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| Warnings and Alerts | ||
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Issue Time: 2026 Jun 14 1328 UTC
CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu Continuation of Serial Number: 3699 Begin Time: 2026 Jun 13 1332 UTC Yesterday Maximum 2MeV Flux: 1520 pfu Space Weather Scales |
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| Current Condition and Alerts | ||
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Issued: 2026 Jun 14 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 13 June follow. Solar flux 122 and estimated planetary A-index 13. The estimated planetary K-index at 1200 UTC on 14 June was 2.00. 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 |
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| Forecast Discussion | ||
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Issued: 2026 Jun 14 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity continued at low levels. Region 4465 (N08W04, Cao/beta) developed a few rudimentary leader spots, and new Region 4468 (N10E46, Cro/beta) was numbered this period. The remaining regions were either stable or in decay. The strongest flare of the period was a C2.5/Sf at 13/1309 UTC associated with a filament eruption near S21W73. The subsequent CME, first observed in LASCO C2 imagery off the SW at 13/1326 UTC, is expected to miss Earth. .Forecast... Solar activity is expected to remain at low levels through 16 Jun, with a slight chance for M-class (R1-R2/Minor-Moderate) flares. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached high levels, with a peak flux of 1,519 pfu. The greater than 10 MeV proton flux remained at background levels. .Forecast... The greater than 2 MeV electron flux is likely to reach high levels on 14-16 Jun. The greater than 10 MeV proton flux is expected to continue at background levels through 16 Jun. Solar Wind .24 hr Summary... Solar wind parameters reflected the continued influence of a negative polarity CH HSS, with some lingering CME enhancements early in the period. Total field strength reached 7 nT, and the Bz component varied between +/-5 nT. Solar wind speeds gradually decreased from a peak near 625 km/s early in the period to a low of around 475 km/s by the end of the period. .Forecast... The solar wind environment is expected to remain mildly enhanced over 14-15 Jun under continued, but waning -CH HSS influences. An additional enhancement is likely on 16 Jun due to the anticipated glancing-blow arrival of a CME from 12 Jun. Geospace .24 hr Summary... The geomagnetic field was at mostly quiet to unsettled levels, with an isolated active period, under -CH HSS and CME influences. .Forecast... The geomagnetic field is expected to be at quiet to unsettled levels, with a chance for active conditions, on 14-15 Jun as -CH HSS influences slowly diminish. Periods of active conditions are likely on 16 Jun due to the anticipated glancing-blow arrival of a CME that left the Sun on 12 Jun. Space Weather Scales |
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| Three Day Forecast | ||
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Issued: 2026 Jun 14 1232 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 Jun 14-Jun 16 2026 is 3.67 (below NOAA Scale levels). NOAA Kp index breakdown Jun 14-Jun 16 2026 Jun 14 Jun 15 Jun 16 00-03UT 2.33 2.67 2.67 03-06UT 2.00 3.00 3.67 06-09UT 1.33 2.67 3.67 09-12UT 2.00 1.67 2.67 12-15UT 1.67 1.67 1.67 15-18UT 1.67 1.00 1.67 18-21UT 2.67 1.67 1.67 21-00UT 2.67 1.67 2.00 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 14-Jun 16 2026 Jun 14 Jun 15 Jun 16 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 Jun 14-Jun 16 2026 Jun 14 Jun 15 Jun 16 R1-R2 10% 10% 10% R3 or greater 1% 1% 1% Rationale: There is a slight chance for R1-R2 (Minor-Moderate) radio blackouts over 14-16 Jun. Space Weather Scales |
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| Weekly Highlights and Forecasts | ||
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Issued: 2026 Jun 08 0243 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 01 - 07 June 2026 Solar activity reached high levels on 03 Jun when Region 4455 (N14, L=88, class/area=Dki/360 on 03 Jun) produced an M9.3/Sf flare (accompanied by Type-II (253 km/s) and Type-IV sweeps, and a 360 sfu Tenflare) at 03/0136 UTC, followed by an M7.7/1b flare (accompanied by Type-II (313 km/s) and Type-IV radio sweeps, and a 540 sfu Tenflare with Castelli-U signature) at 03/0700 UTC, and finally an X1.0/1n flare (accompanied by a Type-IV sweep and a 180 sfu Tenflare) at 03/1128 UTC. The CMEs associated with the three significant flares from AR4455 on 03 Jun arrived at Earth on 05 Jun. Other activity included an M1.8/2n (accompanied by Type-II (838 km/s) and 190 sfu Tenflare) flare at 06/1401 UTC from Region 4461 (S20, L=09, class/area=Dao/70 on 02 Jun). The resulting partial-halo CME, first visible in LASCO C2 imagery at 06/1401 UTC, is anticipated to arrive at Earth around midday on 08 Jun. The greater than 10 MeV proton flux became slightly enhanced after midday on 06 Jun following the M1.8/2n flare at 06/1401 UTC from Region 4461, but remained below event levels with a peak flux of 1.0 pfu observed at 06/1940 UTC. The greater than 10 MeV proton flux gradually returned to background levels on 07 Jun. The greater than 2 MeV electron flux at geosynchronous orbit was at normal to moderate levels on 01-05 Jun, with high levels observed on 06-07 Jun. Geomagnetic field activity reached G1-G2 (Minor-Moderate) storm levels on 05 Jun, and active levels on 06 Jun, following the arrival and passage of the CMEs from 03 Jun. The shock arrival was observed beginning at around 05/0425 UTC, and in the hours following the total magnetic field strength (Bt) reached 20 nT, the Bz component reached as far southward as -17 nT, and solar wind speeds increased to a peak near 740 km/s. Quiet and quiet to unsettled levels under weak coronal hole high speed stream influences prevailed throughout the remainder of the period. Forecast of Solar and Geomagnetic Activity 08 June - 04 July 2026 Solar activity is expected to be at predominately low levels through 04 Jul, with M-class flare probabilities ranging from a chance to likely levels throughout the period. No proton events are expected at geosynchronous orbit, barring significant flare activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 09-10, 13-18 Jun and 04 Jul. Normal to moderate levels are expected to prevail throughout the remainder of the period. Geomagnetic field activity is likely to reach G1-G3 (Minor-Strong) storm levels on 08 Jun, with G1-G2 (Minor-Moderate) levels likely on 09 Jun, due to the anticipated arrival of the CME that left the Sun on 06 Jun. Periods of active conditions are likely on 23-26 Jun due to recurrent CH HSS influences. Quiet and quiet to unsettled levels are expected to prevail throughout the remainder 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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