| Warnings and Alerts | |
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Issue Time: 2025 Nov 26 1045 UTC
EXTENDED WARNING: Geomagnetic K-index of 4 expected Extension to Serial Number: 5160 Valid From: 2025 Nov 24 0226 UTC Now Valid Until: 2025 Nov 26 2359 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: 2025 Nov 26 1210 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 25 November follow. Solar flux 116 and estimated planetary A-index 32. The estimated planetary K-index at 1200 UTC on 26 November was 3.67. 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. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2025 Nov 26 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity was low with only C-class level flares. Region 4291 (S14E19, Eai/beta-gamma) remains to be the largest most complex region on the disk. There was weak flux emergence in its intermediate region producing a new spot that looks to be merging with the trailer. Due to this new growth Region 4291 will maintain its gamma configuration, but is becoming more stable throughout its magnetic field otherwise. Region 4292 (S16W34, Dai/beta) was responsible for a few flares and exhibited growth throughout the period. Circular structure of the flux emergence increases its likelihood for flare activity moving forward. There was a Type II radio sweep at 25/1950 UTC with a velocity of 1050 km/s according to the radio observatory in Hawaii. The associated CME can be seen off the NE part of the disk. Considerable field line movement and ejecta can be seen in the GOES-19 SUVI imagery channels 195 and 304, respectively. Because the source region was beyond the east limb, there poses no impact to Earth. .Forecast... Simple regions throughout the disk will maintain lower chances for flare activity through 28 Nov, with only a 15% chance for M-class (Minor-Moderate) and 1% for X-class (Strong). Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux increased above the 1,000 pfu threshold around 25/1220 UTC and reached a peak of 3,722 pfu. This is due to the geoeffective positioning of the positive polarity coronal hole (CH) high speed stream (HSS). Electrons showed a similar pattern during the passage of this CH HSS one Bartel (27 days) rotation ago, but did not increase until winds relaxed. This rotation however, the CH is significantly larger - extending from the equator to the south pole. Influx of electrons may be too great to be dictated by wind speeds this time around. The greater than 10 MeV proton flux was at background levels. .Forecast... Electrons will remain high at geostationary orbit through 27 Nov due to ongoing effects from the CH HSS. Chances for protons becoming elevated are unlikely (1% chance) due to the simplicity of regions on the disk. Solar Wind .24 hr Summary... Solar wind parameters, as measured by the ACE spacecraft, were enhanced due to the geoeffective position of the positive polarity CH HSS. The total interplanetary magnetic field was between 5-7 nT with the north-south (Bz) component oscillating between +/-6 nT which is typical within a HSS. Solar wind speeds remained between 700-800 km/s. The phi angle remained in the positive (away from the Sun) sector. .Forecast... Solar wind parameters will persist at these levels through the 28 Nov with waning conditions thereafter. Geospace .24 hr Summary... The geomagnetic field was at unsettled to active levels. .Forecast... Due to high solar wind speeds within the CH HSS, isolated periods of G1 (Minor) geomagnetic storming levels will likely continue through 27 Nov. Conditions will diminish to unsettled to active levels 28 Nov. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2025 Nov 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 4 (below NOAA Scale levels). The greatest expected 3 hr Kp for Nov 26-Nov 28 2025 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Nov 26-Nov 28 2025 Nov 26 Nov 27 Nov 28 00-03UT 3.33 4.67 (G1) 4.00 03-06UT 4.00 4.33 4.00 06-09UT 4.00 4.67 (G1) 3.67 09-12UT 3.67 4.00 3.67 12-15UT 3.67 3.67 3.67 15-18UT 3.67 3.67 4.00 18-21UT 4.00 4.00 4.00 21-00UT 4.67 (G1) 4.33 3.67 Rationale: G1 (Minor) geomagnetic storming will remain likely through 27 Nov due to persistant 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 Nov 26-Nov 28 2025 Nov 26 Nov 27 Nov 28 S1 or greater 1% 1% 1% 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 Nov 26-Nov 28 2025 Nov 26 Nov 27 Nov 28 R1-R2 15% 15% 15% R3 or greater 1% 1% 1% Rationale: A slight chance for R1-2 (Minor-Moderate) radio blackouts due to M-class flare activity will persist through 28 Nov. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2025 Nov 24 0142 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 17 - 23 November 2025 Solar activity was at low levels. C-class activity was observed from Regions 4274 (N25, L=274), 4284 (S07, L=177, class/area Dai/150 on 19 Nov), 4290 (S10, L=035, class/area Cao/120 on 22 Nov) and 4291 (S14, L=028, class/area Dao,120 on 22 Nov). No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 19-20 Nov with a peak flux of 2,880 pfu on 20/1435 UTC. Normal to moderate levels were reached on 17-18 Nov and 21-23 Nov. Geomagnetic field activity was at mostly quiet to unsettled levels with isolated active levels observed early on 17 Nov and midday on 23 Nov. Solar wind parameters were enhanced midday on 20 Nov when Bt reached 18 nT and Bz reached values at -10 nT. Solar wind speeds began the highlight period at about 550 km/s, declined to near 325 km/s early on 20 Nov and gradually increased to about 500 km/s late on 23 Nov. Forecast of Solar and Geomagnetic Activity 24 November - 20 December 2025 Solar activity is expected to be expected to be at R1-R2 (Minor-Moderate) levels on 28-30 Nov and 01-11 Dec, primarily due to the flare potential and return of old Region 4274. Mostly C-class activity is expected on 24-27 Nov and 12-20 Dec. No proton events are expected at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at high levels on 28-30 Nov, 01-03 Dec, 08-12 Dec and 16-17 Dec, all due to coronal hole influence. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity is expected to range from quiet to G1-G2 (Minor-Moderate) geomagnetic storm levels. G1-G2 (Minor-Moderate) levels are likely on 26-27 Nov and 03-04 Dec due to anticipated influence from CH HSS. Unsettled to active conditions are likely on 24-25 Nov, 28-30 Nov, 05-07 Dec, 12-14 Dec and 17-19 Dec. Mostly quiet levels are likely on 01-02 Dec, 08-11 Dec, 15-16 Dec and 20 Dec. 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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