Moderate) through 28 Jan. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached high levels with a peak flux of 6,154 pfu observed at 25/1640 UTC. The greater than 10 MeV proton flux was below the S1 (Minor) threshold. .Forecast... The greater than 2 MeV electron flux is expected to remain at high levels on 26 Jan before decreasing to normal to moderate levels on 27 Jan. The greater than 10 MeV proton flux is expected to remain at background levels through 28 Jan. Solar Wind .24 hr Summary... Solar wind parameters reflected weakening positive polarity CH HSS influence and a possible weak transient disturbance late in the period. Total field primarily ranged 4-6 nT, but underwent an increase to 7-8 nT beginning around 26/0542 UTC. The Bz component of the IMF was mostly near neutral or northward with only a few weak southward deflections. Solar wind speeds exhibited an overall decreasing trend ending the period near 500 km/s. Phi was predominantly positive with a few brief excursions into the negative solar sector. .Forecast... Positive polarity CH HSS influencesare expected to gradually diminish over 26 Jan into the first half of 27 Jan. The latter half of 27 Jan should bring negative polarity CH HSS influences and enhancements into the solar wind environment, which will then continue through 28 Jan. Geospace .24 hr Summary... Geomagnetic field activity was at quiet to unsettled levels. .Forecast... Quiet to unsettled geomagnetic conditions are expected to give way to mostly quiet levels by early on 27 Jan. Unsettled conditions are then possible again by late on 27 Jan due to an anticipated solar sector boundary crossing. Isolated G1 (Minor) geomagnetic storming periods are likely on 28 Jan with the onset of negative polarity CH HSS effects. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Jan 26 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 Jan 26-Jan 28 2026 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Jan 26-Jan 28 2026 Jan 26 Jan 27 Jan 28 00-03UT 2.33 2.00 4.00 03-06UT 1.00 1.67 4.67 (G1) 06-09UT 2.00 2.00 3.33 09-12UT 2.33 1.67 3.00 12-15UT 1.33 1.67 3.33 15-18UT 1.67 2.00 3.67 18-21UT 2.00 2.33 4.00 21-00UT 2.67 3.33 4.00 Rationale: G1 (Minor) geomagnetic storming is likely on 28 Jan due to negative polarity CH HSS effects. 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 Jan 26-Jan 28 2026 Jan 26 Jan 27 Jan 28 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 Jan 26-Jan 28 2026 Jan 26 Jan 27 Jan 28 R1-R2 40% 35% 35% R3 or greater 5% 5% 5% Rationale: A chance for R1-2 (Minor-Moderate) radio blackouts due to isolated M-class flares will persist through 28 Jan. Probabilities decrease slightly after day 1 as active regions rotate off of the visible disk. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Jan 26 0257 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 19 - 25 January 2026 Solar activity reached moderate levels on 19 and 21 Jan with three M-class flares (R1-Minor) observed. Region 4345 (S17, L=39, class/area=Esi/160 on 24 Jan) produced an M1.1 flare at 19/1119 UTC and an M1.1/Sf flare at 21/0135 UTC. Region 4349 (S14, L=336, class/area=Dso/230 on 25 Jan) produced an M3.4/1b flare at 21/0712 UTC, the strongest flare of the week. No Earth-directed CMEs were observed in association with flare activity from 19-25 Jan. The greater than 10 MeV proton flux reached S4 (Severe) storm levels on 19 Jan, decreased to S2 (Moderate) levels on 20 Jan, and remained at S1 (Minor) levels on 21-22 Jan following an X1.9/3b flare from Region 4341 that peaked at 18/1809 UTC. Proton fluxes gradually declined over 23-25 Jan. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 19 and 21-25 Jan, with normal to moderate levels observed on 20 Jan. Geomagnetic field activity reached G4 (Severe) storm levels on 19-20 Jan and G3 (Strong) levels on 21 Jan following the arrival of a halo CME associated with the X1.9/3b flare at 18/1809 UTC from Region 4341. G1 (Minor) storming was observed on 22 Jan due to lingering CME effects and the onset of positive polarity CH HSS influences. Active conditions were observed on 23-24 Jan, with quiet to unsettled levels observed on 25 Jan, in response to continued positive polarity CH HSS influences. Forecast of Solar and Geomagnetic Activity 26 January - 21 February 2026 Solar activity is expected to be predominately low with a varying chance for M-class flares (R1-R2/Minor-Moderate) through 21 Feb. 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 26, 28-31 Jan and 01-03, 06-12, 15-21 Feb. Normal to moderate flux levels are expected to persist through the remainder of the period. Geomagnetic field activity is likely to reach G1 (Minor) storm levels on 28 Jan and 13 Feb, with active periods likely on 29 Jan and 04-05, 14-21 Feb, due to the influences of multiple, recurrent CH HSSs. Quiet and quiet-to-unsettled conditions are expected to prevail throughout the remainder of the outlook period. 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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| 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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