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Today’s Sun (artificially-colored in purple) seen at the 211-angstrom wavelength (Extreme Ultraviolet, or EUV), as viewed by the Solar Dynamics Observatory (SDO), by the Atmospheric Imaging Assembly (AIA).
At this wavelength, at a wavelength not seen by the un-aided eye, we observe this full-disk AIA image through the 21.1 nm (211 A) filter. This Extreme Ultraviolet (EUV) waveband is used to monitor active regions in the solar corona.
The image is a ‘false color image’, meaning that observed data are in a range outside of what human eyes can see, so the data are digitally recast into colors that emphasize physically important features. This view is created from data gathered by the Solar Dynamics Observatory (SDO) satellite that flies above Earth’s atmosphere in an inclined geosynchronous orbit.
Emissions captured in this image come from iron (Fe), a trace element in the solar atmosphere that emits Extreme Ultraviolet (EUV) light when heated to temperatures in excess of one million deg K. In the solar corona the temperatures are so high that most chemical elements have lost many of their electrons. Some of the remaining electrons still attached to the atom emit EUV radiation in narrow wavebands or lines.
The 21.1 nm filter (also called channel or bandpass) is dominated by emissions from highly ionized iron: 13 times ionized (missing 13 electrons) iron–Fe XIV. Other ionization levels of iron also contribute. The roman numeral descriptors are consistent with spectral notation: the level of ionization for a given roman numeral is one unit larger that the actual number of missing electrons. Additionally there may be some contribution from hot thermal plasma when solar flares are present. The temperatures associated with this level of ionization is about 2 x 10^6 K.
The bright regions in this image correspond to regions of closed magnetic field loops that trap the hot, emitting plasma. Large bright regions are often called active regions. The dark regions correspond to cooler temperatures and possibly to locations where magnetic field lines open into the heliosphere, and thus, do not trap hot plasma.
With this image, we can monitor active regions.
View live data and images at http://SunSpotWatch.com
We’re on Facebook: http://NW7US.us/swhfr
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- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
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Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
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The YouTube channel: https://YouTube.com/NW7US
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The following is the weekly propagation bulletin from W1AW / ARRL (posting on 20210730 23:52 UTC):
QST de W1AW Propagation Forecast Bulletin 31 ARLP031 >From Tad Cook, K7RA Seattle, WA July 30, 2021 To all radio amateurs
SB PROP ARL ARLP031 ARLP031 Propagation de K7RA
Solar activity slowed this week. Average daily sunspot number declined to 33.9 this week (July 22 to 28) from 48.9 in last week’s report. Wednesday July 28 had no sunspots at all.
Average daily solar flux went from 81.3 to 83.
Geomagnetic indicators held steady, with average daily planetary A index at 6.4 both last week and this week. Average daily middle latitude A index went from 6.4 last week to 6.3 this week.
Predicted solar flux is 76 on July 30 and 31, then 74 on August 1, 72 on August 2 to 4, 74 on August 5 and 6, 75 on August 7 to 12, then 78, 80, 82 and 85 on August 13 to 16, 90 on August 17 and 18, 85 on August 19 and 20, 80 on August 21, 82 on August 22 to 28, 78 on August 29, and 75 on August 30 to September 8.
Predicted planetary A index is 8, 12 and 8 on July 30 through August 1, 5 on August 2 to 9, 12 and 10 on August 10 and 11, 5 on August 12 to 15, 10 and 8 on August 16 and 17, 5 on August 18 to 23, then 12, 12 and 8 on August 24 to 26, 5 on August 27 and 28, 8 on August 29, and 5 on August 30 through September 5.
F. K. Janda, OK1HH is on vacation this week hiking in the mountains of the Czech Republic, so we have forecasts from two of his associates.
‘Solar activity forecast for the period July 30 to August 05, 2021
Activity level is mostly very low X-ray background flux (1.0 to 8.0 A) in the range A5.5 to B1.5 Radio flux (10.7 cm) a fluctuation in the range 74 to 82 Events: class C (0 to 4/period), class M (0/period), class X (0/period), proton (0/period)
Relative sunspot number (Ri) in the range 0 to 55’
'Geomagnetic activity forecast for the period July 30 to August 05, 2021
Quiet on Jul 30 and 31, Aug 2 to 4 Unsettled on Jul 31, Aug 1 to 3, 5 No Active days No Minor storms No Major storms No Severe storms
Geomagnetic activity summary:
Next week, we expect at most quiet to unsettled conditions. The more unsettled events are possible about August 1 and 2, and also about Thursday, August 5.
The other days, we expect quiet to unsettled conditions generally, closer to quiet level.’
KC0V wrote:
'There was a big 2m Es opening from DN70 to the Midwest this afternoon, July 24. I was busy with some chores then happened to look at DXMaps and the APRS VHF propagation map and noticed a large Es cloud located over eastern NE/western IA and another located over SE KS. I quickly tuned into 2m FT8 144.174. Signals were very strong, with +21 db the best report I sent and +29 the best report I received. My QSOs, beginning at 2216z and ending at 2235 UTC were as follows:
WA9DU EM69 WB8ART EM79 AA9JS EN51 KC9IKB EM69 KA9CFD EN40 WA4CQG EM72 KX9X EN50 NY1V EM69 KM8V EN91 K2DRH EN41 AG4V EM55 KO9A EN52 WB8JCW EN80
Then followed 26 minutes of a mixture of single decodes, total quiet, meteor bursts, but no QSOs. Then at 2301 UTC:
K9YK EN60
And then it was over. I don’t know when the opening began since it was well and truly in progress when I got to the radio, but it was an amazing 20 minutes or so.
Unfortunately I was unable to complete with W3IP in FM19, which would have been the longest distance QSO of the opening for me. We heard each other over several sequences but were unable to finish the exchange.
My station: Kenwood TS-2000, Beko HLV-1000 running at 750W, 10 element LFA (by G0KSC) at 35 feet.
73 - Jan, KC0V’
For more information concerning shortwave radio propagation, see http://www.arrl.org/propagation and the ARRL Technical Information Service at http://arrl.org/propagation-of-rf-signals. For an explanation of numbers used in this bulletin, see http://arrl.org/the-sun-the-earth-the-ionosphere.
An archive of past propagation bulletins is at http://arrl.org/w1aw-bulletins-archive-propagation. More good information and tutorials on propagation are at http://k9la.us/.
Instructions for starting or ending email distribution of ARRL bulletins are at http://arrl.org/bulletins .
Sunspot numbers for July 22 through 28, 2021 were 77, 46, 35, 24, 25, 25, and 0, with a mean of 33.1. 10.7 cm flux was 89, 87.4 83.9, 81.6, 80.8, 79.6, and 78.8, with a mean of 83. Estimated planetary A indices were 11, 4, 4, 3, 4, 6, and 13, with a mean of 6.4. Middle latitude A index was 9, 3, 5, 5, 3, 6, and 13, with a mean of 6.3.
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https://groups.io/g/propagation-and-space-weather
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Links of interest:
+ Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
+ https://Twitter.com/NW7US
+ https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel:
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Today’s Sun (artificially-colored in red) seen at the 304-angstrom wavelength (Extreme Ultraviolet, or EUV), as viewed by the Solar Dynamics Observatory (SDO), by the Atmospheric Imaging Assembly (AIA).
At this wavelength, at a wavelength not seen by the un-aided eye, we can see the Sun through the 30.4 nm (304 A) filter. This Extreme Ultraviolet (EUV) waveband is used to monitor the chromosphere and lower transition region. It is useful to see plasma and filament activity, including filamet eruptions and coronal mass ejections (CMEs).
The image is a ‘false color image’, meaning that observed data are in a range outside of what human eyes can see, so the data are digitally recast into colors that emphasize physically important features. This view is created from data gathered by the Solar Dynamics Observatory (SDO) satellite that flies above Earth’s atmosphere in an inclined geosynchronous orbit.
Emissions captured in this image come from helium (He), the second most abundant element in the solar atmosphere. Singly ionized Helium (He II) emits Extreme Ultraviolet (EUV) light when heated to temperatures of ~70,000 deg K. In the upper solar atmosphere the temperatures are so high that most chemical elements have lost many of their electrons. The remaining electron, which is still attached to the atom, emits EUV radiation in narrow wavebands or lines when it is in an excited state.
The 30.4 nm filter (also called channel or bandpass) is dominated by emissions from singly (once) ionized helium which has missing 1 electron–He II. The roman numeral descriptor is consistent with spectral notation: the level of ionization for a given roman numeral is one unit larger that the actual number of missing electrons. The temperatures associated with this level of ionization is range from 6 x 10^4 K to 8 x 10^4 K.
The bright regions in this image correspond to regions of closed magnetic field loops that trap the hot, emitting plasma. Large bright regions are often called active regions. The dark regions correspond to cooler temperatures and possibly to locations where magnetic field lines open into the heliosphere, and thus, do not trap hot plasma.
View live data and images at http://SunSpotWatch.com
We’re on Facebook: http://NW7US.us/swhfr
Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
Links of interest:
- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
- https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel: https://YouTube.com/NW7US
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Here is the current forecast discussion on space weather and geophysical activity, issued 2021 Jul 30 1230 UTC.
Solar Activity
24 hr Summary: Solar activity was very low as the visible solar disk remained spotless. No Earth-directed CMEs were detected in available coronagraph imagery.
Forecast: Very low solar activity is expected to continue 30 Jul-1 Aug.
Energetic Particle
24 hr Summary: The greater than 2 MeV electron flux was normal to moderate and the greater than 10 MeV proton flux maintained background levels.
Forecast: The greater than 2 MeV electron flux is expected to be normal to moderate, with a chance for high levels, 30 Jul-1 Aug due to CH HSS influences. The greater than 10 MeV proton flux is expected to continue at background levels.
Solar Wind
24 hr Summary: Solar wind parameters remained indicative of CH HSS influences. Total IMF strength averaged 3-6 nT with primarily weak southward deviations of the Bz component. Solar wind speed ranged mainly ~435-535 km/s and the phi angle was predominantly in the positive solar sector.
Forecast: Elevated solar wind speed is expected to continue, but slowly wane through 30 Jul as influences of a positive polarity CH HSS weaken, while possible weak connections with an isolated, negative polarity CH HSS could occur. Enhancements in solar wind conditions are anticipated again 31 Jul and 1 Aug due to waning negative polarity CH HSS effects, followed by possible connection to a southward extension of the north polar, positive polarity CH HSS. Additionally, several CMEs (from 25, 27, and 28 Jul) are anticipated to pass close to Earth 30-31 Jul and 1 Aug. While models for these transients indicated mostly close proximity or weak flanking influences, it is probable these nearby passing transients could cause weak disturbances in the solar wind field all three days.
Geospace
24 hr Summary: The geomagnetic field was quiet.
Forecast: The geomagnetic field is expected to be quiet to unsettled on 30-31 Jul, and quiet to active on 1 Aug. These varying responses are anticipated reactions to CH HSS effects and possible additional influences from the close proximity of passing transients.
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
Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
Links of interest:
- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
- https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel: https://YouTube.com/NW7US
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We’re on Facebook: http://NW7US.us/swhfr
Daily solar report: Current Sunspot Cycle 24 Activity and Space Weather
Sunspot count: Sun Spots: 0 as of 07/29/2021 10.7-cm Radio Flux: 76 SFU (SFU=Solar Flux Units) Estimated Planetary A-index (Ap): 8 | K-index (Kp):
Solar Wind: 411 km/s at 4.0 protons/cm3, Bz is 0.0 nT (May 05, 2021 at 0435 UT)
X-ray Solar Flares: 6h hi [B1.1][1925Z 07/29] 24h hi [B1.1][1925Z 07/29]
Background X-ray Level, Last Six Days
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Global HF Propagation Conditions for 0400Z on 05 May, 2021 High Latitude: Normal Middle Latitude: Normal Low Latitude: Normal
Geomagnetic Latitude Ranges: High: 60-90 degrees, Middle: 20-60 degrees, Low: 0-20 degrees
For live data and images, visit http://SunSpotWatch.com
This report has been prepared by your space weather and radio propagation reporter, Tomas ( amateur radio operator, NW7US, http://NW7US.us )
We’re on Facebook: http://NW7US.us/swhfr
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Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
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Links of interest:
+ Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
+ https://Twitter.com/NW7US
+ https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel:
https://YouTube.com/NW7US
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Today’s Sun, seen through a filter of ‘visible’ light (remember: NEVER look directly at the Sun!), as viewed by the Solar Dynamics Observatory (SDO), by the Helioseismic Magnetic Imager (HMI). This image is known as a 'continuum’ image; a continuum image is formed by filtering portions of the visible light part of the spectrum. The SDO HMI is designed to study oscillations and the magnetic field at the solar surface, or photosphere.
The continuum images allow us to track the evolution of sunspots. These images are important as they allow us to better understand the dynamic nature of the solar atmosphere.
Be sure to subscribe to our space weather and propagation email group, on Groups.io
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Spread the word!
Links of interest:
- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
- https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel: https://YouTube.com/NW7US
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Today’s graph, plotting the SESC sunspot number, the 10.7cm Radio Flux, and the Estimated Planetary A Index, for the last 30 days.
The numbers are:
Date | Sunspots | 10.7-cm Flux | Ap ========================================== 2021/07/29 | 0 | 76 | 8For complete live data and images visit http://SunSpotWatch.com
2021/07/28 | 0 | 79 | 13
2021/07/27 | 25 | 80 | 6
2021/07/26 | 25 | 81 | 4
2021/07/25 | 24 | 82 | 3
2021/07/24 | 35 | 84 | 4
2021/07/23 | 46 | 87 | 4
2021/07/22 | 77 | 89 | 11
2021/07/21 | 86 | 94 | 6
2021/07/20 | 59 | 87 | 10
2021/07/19 | 45 | 83 | 7
2021/07/18 | 42 | 80 | 4
2021/07/17 | 53 | 77 | 4
2021/07/16 | 35 | 75 | 4
2021/07/15 | 22 | 74 | 10
2021/07/14 | 23 | 72 | 14
2021/07/13 | 11 | 72 | 5
2021/07/12 | 22 | 72 | 7
2021/07/11 | 23 | 74 | 4
2021/07/10 | 24 | 74 | 6
2021/07/09 | 23 | 74 | 5
2021/07/08 | 23 | 73 | 5
2021/07/07 | 25 | 76 | 6
2021/07/06 | 52 | 83 | 8
2021/07/05 | 43 | 89 | 7
2021/07/04 | 60 | 91 | 3
2021/07/03 | 81 | 94 | 4
2021/07/02 | 72 | 95 | 5
2021/07/01 | 56 | 94 | 7
We’re on Facebook: http://NW7US.us/swhfr
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Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
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Links of interest:
+ Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
+ https://Twitter.com/NW7US
+ https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel:
https://YouTube.com/NW7US
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Did you know? Here’s a space weather and radio propagation educational tidbit – from http://SunSpotWatch.com – at 14:00 UTC on 2021-07-30:
A geomagnetic storm is defined by changes in the “Dst” (or, “DST”), which stands for the “Disturbance, storm time” index. A geomagnetic storm has three phases: an initial phase, a main phase and a recovery phase.
The geomagnetic storm recovery phase is that period when Dst changes from the minimum value to its quiet-time value. The period of the geomagnetic storm recovery phase may be as short as 8 hours or as long as 7 days.
Size of a geomagnetic storm is classified as: (1) moderate ( -50 nT >minimum of Dst > -100 nT) (2) intense (-100 nT > minimum Dst > -250 nT) (3) super-storm ( minimum of Dst
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Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
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Links of interest:
+ Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
+ https://Twitter.com/NW7US
+ https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel:
https://YouTube.com/NW7US
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Today’s Sun (artificially-colored in yellow) seen at the 171-angstrom wavelength (Extreme Ultraviolet, or EUV), as viewed by the Solar Dynamics Observatory (SDO), by the Atmospheric Imaging Assembly (AIA).
At this wavelength, at a wavelength not seen by the un-aided eye, we observe the Sun with the 17.1 nm (171 A) filter. This Extreme Ultraviolet (EUV) waveband is used to monitor the corona and upper transition region. With this filter, we can see the myrid of massive magnetic field lines, from simple to complex, that weave and twist throughout the Sun.
The image is a ‘false color image’, meaning that observed data are in a range outside of what human eyes can see, so the data are digitally recast into colors that emphasize physically important features. This view is created from data gathered by the Solar Dynamics Observatory (SDO) satellite that flies above Earth’s atmosphere in an inclined geosynchronous orbit.
Emissions captured in this image come from iron (Fe), a trace element in the solar atmosphere that emits Extreme Ultraviolet (EUV) light when heated to temperatures in excess of one million deg K. In the solar corona the temperatures are so high that most chemical elements have lost many of their electrons. Some of the remaining electrons still attached to the atom emit EUV radiation in narrow wavebands or lines.
The 17.1 nm filter, or channel, is dominated by emissions from highly ionized iron: 8 times ionized (missing 8 electrons) iron–Fe IX. The roman numeral descriptors are consistent with spectral notation: the level of ionization for a given roman numeral is one unit larger that the actual number of missing electrons. The temperatures associated with this level of ionization is about 6 x 10^5 K.
The bright regions in this image correspond to regions of closed magnetic field loops that trap the hot, emitting plasma. Large bright regions are often called active regions. The dark regions correspond to cooler temperatures and possibly to locations where magnetic field lines open into the heliosphere, and thus, do not trap hot plasma.
View live data and images at http://SunSpotWatch.com
We’re on Facebook: http://NW7US.us/swhfr
Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
Links of interest:
- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
- https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel: https://YouTube.com/NW7US
..
Today’s Sun (artificially-colored in purple) seen at the 211-angstrom wavelength (Extreme Ultraviolet, or EUV), as viewed by the Solar Dynamics Observatory (SDO), by the Atmospheric Imaging Assembly (AIA).
At this wavelength, at a wavelength not seen by the un-aided eye, we observe this full-disk AIA image through the 21.1 nm (211 A) filter. This Extreme Ultraviolet (EUV) waveband is used to monitor active regions in the solar corona.
The image is a ‘false color image’, meaning that observed data are in a range outside of what human eyes can see, so the data are digitally recast into colors that emphasize physically important features. This view is created from data gathered by the Solar Dynamics Observatory (SDO) satellite that flies above Earth’s atmosphere in an inclined geosynchronous orbit.
Emissions captured in this image come from iron (Fe), a trace element in the solar atmosphere that emits Extreme Ultraviolet (EUV) light when heated to temperatures in excess of one million deg K. In the solar corona the temperatures are so high that most chemical elements have lost many of their electrons. Some of the remaining electrons still attached to the atom emit EUV radiation in narrow wavebands or lines.
The 21.1 nm filter (also called channel or bandpass) is dominated by emissions from highly ionized iron: 13 times ionized (missing 13 electrons) iron–Fe XIV. Other ionization levels of iron also contribute. The roman numeral descriptors are consistent with spectral notation: the level of ionization for a given roman numeral is one unit larger that the actual number of missing electrons. Additionally there may be some contribution from hot thermal plasma when solar flares are present. The temperatures associated with this level of ionization is about 2 x 10^6 K.
The bright regions in this image correspond to regions of closed magnetic field loops that trap the hot, emitting plasma. Large bright regions are often called active regions. The dark regions correspond to cooler temperatures and possibly to locations where magnetic field lines open into the heliosphere, and thus, do not trap hot plasma.
With this image, we can monitor active regions.
View live data and images at http://SunSpotWatch.com
We’re on Facebook: http://NW7US.us/swhfr
Be sure to subscribe to our space weather and propagation email group, on Groups.io
https://groups.io/g/propagation-and-space-weather
Spread the word!
Links of interest:
- Amazon space weather books: http://g.nw7us.us/fbssw-aSWSC
- https://Twitter.com/NW7US
- https://Twitter.com/hfradiospacewx
Space Weather and Ham Radio YouTube Channel News:
I am working on launching a YouTube channel overhaul, that includes series of videos about space weather, radio signal propagation, and more.
Additionally, I am working on improving the educational efforts via the email, Facebook, YouTube, Tumblr, and other activities.
You can help!
Please consider becoming a Patron of these space weather and radio communications services, beginning with the YouTube channel:
The YouTube channel: https://YouTube.com/NW7US
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