|
|
| Warnings and Alerts | |
| Issue Time: 2026 Jun 20 0407 UTC ALERT: Type II Radio Emission Begin Time: 2026 Jun 20 0407 UTC Estimate Velocity: 300 km/s Space Weather Scales | |
| Current Condition and Alerts | |
|
Issued: 2026 Jun 20 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 19 June follow. Solar flux 111 and estimated planetary A-index 7. The estimated planetary K-index at 1200 UTC on 20 June was 1.67. Space weather for the past 24 hours has been minor. Radio blackouts reaching the R1 level occurred. No space weather storms are predicted for the next 24 hours. Space Weather Scales |
|
| Forecast Discussion | |
|
Issued: 2026 Jun 20 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity reached moderate levels when Region 4472 (S14E61, Cao/beta) produced an M1.3 flare (R1-Minor) at 20/0151 UTC; the strongest of the period. Region 4470 (N08E21, Dao/beta) exhibited minor growth this period and produced a C1.4 flare at 20/0307 UTC that was accompanied by a Type-II radio sweep (~300 km/s). The remaining regions were either stable or in decay. New spots were observed rotating into view on the E limb near S08, but these remain unnumbered pending additional observational data. A CME associated with the M1.3 flare at 20/0151 UTC, and first visible in LASCO C2 imagery off the E at 20/0212 UTC, is expected to miss Earth. Another CME, first visible in C2 imagery at 20/0312 UTC, was associated with activity on the far side and is not Earth-directed. .Forecast... Solar activity is expected to continue at low levels on 20-22 Jun, with a slight chance for M-class (R1-Minor) flares. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached moderate levels. The greater than 10 MeV proton flux remained at background values. .Forecast... The greater than 2 MeV electron flux is expected to reach moderate levels over 20-22 Jun. The greater than 10 MeV proton flux is expected to remain at background levels through 22 Jun. Solar Wind .24 hr Summary... Solar wind parameters remained mildly enhanced under positive polarity CH HSS influences. Total magnetic field strength reached 10 nT, and the Bz component was observed as far south as -7 nT. Solar wind speeds ranged between ~360-460 km/s. Phi angle was primarily oriented in a positive solar sector. .Forecast... Solar wind parameters are expected to remain slightly enhanced through 21 Jun due to CH HSS influences. Geospace .24 hr Summary... The geomagnetic field was at quiet to unsettled levels under waning CH HSS influences. .Forecast... The geomagnetic field is expected to continue at quiet to unsettled levels on 20-21 Jun as CH HSS influences diminish. Mostly quiet conditions are expected to prevail on 22 Jun. Space Weather Scales |
|
| Three Day Forecast | |
|
Issued: 2026 Jun 20 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 Jun 20-Jun 22 2026 is 3.00 (below NOAA Scale levels). NOAA Kp index breakdown Jun 20-Jun 22 2026 Jun 20 Jun 21 Jun 22 00-03UT 2.67 2.67 1.67 03-06UT 2.00 3.00 2.00 06-09UT 2.00 2.67 1.67 09-12UT 1.67 2.00 1.67 12-15UT 1.67 1.67 1.00 15-18UT 1.00 0.67 1.33 18-21UT 1.67 1.00 0.67 21-00UT 2.67 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 Jun 20-Jun 22 2026 Jun 20 Jun 21 Jun 22 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 Radio blackouts reaching the R1 levels were observed over the past 24 hours. The largest was at Jun 20 2026 0151 UTC. Radio Blackout Forecast for Jun 20-Jun 22 2026 Jun 20 Jun 21 Jun 22 R1-R2 20% 20% 20% R3 or greater 1% 1% 1% Rationale: There is a slight chance for R1 (Minor) or greater radio blackouts over 20-22 Jun. Space Weather Scales |
|
| Weekly Highlights and Forecasts | |
|
Issued: 2026 Jun 15 0248 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 08 - 14 June 2026 Solar activity was at low levels the entire period, with only C-class flares observed. There were five flares at or above the C5 level, with all but one originating from Region 4465 (N09, L=292, class/area=Dhi/255 on 11 Jun). These included: a C7.2 at 09/0249 UTC, a C6.7/1f at 11/0026 UTC, a C9.0 at 11/0828 UTC (the largest of the period), and finally a C5.2 flare at 12/0214 UTC. The only other flare greater than C5 was a C6.1 flare at 11/0044 UTC from Region 4456 (N17, L=63, class/area=Dai/80 on 08 Jun). Additional activity included a type-II radio sweep at 09/1557 UTC, with an estimated velocity of 917 km/s, likely associated with low-level C-class flaring from Region 4463 (N16, L=339, class/area=Hsx/70 on 10 Jun). An associated CME was first observed in the NE quadrant of LASCO/C2 around 09/1630 UTC, which correlated to an eruption near (and south of) Region 4463. Analysis suggested glancing effects near-Earth on 13-14 June. A second type-II sweep (est. velocity = 1,127 km/s) was detected by the RSTN stations at 10/1715 UTC. An associated CME was first observed in the NE quadrant in LASCO/C2 imagery at 10/1800 UTC, with modeling and analysis indicating no Earth-directed component was likely. The third and final type-II sweep of the period was associated with the C6.7/1f flare from Region 4465 observed at 11/0002 UTC, and had an estimated velocity of 918 km/s. Additionally, a type-IV radio sweep and a partial halo CME were observed, with analysis indicating potential impact near-Earth starting early on 13 Jun. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 08-10 and 13-14 Jun, with a peak flux of 4,259 pfu at 09/1525 UTC. Flux levels were low to moderate on 11-12 Jun. Geomagnetic field activity was at quiet to unsettled levels on 08-10 and 14 Jun under nominal conditions. Active to G1 (Minor) storm conditions were observed on 11 Jun with unsettled to active conditions observed on 12-13 Jun under negative polarity coronal hole high speed stream (CH HSS) influences, combined with weak CME effects, likely associated with the CME that left the Sun on 09 Jun. Forecast of Solar and Geomagnetic Activity 15 June - 11 July 2026 Solar activity is expected to be at mostly low levels through 19 Jun, with increasing chances for M-class activity after 20 Jun with the anticipated return of Region 4455 (N14, L=88, class/area=Dki/360 on 03 Jun) No proton events are expected at geosynchronous orbit, barring siginifcant flare activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at high levels on 15-17 Jun and 04-10 Jul. Normal to moderate levels are expected to prevail throughout the remainder of the period. Geomagnetic field activity is expected to be at quiet to unsettled levels on 15, 17-24, and 26-30 Jun, as well as 01-02, 04-07, and 10-11 Jul. Active conditions are likely on 16, and 25 Jun and 03, 08, and 09 Jul under elevated CH HSS influence. 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 | |
 |
|
| Daily Video HMI Continuum | |
 |
|
| Daily Video 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. |