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| Warnings and Alerts | |
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Issue Time: 2026 Jan 23 0903 UTC
EXTENDED WARNING: Geomagnetic K-index of 4 expected Extension to Serial Number: 5231 Valid From: 2026 Jan 22 2224 UTC Now Valid Until: 2026 Jan 23 1800 UTC Warning Condition: Persistence Potential Impacts: Area of impact primarily poleward of 65 degrees Geomagnetic Latitude. Induced Currents - Weak power grid fluctuations can occur. Aurora - Aurora may be visible at high latitudes such as Canada and Alaska. Space Weather Scales |
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| Current Condition and Alerts | |
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Issued: 2026 Jan 23 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 22 January follow. Solar flux 194 and estimated planetary A-index 18. The estimated planetary K-index at 1200 UTC on 23 January was 4.33. 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 G1 level are expected. Radio blackouts reaching the R2 level are likely. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Jan 23 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 4342 (N13W45, Dso/beta), 4345 (S17W42, Eai/beta-delta), 4351 (S05W08, Dai/beta), and 4353 (N17W03, Dao/beta-delta). The largest flare was a C9.5 at 22/1954 UTC. Slight growth was observed in Regions 4348 (S17W71, Cro/beta), 4351, 4353 and new Region 4354 (S13W00, Bxo/beta). Regions 4344 (N19W56, L=52) and 4350 (N21E04, L=353) decayed to plage. All remaining regions were either stable or in slight decay. No Earth-directed CMEs were observed. .Forecast... Solar activity is likely (60%) to be at moderate (R1/R2, Minor/Moderate) levels, with a slight chance (10%) for X-class flares (R3-Strong) on 23-25 Jan, primarily due to the magnetic potential of Regions 4342, 4345, 4351, and 4353. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached high levels with a peak flux of 5,365 pfu observed at 22/1420 UTC. The greater than 10 MeV proton flux was below the S1 (Minor) threshold and still returning to background levels. .Forecast... The greater than 2 MeV electron flux is expected to reach high levels on 23-25 Jan. The greater than 10 MeV proton enhancement is expected to continue to decline towards background levels over 23-25 Jan. Solar Wind .24 hr Summary... Solar wind parameters reflected high speed stream activity. Solar wind speed fluctuated between ~500-550 km/s. The total magnetic field (Bt) slowly decreased over the reporting period from ~10 nT to ~5 nT, while the Bz (north-south) component was between +8/-7 nT with two intervals of sustained ~-7 nT: one for 4 hrs starting at starting at 22/2045 UTC and another for 2 hrs starting at 23/0645 UTC. Phi angle was variable but largely positive (away from the Sun) for the majority of the reporting period. .Forecast... Solar wind parameters are expected to gradually diminish with possible intermittent connections with the positive polarity CH HSS over 23-25 Jan. Geospace .24 hr Summary... The geomagnetic field was at quiet to G1 (Minor) storm levels due to a period of sustained southward Bz at the end of the reporting period. .Forecast... The geomagnetic field is expected to be at unsettled to G1 (Minor) levels on 23 Jan as HSS activity persists. Quiet to unsettled levels are expected on 24-25 Jan as HSS activity gradually wanes. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Jan 23 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 Jan 23-Jan 25 2026 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Jan 23-Jan 25 2026 Jan 23 Jan 24 Jan 25 00-03UT 4.33 3.00 2.33 03-06UT 4.00 3.00 2.67 06-09UT 3.67 2.33 2.33 09-12UT 4.33 2.33 1.67 12-15UT 4.67 (G1) 1.67 1.33 15-18UT 3.67 1.67 1.33 18-21UT 2.33 2.00 2.00 21-00UT 2.67 2.33 2.33 Rationale: G1 (Minor) geomagnetic storms are possible on 23 Jan due to periods of sustained -Bz in an ongoing high speed stream. 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 23-Jan 25 2026 Jan 23 Jan 24 Jan 25 S1 or greater 10% 10% 10% Rationale: There is a slight chance for S1 (Minor) or greater solar radiation storms on 23-25 Jan. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for Jan 23-Jan 25 2026 Jan 23 Jan 24 Jan 25 R1-R2 60% 60% 60% R3 or greater 10% 10% 10% Rationale: R1-R2 (Minor-Moderate) radio blackouts are likely, with a slight chance for R3 (Strong) events, on 23-25 Jan. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Jan 19 0216 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 12 - 18 January 2026 Solar activity ranged from low to strong levels. Forty-five C-class, three M-class (R1-Minor) and one X-class (R3-Strong) activity was observed from various regions on the disk during the period. A majority of the activity was observed from Regions 4341 (S11, L=046, class/area Dkc/840 on 16 Jan), 4342 (N17, L=041, class/area Dso/180 on 16 Jan) and 4343 (S11, L=097, class/area Dki/310 on 16 Jan). Region 4341 produced the following R1 (Minor) flare activity; an M1.6/1f at 14/2033 UTC, an M2.1/2b at 17/1029 UTC and an M1.1/2n at 17/2351 UTC. This region also produced an X1.9/3b long-duration event at 18/1809 UTC. Associated with this flare was a 693 km/s Type II sweep, a Type IV sweep, a 3,200 sfu Tenflare and a Castelli-U radio burst. An associated full-halo CME was first noted in GOES CCOR-1 imagery at about 18/1830 UTC. Additional coronagraph imagery will determine any Earth-directed component. A 10 MeV at 10 pfu proton event at geosynchronous orbit (S1-Minor) was first observed at 18/2255 UTC. This event occurred in association with the X1.9 flare at 18/1830 UTC. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 12-18 Jan. A peak flux of 9,398 pfu was observed at 14/1645 UTC. Geomagnetic field activity was at quiet to minor storm levels (G1-Minor) throughout the period. Quiet to active levels were detected on 12-13 Jan associated with waning CME influence and effects from a negative polarity CH HSS. Mostly quiet levels were observed on 14 Jan. Unsettled to minor storm (R1-Minor) levels were detected on 15 through midday on 17 Jan. Unsettled to active levels were observed on the later half of 17 Jan through 18 Jan due to positive polarity CH HSS. Forecast of Solar and Geomagnetic Activity 19 January - 14 February 2026 Solar activity is likely to remain at low levels, with a chance for R1-R2 (Minor-Moderate) and a slight chance for R3 (Strong) levels over the next forecast period, all due to multiple regions on the visible disk as well as regions expected to return. 10 Mev at 10 pfu proton events (S1-Minor) are expected at geosynchronous orbit on 19-20 Jan. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 19-27 Jan and 12-14 Feb, all due to the anticipated influence of multiple, recurrent coronal holes. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity is likely to reach (G1-Minor) geomagnetic storm levels on 29 Jan and unsettled to active levels on 19-23, 27-28, 30-31 Jan, 04-11 and 13-14 Feb. All enhancements in activity are due to the anticipated influence of multiple, recurrent CH HSSs. The remainder of the outlook period is expected to be mostly quiet. 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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