Space Weather

Warnings

Issue Time: 2025 Oct 29 1112 UTC EXTENDED WARNING: Geomagnetic K-index of 4 expected Extension to Serial Number: 5122 Valid From: 2025 Oct 27 2325 UTC Now Valid Until: 2025 Oct 29 2100 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

Current Condition and Alerts

Issued: 2025 Oct 29 1205 UTC Prepared by the US Dept. of Commerce, NOAA, Space Weather Prediction Center Geophysical Alert Message Solar-terrestrial indices for 28 October follow. Solar flux 122 and estimated planetary A-index 19. The estimated planetary K-index at 1200 UTC on 29 October was 3.00. 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

Forecast Discussion

Issued: 2025 Oct 29 1230 UTC Prepared by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction Center Solar Activity .24 hr Summary... Solar activity reached low levels due to an isolated C1.6 flare at 28/1626 UTC from Region 4267 (N04W05, Dso/beta). Slight growth was observed in Regions 4267 and 4266 (N17W31, Cro/beta). The rest of the spotted regions were either stable or in decay. Other activity included a CME off the NE limb at 29/0012 UTC. An associated Type II radio sweep (1,357 km/s) was reported with the CME, however SUVI 195 imagery revealed the CME to have originated on the far side. Also, an approximate 12 degree filament eruption, centered near N27W24 was observed lifting off beginning at 29/0058 UTC. CME analysis will be conducted as imagery becomes available. .Forecast... Solar activity is expected to remain very low to low through 31 Oct. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux was at normal to moderate levels. The greater than 10 MeV proton flux was at background levels. .Forecast... The greater than 2 MeV electron flux is expected to reach high levels on 30-31 Oct in response to the positive coronal hole (CH) high speed stream (HSS) influence. The greater than 10 MeV proton flux is expected to remain at background levels through 31 Oct. Solar Wind .24 hr Summary... Solar wind parameters continued under CH HSS influence, albeit to a lesser extent than recurrent trends. Solar wind speed increased from approximately 400 km/s to near 480 km/s. Total field continued to be enhanced around 9-13 nT with the Bz component between +12/-11 nT. Phi angle was predominantly positive. .Forecast... Solar wind parameters are expected to continue to reflect positive CH/HSS influences through 31 Oct. Geospace .24 hr Summary... The geomagnetic field has been unsettled to active due to CH HSS activity. .Forecast... Unsettled to active conditions are expected through 31 Oct, with G1 (Minor) storming likely on 29-30 Oct, due to persistent CH HSS effects. Space Weather Scales

Three Day Forecast

Issued: 2025 Oct 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 4 (below NOAA Scale levels). The greatest expected 3 hr Kp for Oct 29-Oct 31 2025 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Oct 29-Oct 31 2025 Oct 29 Oct 30 Oct 31 00-03UT 3.00 4.67 (G1) 3.67 03-06UT 3.00 4.00 3.67 06-09UT 3.33 4.00 3.33 09-12UT 3.00 3.67 3.00 12-15UT 3.00 3.67 3.00 15-18UT 4.00 4.00 3.33 18-21UT 4.67 (G1) 3.33 3.00 21-00UT 4.00 3.33 3.00 Rationale: G1 (Minor) geomagnetic storming is likely on 29-30 Oct due to persistent 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 Oct 29-Oct 31 2025 Oct 29 Oct 30 Oct 31 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 Oct 29-Oct 31 2025 Oct 29 Oct 30 Oct 31 R1-R2 5% 5% 5% R3 or greater 1% 1% 1% Rationale: No R1 (Minor) or greater radio blackouts are expected. No significant active region flare activity is forecast. Space Weather Scales

Weekly Highlights and Forecasts

Issued: 2025 Oct 27 0243 UTC Prepared by the US Dept. of Commerce, NOAA, Space Weather Prediction Center Highlights of Solar and Geomagnetic Activity 20 - 26 October 2025 Solar activity was at moderate levels on 20 Oct with a single M-class flare observed. Region 4248 (N07, L=262, class/area=Eki/380 on 17 Oct) produced an M1.1 flare, the largest of the period, at 20/0527 UTC. Region 4262 (S12, L=132, class/area=Cai/150 on 22 Oct) produced a pair of long duration C-class flares. The first was a C4.7 that peaked at 22/0152 UTC, with the second being a C2.7 flare at 22/0909 UTC. Additionally, there were two far sided CMEs, likely originating from old Region 4246 (N24, L=290, class/area=Ekc/840 on 16 Oct). These events were observed in LASCO coronagraph imagery on 21/2024 UTC. Additionally, Type II (est. 2474 km/s) and Type IV radio sweeps were observed at 21/2011 UTC, likely associated with the far-sided events as well. There was also a weak CME observed in LASCO imagery on 23/1545 UTC, likely associated with a C2.1 flare at 23/1506 UTC from Region 4256 (S15, L=155, class/area=140/Dao on 18 Oct. This CME is expected to arrive at Earth on 27 Oct. Activity was at low levels from 21-26 Oct. No proton events were observed at geosynchronous orbit. However, the 10 MeV proton flux levels were slightly elevated on 22-23 Oct following the far-sided CME eruptions. Conditions were at background levels on 20-21 Oct and 24-26 Oct. The greater than 2 MeV electron flux at geosynchronous orbit was at normal to moderate levels from 20-26 Oct. Geomagnetic field activity was at mostly quiet to unsettled levels from 20-26 Oct, with the exception of an isolated active period on 25 Oct, likely associated with residual CH HSS influence. Forecast of Solar and Geomagnetic Activity 27 October - 22 November 2025 Solar activity is expected to be at moderate levels on 31 Oct - 15 Nov due to the return of Region 4246. Low levels are expected to prevail on 20 Oct - 30 Oct and 14 Nov - 22 Nov as multiple regions depart the visible disk. No proton events are expected at geosynchronous orbit from 27 Oct - 22 Nov. However, depending on the complexity of returning Region 4246, an isolated proton event is possible. The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at high levels from 31 Oct - 15 Nov due to responses from recurrent CH HSS influences. Moderate levels are expected on 27 - 30 Oct and 16 Nov - 22 Nov. Geomagnetic field activity is expected to be at quiet to unsettled levels on 01 Nov - 06 Nov, 10 Nov - 14 Nov, and 16 Nov - 22 Nov. Active conditions are expected on 27 Oct and 31 Oct, 07 Nov - 09 Nov, and 15 Nov, with G1/G2 conditions likely on 28 Oct - 30 Oct due to recurrent positive polarity CH HSS influence, mixed with possible weak influence from the CME that left the Sun on 23 Oct. 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

Channel | Region of atmosphere | Primary ion(s) 171Å | quiet corona, upper transition region | Fe IX

Daily Image AIA 171 PFSS Model

Currently No Data AIA 171 PFSS Channel | Region of atmosphere | Primary ion(s) 171Å | quiet corona, upper transition region | Fe IX

Daily Image AIA 193

Channel | Region of atmosphere | Primary ion(s) 193Å | corona and hot flare plasma | Fe XII, XXIV

Daily Image AIA 304

Channel | Region of atmosphere | Primary ion(s) 304Å | chromosphere, transition region | He II

Daily Video AIA 171

Daily Video AIA 171 PFSS Model

Currently No Data PFSS Video

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

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.