|
|
| Warnings and Alerts | |
| No Current Warnings Space Weather Scales | |
| Current Condition and Alerts | |
|
Issued: 2026 Mar 10 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 09 March follow. Solar flux 128 and estimated planetary A-index 7. The estimated planetary K-index at 1200 UTC on 10 March was 3.00. 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 |
|
| Forecast Discussion | |
|
Issued: 2026 Mar 10 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity was low. Low-level C-class flares were observed from Regions 4381 (N08W56, Cso/beta), 4387 (N09E46, Dro/beta) and new Region 4389 (N13E67, Ero/beta). The largest event of the period was a C7.8/Sf observed at 09/2038 UTC from Region 4387. Region 4381 simplified with some dissipation of its intermediate spots, while Region 4384 (N09W34, Cso/beta) showed a decline in its trailing spot. Region 4385 (S09, L=161) decayed to plage. Region 4387 remained relatively stable throughout the period. Region 4388 (S15W25, Cri/beta) was numbered this period and showed some evolution with new flux emergence and reconfiguration of the group, though its overall extent remained largely unchanged. No Earth-directed CMEs were observed in available coronagraph imagery. .Forecast... Solar activity is expected to be at low levels, with a slight chance for M-class (R1-R2/Minor-Moderate) flares through 12 Mar. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached high levels with a peak flux of 1,320 pfu observed at 09/1610 UTC. 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 10-12 Mar. The greater than 10 MeV proton flux is expected to continue at background levels through 12 Mar. Solar Wind .24 hr Summary... Solar wind parameters indicated a waning, negative-polarity, CH HSS influence. Solar wind speed decreased from approximately 480 km/s to near 400 km/s. Total field ranged from 1-5 nT while the Bz component was between +/-5 nT. Phi angle was predominantly negative. .Forecast... Mildly enhanced solar wind parameters are expected to continue through 10 Mar as HSS conditions continue to wane, alongside possible transient influences from the 06 Mar CME. A return to nominal levels is expected on 11-12 Mar. Geospace .24 hr Summary... The geomagnetic field was quiet to unsettled. .Forecast... The geomagnetic field is expected to be quiet to unsettled on 10 Mar as HSS conditions continue to diminish with enhancements possible due to the anticipated arrival of the 06 Mar CME. Mostly quiet conditions are expected on 11-12 Mar. Space Weather Scales |
|
| Three Day Forecast | |
|
Issued: 2026 Mar 10 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 Mar 10-Mar 12 2026 is 3.33 (below NOAA Scale levels). NOAA Kp index breakdown Mar 10-Mar 12 2026 Mar 10 Mar 11 Mar 12 00-03UT 3.33 2.67 1.67 03-06UT 2.67 2.33 1.33 06-09UT 2.33 2.00 1.33 09-12UT 3.00 1.00 1.33 12-15UT 1.00 1.33 1.33 15-18UT 1.00 1.33 1.67 18-21UT 1.67 1.67 1.33 21-00UT 2.00 1.67 1.67 Rationale: No G1 (Minor) or greater geomagnetic storms are expected. No significant transient or recurrent solar wind features are forecast. 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 Mar 10-Mar 12 2026 Mar 10 Mar 11 Mar 12 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 Mar 10-Mar 12 2026 Mar 10 Mar 11 Mar 12 R1-R2 20% 20% 20% R3 or greater 1% 1% 1% Rationale: There exists a slight chance for R1-R2 (Minor-Moderate) radio blackouts over 10-12 Mar. Space Weather Scales |
|
| Weekly Highlights and Forecasts | |
|
Issued: 2026 Mar 09 0207 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 02 - 08 March 2026 Solar activity was at low levels with a total of 24 C-class flares observed. The largest flares of the period were observed early on 02 March; a C6.1 flare at 02/0206 UTC from Region 4380 (S20, L=195, class/area Dao/140 on 26 Feb) and a C5.2 at 02/0615 UTC and a C 5.9 at 02/ 0749 UTC, both from Region 4381 (N08, L=173, class/area Eao/220 on 03 Mar). Region 4384 (N10, L=150, class/area Eho/300 on 03 Mar) was the most active, producing 10 weak C-class events. No Earth-directed CMEs were observed in available LASCO imagery. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 02, 03 and 08 Mar with a peak flux of 10,450 pfu observed at 02/1810 UTC. Normal to moderate levels were observed on 04-07 Mar. Geomagnetic field activity reached quiet to G1 (Minor) geomagnetic storm levels during the period. Quiet levels were observed on 02 Mar through midday on 03 Mar. Unsettled to G1 (Minor) storm levels were observed on the last half of 03 Mar into early 04 Mar due to effects from a positive polarity CH HSS. Quiet to isolated unsettled levels were observed on a majority of 04 Mar through 06 Mar. Negative polarity CH HSS effects influenced 07-08 Mar with quiet to active levels observed on the 7th and quiet to G1 (minor) storms observed on 08 Mar. Solar wind parameters observed a peak wind speed of about 675 km/s late on 07 Mar. Total field reached peaks of 11 nT on 03 Mar and 12 nT midday on 07 Mar, while Bz was southward to -10 nT late on 03 Mar and -9 nT late on 06 Mar. Phi angle was in a mostly positive orientation on 02 Mar through midday on 06 Mar and in a negative orientation from midday on 06 Mar through 08 Mar. Forecast of Solar and Geomagnetic Activity 09 March - 04 April 2026 Solar activity is expected to be at low levels, with a slight chance for M-class (R1-R2/Minor-Moderate) flares throughout the outlook period. Elevated probabilities are related to the flare potential of both currently observed spot groups as well as the potential from returning regions. 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 09-11, 16-19, 23-30 Mar and 04 Apr due to the influence from multiple, recurrent, CH HSSs. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity is expected to reach G1 (Minor) geomagnetic storm levels on 14 Mar, 22 Mar, 25 Mar and 03-04 Apr during the onset CH HSS. G2 (Moderate) geomagnetic storm levels are likely on 21 Mar due to negative polarity CH HSS effects. Unsettled to active levels are likely on 09-11, 15-20, 23-24, 26-28, 30 Mar and 02 Apr. All elevated levels of geomagnetic activity are associated with the anticipated influence of multiple, recurrent, CH HSSs. The remainder of the outlook period is likely to be at mostly quiet levels. 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 | |
 |
|
| Daily Image AIA 171 PFSS Model | |
 |
|
| Daily Image AIA 193 | |
 |
|
| Daily Image AIA 304 | |
 |
|
| Daily Video AIA 171 | |
 |
|
| Daily Video AIA 171 PFSS Model | |
 |
|
| 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. |
.jpg)