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| Warnings and Alerts | |
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Issue Time: 2026 Apr 15 0756 UTC
CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu Continuation of Serial Number: 3675 Begin Time: 2026 Apr 03 0920 UTC Yesterday Maximum 2MeV Flux: 1705 pfu Potential Impacts: Satellite systems may experience significant charging resulting in increased risk to satellite systems. Space Weather Scales |
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| Current Condition and Alerts | |
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Issued: 2026 Apr 15 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 14 April follow. Solar flux 101 and estimated planetary A-index 4. The estimated planetary K-index at 1200 UTC on 15 April was 0.67. 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 |
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| Forecast Discussion | |
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Issued: 2026 Apr 15 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity was at very low levels with only isolated B-class flaring mostly from Region 4416 (N20W37, Dso/beta). There are currently four numbered regions on the visible disk. Region 4416 remains the largest group by area but exhibited signs of structural weakening, including flux submergence and a slight decay of its intermediary pores. Region 4419 (N13E58, Csi/beta-gamma) was the most complex group on the disk and showed flux emergence, growth, and divergence within its intermediary spots, leading to the development of a mixed-polarity gamma configuration. Region 4418 (S11W07, Bxo/beta) is trending toward plage with only two small bipolar pores remaining and Region 4415 (S18W05, Hsx/alpha) remained stable. CMEs observed in coronagraph imagery were determined to be directed away from Earth. .Forecast... Solar activity is expected to be at low to very low levels, with a slight chance for M-flares (R1-R2/Minor-Moderate) through 17 Apr. Energetic Particle .24 hr Summary... Electrons greater than 2 MeV at geosynchronous orbit reached high levels with a peak of 1705 pfu observed at 14/1445 UTC. The greater than 10 MeV proton flux was at background levels. .Forecast... The greater than 2 MeV electron flux is likely to reach high levels through 17 Apr. The greater than 10 MeV proton flux is expected to remain at background levels through 17 Apr. Solar Wind .24 hr Summary... Solar wind parameters reflected waning coronal hole high speed stream influences toward a nominal regime. Total magnetic field (Bt) remained steady and weak, generally ranging between 4 and 6 nT. The North-South (Bz) component was predominantly northward, though it exhibited occasional southward deviations with a maximum deflection of -4 nT. Solar wind speeds underwent a gradual, albeit erratic, decline from early-period highs near 420 km/s, to stabilize around 375 km/s by the end of the reporting period. The phi angle was predominantly oriented in a positive (away from the Sun) orientation. .Forecast... Solar wind parameters are expected to remain primarily near nominal levels through 16 Apr. Significant enhancements are anticipated on 17 Apr with the onset of a corotating interaction region (CIR) that will precede the arrival of a negative polarity high-speed stream (-CH HSS). Geospace .24 hr Summary... The geomagnetic field was quiet. .Forecast... The geomagnetic field is expected to be at mostly quiet to unsettled through 16 Apr. Activity is forecast to increase on 17 Apr to active levels in response to the arrival of the CIR and the subsequent onset of the -CH HSS. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Apr 15 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 1 (below NOAA Scale levels). The greatest expected 3 hr Kp for Apr 15-Apr 17 2026 is 4.00 (below NOAA Scale levels). NOAA Kp index breakdown Apr 15-Apr 17 2026 Apr 15 Apr 16 Apr 17 00-03UT 0.67 1.67 2.33 03-06UT 1.33 2.67 2.67 06-09UT 1.33 2.67 4.00 09-12UT 0.67 2.33 3.67 12-15UT 2.67 1.67 3.33 15-18UT 2.33 1.67 2.67 18-21UT 2.33 1.67 3.33 21-00UT 1.67 2.33 3.67 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 Apr 15-Apr 17 2026 Apr 15 Apr 16 Apr 17 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 Apr 15-Apr 17 2026 Apr 15 Apr 16 Apr 17 R1-R2 10% 15% 15% R3 or greater 1% 1% 1% Rationale: There is a slight chance for R1-R2 (Minor-Moderate) radio blackouts on 15-17 Apr, primarily due to the development of Region 4419. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Apr 13 0104 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 06 - 12 April 2026 Solar activity was at very low to moderate levels during the period. Moderate levels were reached on 09 Apr, with low levels observed on 06-08 Apr and 11-12 Apr. Very low levels occurred on 10 Apr. Region 4409 (N02, L=158, class/area=Eai/190 on 07 Apr) was the most active region of the period, producing 11 C-class flares and the only M-class flare of the period, an impulsive M1.0/Sf at 09/0845 UTC. Region 4417 (S08, L=123, class/area=Dao/30 on 12 Apr) also contributed notable activity with 7 C-class flares after appearing quickly on 11 Apr near the West limb. Other activity included a C8.7/Sf flare from Region 4414 (N15, L=26, class/area Dro/30 on 08 Apr) at 08/1543 UTC, which was associated with Type III radio emissions and a weak CME without any Earth-directed components. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit was at high levels throughout the reporting period. Flux levels reached a peak value of 10,679 pfu at 09/1605 UTC. Geomagnetic field activity ranged from quiet to active levels during the period. The beginning of the period (06-07 Apr) saw quiet to unsettled conditions as the influence of a negative polarity coronal hole high speed stream (-CH HSS) continued to wane. From 10-12 Apr, quiet to active levels were observerd under the onset and influence of a positive polarity CH HSS (+CH HSS). Quiet conditions prevailed during all other days of the period under a nominal solar wind regime. Forecast of Solar and Geomagnetic Activity 13 April - 09 May 2026 Solar activity is expected to be at low levels, with a varying chance for M-class (R1-R2/Minor-Moderate) flares and a slight chance for X-class (R3/Strong or greater) flares through 09 May. No proton events are expected at geosynchronous orbit, barring any significant, non-recurrent solar activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 13-17 Apr, 19-24 Apr, 26-28 Apr, 30 Apr-05 May, and 08-09 May. Normal to moderate flux levels are expected on 18 Apr, 25 Apr, 29 Apr, and 06-07 May. Geomagnetic field activity is anticipated to reach G1-G2 (Minor-Moderate) storm levels on 19 Apr and 29 Apr due to -CH HSS influences, and on 07 May due to +CH HSS influences. Active conditions are expected on 18 Apr, 20 Apr, and 30 Apr-01 May in response to -CH HSS effects, and on 15 Apr, 25 Apr, and 08 May due to +CH HSS effects. Mostly quiet to unsettled conditions are expected for all other days of the period. 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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| Daily Video HMI Continuum | |
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| Daily Video 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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