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Here is this week’s space weather and geophysical report, issued 2015 Nov 16 0630 UTC.

Highlights of Solar and Geomagnetic Activity 09 – 15 November 2015

Solar activity was at very low to moderate levels over the period. The period began at moderate levels with an M3/2b flare at 09/1312 UTC from Region 2449 (S12, L=207, class/area Dao/150 on 08 Nov). Associated with the flare were Type II (957 km/s) and Type IV radio sweeps, a 670 sfu Tenflare, and a partial halo coronal mass ejection (CME). Originally, the CME was thought to have a partial Earth-directed component; however, there was no arrival apparent in ACE/SWEPAM data. Low levels were observed on 10 and 13 November due to low level C-flare activity from Regions 2443 (N07, L=316, class/area Fkc/650 on 01 Nov) and 2452 (S08, L=169, class/area Axx/010 on 11 Nov). Late on 15 November, two filament eruptions occurred in the SW quadrant. The first was an approximate 21 degree filament eruption centered near S11W17 that was observed lifting off around 15/2114 UTC in SDO/AIA 304 imagery. The second was an approximate 19 degree filament eruption centered near S26W24 observed lifting off around 16/0114 UTC. Analysis was ongoing for these two events, however given their location and initial trajectory, an Earth-directed component is probable.

An enhancement (below S1-Minor threshold) of the greater than 10 MeV proton flux occurred at 09/2130 UTC associated with the M3 flare. Particle flux measurements reached a maximum of 3.7 pfu 10/0020 UTC before declining to background levels by early on 11 November.

The greater than 2 MeV electron flux at geosynchronous orbit was at high to very high levels over the period. Very high levels occurred on 11 and 13 November with maximum flux levels of 59,508 pfu at 11/1915 UTC and 88,813 pfu at 13/1355 UTC, respectively.

Geomagnetic field activity ranged from quiet to major storm levels. The period began under the influence of a prolonged negative Bz component followed by a solar sector boundary crossing mid-day on 09 November. Shortly after, a co-rotating interaction region preceding a positive polarity coronal hole high speed stream (CH HSS) became geoeffective starting in the latter half of 09 November. Total field rose briefly to 12 nT with solar wind speeds increasing to the 650-750 km/s range. Solar wind continued to be enhanced through 12 November as CH HSS effects declined. The geomagnetic field responded with unsettled to (G1-minor) minor storm levels on 09 November, active to (G2-moderate) major storm levels on 10 November, and quiet to minor storm levels on 11 November. Quiet levels were observed on 12 November. By 13 November, another positive polarity CH HSS became geoeffective causing total field to initially rise to 10 nT with solar wind speeds in the upper 400 km/s range. Total field remained slightly agitated from 14-15 November with total field ranging from 5-9 nT. As a result, quiet to active levels were observed on 13 November, with quiet to unsettled levels on 14-15 November.

Forecast of Solar and Geomagnetic Activity 16 November – 12 December 2015

Solar activity is expected to be at very low to low levels with a chance for M-class (R1-R2, minor-moderate) flares from 22 November through 05 December with the return of old Region 2443 (N07, L=316).

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 from 16-18 November and again from 01-12 December due to recurrent CH HSS influence. Normal to moderate levels are expected from 19-30 November.

Geomagnetic field activity is expected to be at unsettled to active levels from 16-19 November due to prolonged southward Bz as well as a negative polarity CH HSS on 18-19 November. Multiple recurrent positive polarity CH HSSs are expected to influence the geomagnetic field from 30 November-02 December, 05-08 December, and 10-12 December causing unsettled to active levels with (G1-minor) storm periods likely on 30 November-01 December, and 06-08 December.

The eruptive filaments on 15-16 November are not in the present forecast as we are waiting on further imagery to model these events.

Don’t forget to visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com/

Live Aurora mapping is at http://aurora.sunspotwatch.com/

If you are on Twitter, please follow these two users: + https://Twitter.com/NW7US + https://Twitter.com/hfradiospacewx

Get the space weather and radio propagation self-study course, today. visit http://SunSpotWatch.com/swc for the latest sale and for more information!

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Here is this week’s space weather and geophysical report, issued 2015 Nov 09 0211 UTC.

Highlights of Solar and Geomagnetic Activity 02 – 08 November 2015

Solar activity was at very low to moderate levels. The summary period began with numerous weak to mid-level C-class flares from Regions 2443 (N07, L=316, class/area Fkc/650 on 01 Nov) and 2445 (N15, L=026, class/area Dac/240 on 02 Nov) observed on 02-03 November. Activity increased to moderate levels (R1-Minor) on 04 November. At 04/0326 UTC, Region 2445 produced an M1/1n flare with an associated Type II radio sweep (790 km/s estimated shock velocity). In addition, discrete frequency bursts of 56,000 sfu and 41,000 sfu were observed on 245 MHz and 410 MHz, respectively. Region 2445 also prodcued an M2/1n flare at 04/1203 UTC with an associated Type II sweep (1033 km/s estimated shock velocity). Shortly afterward, Region 2443 produced an M3/2b flare with associated Type II (955 km/s estimated shock velocity) and Type IV sweeps. This event also prodcued an associated partial-halo coronal mass ejection (CME), first observed in LASCO C2 imagery at 04/1436 UTC.

By 05 November, activity levels declined to very low levels. Levels increased to low on 06-07 November with weak to mid-level C-class activity observed from Regions 2446 (N15, L-349, class/area Cro/020 on 01 Nov), 2448 (N06, L=234, class/area Dao/140 on 06 Nov), 2449 (S12, L=209, class/area Dao/150 on 07 Nov) and 2450 (S23, L=200, class/area Bxo/010 on 07 Nov).

No proton events were observed at geosynchronous orbit.

The greater than 2 MeV electron flux at geosynchronous orbit was at normal levels on 02-03 November and high levels on 04-07 November due to enhanced solar wind speeds.

Geomagnetic field activity was at quiet to major storm levels. The summary period began with quiet to unsettled levels on 02 November. Solar wind speeds, measured at the ACE spacecraft, were weak at about 300 km/s. Field activity picked up to unsettled to minor storm levels (G1-Minor) on 03-04 November due to effects from an equatorial, positive polarity coronal hole high speed stream (CH HSS). Wind parameters observed a rapid increase in winds speeds to an average of about 675 km/s with a peak of near 770 km/s early on 04 November. Total field (Bt) increased to peak at 34 nT about 03/0700 UTC while the Bz component reached a maximum southward extent of -24 nT at 03/0620 UTC. Activity levels decreased to quiet to active on 05 November through early on 06 November as effects from the CH HSS waned. Quiet levels were observed from 06/0300-1800 UTC. During this time frame, wind speeds decreased to near 475 km/s while Bt and Bz relaxed to nominal levels.

On 06/1800-2400 UTC, field activity increased to active levels and further increased to minor to major storm levels (G1-G2 / Minor-Moderate) for the first half of 07 November. This increase in activity was attributed to the arrival of the 04 November CME. Wind speeds increased to 719 km/s at 07/0257 UTC, Bt increased to 20 nT late on 06 November and the Bz component varied between +18 nT to -16 nT. The last half of 07 November through the first half of 08 November saw field conditions relax to quiet levels. Wind speeds declined to about 425 km/s while Bt and Bz relaxed to nominal levels. By midday on the 8th, wind parameters indicated the likely onset of a co-rotating interaction region in advance of a recurrent positive polarity CH HSS. Wind speeds peaked to near 550 km/s late on the 8th while Bt reached 10 nT and Bz was mostly southward to -6 nT.

Forecast of Solar and Geomagnetic Activity 09 November – 05 December 2015

Solar activity is expected to be at predominately low levels with a chance for moderate levels (R1-R2 / Minor-Moderate) through the outlook period. Regions 2443 and 2449 , coupled with the return of old Region 2437 (S18, L=098) on 12 November, are the regions most likely to produce M-class activity.

No proton events are expected at geosynchronous orbit in the absence of any significant flare activity.

The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at moderate to high levels on 09-16 November and again on 01-05 December due to an enhanced solar wind enviroment as recurrent CH HSSs become geoeffective. Normal to moderate levels are expected on 10-30 November.

Geomagnetic field activity is expected to be at unsettled to active levels on 09-11 November. Minor storm levels (G1-Minor) are expected on 09 November as a recurrent, positive polarity CH HSS impacts Earth. Unsettled to active levels are expected on 16-17 November due to extended periods of southward Bz. Unsettled to active levels are expected on 30 November – 02 December and again on 05 December, with minor storm levels likely on 30 November and 01 December. This activity is due to recurrent positive polarity CH HSSs. Quiet to unsettled levels are expected for 12-15 and 18-29 November.

Don’t forget to visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com/

Live Aurora mapping is at http://aurora.sunspotwatch.com/

If you are on Twitter, please follow these two users: + https://Twitter.com/NW7US + https://Twitter.com/hfradiospacewx

Get the space weather and radio propagation self-study course, today. visit http://SunSpotWatch.com/swc for the latest sale and for more information!

Check out the stunning view of our Sun in action, as seen during the last five years with the Solar Dynamics Observatory (SDO): https://www.youtube.com/watch?v=zXN-MdoGM9g

We’re on Facebook: http://NW7US.us/swhfr

Here is this week’s space weather and geophysical report, issued 2015 Nov 02 0132 UTC.

Highlights of Solar and Geomagnetic Activity 26 October – 01 November 2015

Solar activity was at low levels on 26-30 October and 01 November with numerous C-class events, primarily observed from Region 2443 (N07, L=316, class/area Fkc/650 on 01 Nov). An isolated M1/Sf (R1-Minor) flare was observed on 31 October at 1752 UTC from Region 2443. On 29 October, Type II (estimated 972 km/s shock velocity) and Type IV radio emissions were detected at 0219 UTC and 0230 UTC, respectively. SOHO/LASCO C2 imagery observed a non Earth-directed CME off the SW limb at 29/0236 UTC, believed to be associated with the Type II and Type IV radio activity.

A short-lived greater than 10 MeV at greater than or equal to 10 pfu proton event was observed on 29 October. The event began at 29/0550 UTC, reached a maximum of 23 pfu at 29/1000 UTC and ended at 29/1700 UTC. Coincident with this event was a short-lived greater than 100 MeV at greater than or equal to 1 pfu event. This event began at 29/0435 UTC, reached a maximum of 2 pfu at 29/0610 UTC and ended at 29/0930 UTC. Both of these events were most likely associated with activity just beyond the SW limb described above.

The greater than 2 MeV electron flux at geosynchronous orbit was at normal levels on 26, 30-31 October and 01 November with moderate levels obsered on 27-29 October.

Geomagnetic field activity was predominately at quiet levels with some unsettled periods observed on 30-31 October and 01 November. Solar wind parameters reflected a mostly nominal environment with wind speeds ranging from a high of 483 km/s at 26/1145 UTC to a low of 287 km/s at 29/0746 UTC. Total field strength ranged from 1-10 nT while the Bz component did not vary much beyond +/- 7 nT. Phi angle was in a positive (away) orientation from the beginning of the period through early on 28 October when a switch to a negative (towards) sector was observed. Phi switched back to a positive sector at about 29/1915 UTC and remained so through the balance of the summary period.

Forecast of Solar and Geomagnetic Activity 02 November – 28 November 2015

Solar activity is expected to be at predominately low levels with moderate levels (R1-R2.Minor-Moderate) likely through the outlook period. Region 2443, through 10 November, and the return of old Regions 2434 (S09, L=165) on 07 November and 2437 (S18, L=098) on 12 November are likely to produce M-class activity through the outlook period.

No proton events are expected at geosynchronous orbit in the absence of any siginifcant flare activity.

The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at high to very high levels on 02-13 November due to an enhanced solar wind environment as a recurrent, trans-equatorial coronal hole high speed stream (CH HSS) becomes geoeffective. Normal to moderate levels are expected from 14-28 November.

Geomagnetic field activity is expected to began the period at G1 (Minor), G2 (Moderate) and G3 (Strong) levels on 02 November followed by G1 to G2 levels on 03 November as a recurrent, trans-equatorial CH HSS impacts Earth. Unsettled to active levels are expected on 04-06 November as CH HSS effects wane. Unsettled to active levels are expected on 13-14 November and 16-17 November due to periods of southward Bz and a weak positive polarity CH HSS. Quiet to unsettled levels are expected for the remainder of the outlook period.

Don’t forget to visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com/

Live Aurora mapping is at http://aurora.sunspotwatch.com/

If you are on Twitter, please follow these two users: + https://Twitter.com/NW7US + https://Twitter.com/hfradiospacewx

Get the space weather and radio propagation self-study course, today. visit http://SunSpotWatch.com/swc for the latest sale and for more information!

Check out the stunning view of our Sun in action, as seen during the last five years with the Solar Dynamics Observatory (SDO): https://www.youtube.com/watch?v=zXN-MdoGM9g

We’re on Facebook: http://NW7US.us/swhfr

Space Weather. The Sun-Earth Connection. Ionospheric radio propagation. Solar storms. Coronal Mass Ejections (CMEs). Solar flares and radio blackouts. All of these topics are interrelated for the amateur radio operator, especially when the activity involves the shortwave, or high-frequency, radiowave spectrum.

Learning about space weather and radio signal propagation via the ionosphere aids you in gaining a competitive edge in radio DX contests. Want to forecast the radio propagation for the next weekend so you know whether or not you should attend to the Honey-do list, or declare a radio day?

In the last ten years, amazing technological advances have been made in heliophysics research and solar observation. These advances have catapulted the amateur radio hobbyist into a new era in which computer power and easy access to huge amounts of data assist in learning about, observing, and forecasting space weather and to gain an understanding of how space weather impacts shortwave radio propagation, aurora propagation, and so on.

I hope to start “blogging” here about space weather and the propagation of radio waves, as time allows. I hope this finds a place in your journey of exploring the Sun-Earth connection and the science of radio communication.

With that in mind, I’d like to share some pretty cool science. Even though the video material in this article are from 2010, they provide a view of our Sun with the stunning solar tsunami event:

On August 1, 2010, the entire Earth-facing side of the sun erupted in a tumult of activity. There was a C3-class solar flare, a solar tsunami, multiple plasma-filled filaments of magnetism lifting off the stellar surface, large-scale shaking of the solar corona, radio bursts, a coronal mass ejection and more!

At approximately 0855 UTC on August 1, 2010, a C3.2 magnitude soft X-ray flare erupted from NOAA Active Sunspot Region 11092 (we typically shorten this by dropping the first digit: NOAA AR 1092).

At nearly the same time, a massive filament eruption occurred. Prior to the filament’s eruption, NASA’s Solar Dynamics Observatory (SDO) AIA instruments revealed an enormous plasma filament stretching across the sun’s northern hemisphere. When the solar shock wave triggered by the C3.2-class X-ray explosion plowed through this filament, it caused the filament to erupt, sending out a huge plasma cloud.

In this movie, taken by SDO AIA at several different Extreme Ultra Violet (EUV) wavelengths such as the 304- and 171-Angstrom wavelengths, a cooler shock wave can be seen emerging from the origin of the X-ray flare and sweeping across the Sun’s northern hemisphere into the filament field. The impact of this shock wave may propelled the filament into space.

This movie seems to support this analysis: Despite the approximately 400,000 kilometer distance between the flare and the filament eruption, they appear to erupt together. How can this be? Most likely they’re connected by long-range magnetic fields (remember: we cannot see these magnetic field lines unless there is plasma riding these fields).

In the following video clip, taken by SDO AIA at the 304-Angstrom wavelength, a cooler shock wave can be seen emerging from the origin of the X-ray flare and sweeping across the sun’s northern hemisphere into the filament field. The impact of this shock wave propelled the filament into space. This is in black and white because we’re capturing the EUV at the 304-Angstrom wavelength, which we cannot see. SDO does add artificial color to these images, but the raw footage is in this non-colorized view.

The followling video shows this event in the 171-Angstrom wavelength, and highlights more of the flare event:

The following related video shows the “resulting” shock wave several days later. Note that this did NOT result in anything more than a bit of aurora seen by folks living in high-latitude areas (like Norway, for instance).

This fourth video sequence (of the five in the first video shown in this article) shows a simulation model of real-time passage of the solar wind. In this segment, the plasma cloud that was ejected from this solar tsunami event is seen in the data and simulation, passing by Earth and impacting the magnetosphere. This results in the disturbance of the geomagnetic field, triggering aurora and ionospheric depressions that degrade shortwave radio wave propagation.

At about 2/3rd of the way through, UTC time stamp 1651 UTC, the shock wave hits the magnetosphere.

This is a simulation derived from satellite data of the interaction between the solar wind, the earth’s magnetosphere, and earth’s ionosphere. This triggered aurora on August 4, 2010, as the geomagnetic field became stormy (Kp was at or above 5).

While this is an amazing event, a complex series of eruptions involving most of the visible surface of the sun occurred, ejecting plasma toward the Earth, the energy that was transferred by the plasma mass that was ejected by the two eruptions (first, the slower-moving coronal mass ejection originating in the C-class X-ray flare at sunspot region 1092, and, second, the faster-moving plasma ejection originating in the filament eruption) was “moderate.” This event, especially in relationship with the Earth through the Sun-Earth connection, was rather low in energy. It did not result in any news-worthy events on Earth–no laptops were fried, no power grids failed, and the geomagnetic activity level was only moderate, with limited degradation observed on the shortwave radio spectrum.

This “Solar Tsunami” is actually categorized as a “Moreton wave”, the chromospheric signature of a large-scale solar coronal shock wave. As can be seen in this video, they are generated by solar flares. They are named for American astronomer, Gail Moreton, an observer at the Lockheed Solar Observatory in Burbank who spotted them in 1959. He discovered them in time-lapse photography of the chromosphere in the light of the Balmer alpha transition.

Moreton waves propagate at a speed of 250 to 1500 km/s (kilometers per second). A solar scientist, Yutaka Uchida, has interpreted Moreton waves as MHD fast-mode shock waves propagating in the corona. He links them to type II radio bursts, which are radio-wave discharges created when coronal mass ejections accelerate shocks.

I will be posting more of these kinds of posts, some of them explaining the interaction between space weather and the propagation of radio signals.

For live space weather and radio propagation, visit http://SunSpotWatch.com/. Be sure to subscribe to my YouTube channel: https://YouTube.com/NW7US.

The fourth video segment is used by written permission, granted to NW7US by NICT. The movie is copyright@NICT, Japan. The rest of the video is courtesy of SDO/AIA and NASA. Music is courtesy of YouTube, from their free-to-use music library. Video copyright, 2015, by Tomas Hood / NW7US. All rights reserved.

Here is this week’s space weather and geophysical report, issued 2015 Aug 03 0155 UTC.

Highlights of Solar and Geomagnetic Activity 27 July – 02 August 2015

Solar activity was dominated by B-class flare activity (very low levels) throughout the majority of the summary period, however, Region 2390 (S17, L=199, class/area=Dai/170 on 27 Jul) produced a single C1 flare (low levels) at 01/2005 UTC, which was the largest event of the period. No Earth-directed coronal mass ejections (CMEs) were observed during the summary period.

No proton events were observed at geosynchronous orbit.

The greater than 2 MeV electron flux at geosynchronous orbit was at normal levels on 31 Aug with moderate levels observed throughout the remainder of the summary period.

Geomagnetic field activity reached active levels on 27, 30-31 Jul and 02 Aug in response to an enhanced solar wind environment caused by the influence of multiple weak coronal hole high speed streams (CH HSSs). Geomagnetic field activity remained at quiet to unsettled levels throughout the remainder of the summary period.

Forecast of Solar and Geomagnetic Activity 03 August – 29 August 2015

Solar activity is expected to be at very low (B-class flare activity) to low levels (C-class flare activity) throughout the outlook period.

No proton events are expected at geosynchronous orbit.

The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at moderate levels on 07-08, 17-21, 23, and 26-29 Aug in response to enhanced geomagnetic field activity cause by the influence of multiple recurrent coronal hole high speed streams (CH HSSs). High electron flux levels are expected for the remainder of the outlook period.

Geomagnetic field activity is expected to reach G1 (Minor) geomagnetic storm levels on 28 Aug with active levels expected on 06-07, 17, 20, 26-27, and 29 Aug, all due to the influence of multiple recurrent CH HSSs. The geomagnetic field is expected to be at quiet to unsettled levels throughout the remainder of the outlook period.

Don’t forget to visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com/

Live Aurora mapping is at http://aurora.sunspotwatch.com/

If you are on Twitter, please follow these two users: + https://Twitter.com/NW7US + https://Twitter.com/hfradiospacewx

Get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

Check out the stunning view of our Sun in action, as seen during the last five years with the Solar Dynamics Observatory (SDO): https://www.youtube.com/watch?v=zXN-MdoGM9g

We’re on Facebook: http://NW7US.us/swhfr

Watch this video on a large screen. (It is HD). Discuss. Share.

This video features stunning clips of the Sun, captured by SDO from each of the five years since SDO’s deployment in 2010. In this movie, watch giant clouds of solar material hurled out into space, the dance of giant loops hovering in the corona, and huge sunspots growing and shrinking on the Sun’s surface.

April 21, 2015 marks the five-year anniversary of the Solar Dynamics Observatory (SDO) First Light press conference, where NASA revealed the first images taken by the spacecraft. Since then, SDO has captured amazingly stunning super-high-definition images in multiple wavelengths, revealing new science, and captivating views.

February 11, 2015 marks five years in space for NASA’s Solar Dynamics Observatory, which provides incredibly detailed images of the whole Sun 24 hours a day. February 11, 2010, was the day on which NASA launched an unprecedented solar observatory into space. The Solar Dynamics Observatory (SDO) flew up on an Atlas V rocket, carrying instruments that scientists hoped would revolutionize observations of the Sun.

Capturing an image more than once per second, SDO has provided an unprecedentedly clear picture of how massive explosions on the Sun grow and erupt. The imagery is also captivating, allowing one to watch the constant ballet of solar material through the sun’s atmosphere, the corona.

The imagery in this “highlight reel” provide us with examples of the kind of data that SDO provides to scientists. By watching the sun in different wavelengths (and therefore different temperatures, each “seen” at a particular wavelength that is invisible to the unaided eye) scientists can watch how material courses through the corona. SDO captures images of the Sun in 10 different wavelengths, each of which helps highlight a different temperature of solar material. Different temperatures can, in turn, show specific structures on the Sun such as solar flares or coronal loops, and help reveal what causes eruptions on the Sun, what heats the Sun’s atmosphere up to 1,000 times hotter than its surface, and why the Sun’s magnetic fields are constantly on the move.

Coronal loops are streams of solar material traveling up and down looping magnetic field lines). Solar flares are bursts of light, energy and X-rays. They can occur by themselves or can be accompanied by what’s called a coronal mass ejection, or CME, in which a giant cloud of solar material erupts off the Sun, achieves escape velocity and heads off into space.

This movie shows examples of x-ray flares, coronal mass ejections, prominence eruptions when masses of solar material leap off the Sun, much like CMEs. The movie also shows sunspot groups on the solar surface. One of these sunspot groups, a magnetically strong and complex region appearing in mid-January 2014, was one of the largest in nine years as well as a torrent of intense solar flares. In this case, the Sun produced only flares and no CMEs, which, while not unheard of, is somewhat unusual for flares of that size. Scientists are looking at that data now to see if they can determine what circumstances might have led to flares eruptions alone.

Scientists study these images to better understand the complex electromagnetic system causing the constant movement on the sun, which can ultimately have an effect closer to Earth, too: Flares and another type of solar explosion called coronal mass ejections can sometimes disrupt technology in space as well as on Earth (disrupting shortwave communication, stressing power grids, and more). Additionally, studying our closest star is one way of learning about other stars in the galaxy.

Goddard built, operates and manages the SDO spacecraft for NASA’s Science Mission Directorate in Washington, D.C. SDO is the first mission of NASA’s Living with a Star Program. The program’s goal is to develop the scientific understanding necessary to address those aspects of the sun-Earth system that directly affect our lives and society.

https://www.youtube.com/watch?v=zXN-MdoGM9g

Watch this amazing explosion on the Sun. From sunspot complex 1226-1227 comes an X-ray Flare peaking at a magnitude of M2.5 at 0640 UTC on 7 June, 2011.

Source: https://www.youtube.com/watch?v=KQMrRu8BWDo

This X-ray flare hurled a massive coronal mass ejection (CME) toward the Earth. This not-squarely Earth-directed CME is moving at 1400 km/s according to NASA models. The CME did not deliver even a noticeable glancing blow to Earth’s magnetic field late June 8th or June 9th.

What can be seen clearly in this movie is one of the most spectacular prominence eruptions ever observed. In fact, one could call it a “prominence explosion”. The prominence material expanded to a volume some 75 times as big across as the earth!

This X-ray flare also triggered an S1-level solar radiation storm, causing a long-lasting polar cap absorption (PCA) event. A polar cap absorption (PCA) event affects the propagation of a shortwave radio signal as it makes its way over the polar regions. In short, radio communications on lower shortwave radio frequencies become more difficult, as those radio signals are absorbed by the ionosphere (in the D-region) over the polar regions.

What does this mean in real-world communications? Trans-polar airline pilots may find it more difficult to communicate with regional air traffic control, shortwave radio listeners who want to hear a broadcast from a country by receiving a transmission from a country by way of a transmission beamed over the pole (like, from Europe into the USA via the North Pole), or other such communications, will find those signals all but gone. The stronger the PCA event, the higher the frequencies absorbed over the polar regions, with the greatest absorption occurring at the lower frequencies.

This movie spans the period of time from 0300 UTC through 1556 UTC, and is composed of the 171-Angstrom, 304-Angstrom, and 335-Angstrom wavelength views as captured by the filters of the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA). In this movie, the AIA instruments capture the Sun’s extreme ultraviolet light and reveal a very large eruption of cool gas. It is somewhat unique because at many places in the eruption there seems to be even cooler material–at temperatures less than 80,000 K.

The following is a linked video that is part of this event: http://www.youtube.com/watch?v=L4CsjcUGoaw

Watch as we zoom out to see a total view of the June 7, 2011 moderately-powerful X-ray Flare and Prominence Eruption. This movie will give you a full perspective of the immense size of this prominence eruption as it spews out away from the Sun.

The X-ray Flare peaked at a moderate magnitude of M2.5 at 0640 UTC, but unleashed a huge prominence eruption. The massive cloud of plasma was ejected out into interplanetary space, but missed the Earth. This movie stars with a “close-up” view by the Solar Dynamics Observatory at a combined wavelength view at 94 and 304 Angstroms. Then, the movie views the event further back through the eyes of the COR1 spacecraft (with the SDO AIA 304 image superimposed in the middle). Next, we zoom out to the COR2 spacecraft and superimpose the COR1 and SDO views. Then, we zoom further back to the H1 view… and finally look again at the event close-up.

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Source: SDO AIA NASA SOHO