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The latest dx news/current propagation and more. Visit mike's Amateur Radio Page at www.qsl.net/swlham

Monday, July 31, 2017

Today’s Sun (artificially-colored in purple) seen at the...



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 monitore active regions.

View live data and images at http://SunSpotWatch.com

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Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

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Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

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Latest TEC map from NASA. What is TEC? Total Electron Content...



Latest TEC map from NASA. What is TEC? Total Electron Content (or TEC) is an important descriptive quantity for the ionosphere of the Earth. TEC is the total number of free electrons integrated between two points, along a tube of one meter squared cross section, i.e., the electron columnar number density. Affected by solar activity, Total Electron Content (TEC) describes the total number of free electrons present within one square meter between two points (i.e. between the receiver and satellite involved in measuring TEC).

These maps are also used to monitor ionospheric weather, and to nowcast ionospheric storms that often occur responding to activities in solar wind and Earth’s magnetosphere as well as thermosphere.

View live data and images at http://SunSpotWatch.com

Follow: http://ift.tt/1iWH4ta and http://ift.tt/1wJXm19

Facebook: http://NW7US.us/swhfr

And: 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

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

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3XY4D – Rep. of Guinea

UPDATE – dates confirmed as October 27 – November 6, 2017. 3XY4D By F5RAV Luc & F5NVF GĂ©rard , October & November 2017 in Ratoma republic of Guinea , details will be given soon ! 73′ — Charlie5Charlie (@6V7T) April 12, 2017

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The Spectrum Monitor -- August, 2017 • AmateurRadio.com

The Spectrum Monitor -- August, 2017 • AmateurRadio.com

3XY4D Guinea. From DXNews.com

Luc, F5RAV inform dxnews.com, that Luc, F5RAV and Patrick, F5NVF will be active from Guinea 27 October - 6 November 2017 as 3XY4D.

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3XY3D Kassa Island Los Islands. From DXNews.com

Alain F5OZC and Sebastien F8DQZ will be active from Kassa Island, Los Islands (Iles de Los), IOTA AF - 051, 1 - 30 November 2017 as 3XY3D.

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Today’s Sun (artificially-colored in red) seen at the...



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

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources "on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Here is the current forecast discussion on space weather and...



Here is the current forecast discussion on space weather and geophysical activity, issued 2017 Jul 31 1230 UTC.

Solar Activity

24 hr Summary: Solar activity was very low. Region 2669 (N18W43) decayed to plage. B-class activity, including a B9 event at 31/0913 UTC, was observed on the ESE limb from an area of enhanced brightening visible on GOES-15 SXI imagery. This area most likely signals the return of old Region 2665 (S06, L=113). No Earth-directed CMEs were observed in available coronagraph imagery.

Forecast: Solar activity is likely to be at low levels with a slight chance for M-class (R1-R2, Minor-Moderate) flares for the forecast period (31 Jul-02 Aug) due to the return of old Region 2665 (S06, L=113) on or about 31 July.

Energetic Particle

24 hr Summary: The greater than 2 MeV electron flux was at high levels with a peak flux of 7,053 pfu observed at 30/1610 UTC. The greater than 10 MeV proton flux was at background levels.

Forecast: The greater than 2 MeV electron flux is expected to decrease to normal to moderate levels on day one (31 Jul) with the arrival of a negative polarity CH HSS. Moderate to high levels are expected to return on days two and three (01-02 Aug). The greater than 10 MeV proton flux is expected to persist at background levels throughout the forecast period.

Solar Wind

24 hr Summary: Solar wind parameters reflected a nominal solar wind environment. Solar wind speed averaged about 325 km/s. Total field was steady near 5 nT while the Bz component varied between +/-4 nT. Phi angle was oriented in a positive solar sector. A period of non-physical plasma values on the DSCOVR spacecraft was reported from 30/2335 UTC to 31/0354 UTC.

Forecast: The near-Earth solar wind environment is expected to become enhanced beginning on day one (31 Jul) due to the influence of a negative polarity CH HSS. Conditions are expected to continue to be enhanced through day two and slowly diminishing by day three (01-02 Aug).

Geospace

24 hr Summary: The geomagnetic field was quiet under a nominal solar wind regime.

Forecast: Quiet to active levels are expected on days one and two (31 Jul-01 Aug) as a negative polarity CH HSS is expected to influence the geomagnetic field. Quiet to unsettled levels are expected by day three (02 Aug) as CH HSS effects begin to wane.

Don’t forget to visit our live space weather and radio propagation web site, at: http://ift.tt/17yXOGK

Live Aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users: + http://ift.tt/1iWH4ta + http://ift.tt/1wJXm19

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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3XY3D – Los Island AF-051

NEWS UPDATE – Alain, F5OZC informs DX-World.net that 3XY3D will again be active from both Conarky, Guinea and Kassa, Los Island AF-051 between November 1-30, 2017. [previous info below] FEBRUARY 8 @ 16:00z – Today, the callsign 3XY3D (correct call) was issued and now they are active currently on 14250Mhz. The image below is of […]

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Daily solar report: Current Sunspot Cycle 24 Activity and Space...



Daily solar report: Current Sunspot Cycle 24 Activity and Space Weather

Sunspot count: Sun Spots: 11 as of 07/30/2017 10.7-cm Radio Flux: 70 SFU (SFU=Solar Flux Units) Estimated Planetary A-index (Ap): 4 | K-index (Kp): 0

Solar Wind: 330 km/s at 5.0 protons/cm3, Bz is -2.0 nT (Jul 31, 2017 at 1812 UT)

X-ray Solar Flares: 6h hi [B1.4][0316Z 07/31] 24h hi [B1.4][0316Z 07/31]

Background X-ray Level, Last Six Days

Jul 30 2017 :: A4.6 Jul 29 2017 :: A4.0 Jul 28 2017 :: A3.7 Jul 27 2017 :: A3.9 Jul 26 2017 :: A3.8 Jul 25 2017 :: A4.5

Global HF Propagation Conditions for 1800Z on 31 Jul, 2017 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 )

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

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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DXCC Most Wanted 2017. From DXNews.com

DXCC Most wanted countries 2017 Club Log version. Updated 31 July 2017.

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Today’s Sun, seen through a filter of...



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.

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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

Twitter feeds:
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Here is this week’s space weather and geophysical report,...



Here is this week’s space weather and geophysical report, issued 2017 Jul 31 0238 UTC.

Highlights of Solar and Geomagnetic Activity 24 - 30 July 2017

Solar activity was very low throughout the summary period. A B1 flare, observed at 27/2136 UTC from a plage region near center disk, was the strongest event of the period. Region 2668 (N03, L=311, class/area Axx/010 on 25 Jul) decayed to plage by 26 Jul and Region 2669 (N18, L=255, class/area Axx/010 on 30 Jul) remained inactive. No Earth-directed CMEs were observed in available coronagraph imagery.

No proton events were observed at geosynchronous orbit.

The greater than 2 MeV electron flux at geosynchronous orbit was at normal to high levels on 26 Jul, high levels on 30 Jul and moderate to high levels throughout the remaining days of the period. A maximum flux of 18,800 pfu was observed at 25/1515 UTC. The enhancements in flux levels were due to persistently elevated solar winds from a slowly-waning, positive polarity CH HSS.

Geomagnetic field activity ranged from quiet to active levels over the past week. Quiet to active levels were observed on 24 Jul and 26 July; quiet to unsettled levels were observed on 25 Jul and 27-28 Jul; the remaining days were quiet. Geomagnetic activity was associated with the influence of a slowly-waning, positive polarity CH HSS enhancing solar wind speeds. A steady decline in wind speed was observed over the entire reporting period from a peak speed of 705 km/s at 24/2219 UTC to a low of around 350 km/s by the end of 30 Jul.

Forecast of Solar and Geomagnetic Activity 31 July - 26 August 2017

Solar activity is expected to be at low levels with a chance for M-class flare (R1-R2/Minor-Moderate) on 31 Jul - 13 Aug due to the return of old Region 2665 (S06, L=113) rotating across the visible disk. The remainder of the outlook period is expected to be at very low levels.

No proton events are expected at geosynchronous orbit.

The greater than 2 MeV electron flux at geosynchronous orbit is expected to range from normal background to high levels. High levels are expected on 01-03 Aug, 05-10 Aug, and 18-26 Aug; moderate levels are expected 31 Jul and 11 Aug; normal background levels are expected for 04 Aug and 12-17 Aug. All enhancements in electron flux are due to multiple anticipated recurrent CH HSSs.

Geomagnetic field activity is expected to range from quiet to G1 (Minor) geomagnetic storm levels. G1 (Minor) storm levels are likely on 04-05 Aug and again on 17-18 Aug; active conditions are likely on 31 Jul, 06 Aug and 19 Aug; unsettled levels are likely on 01-02 Aug, 07 Aug and 20-21 Aug; quiet conditions are expected for the remaining days of the outlook period. All anticipated enhancements in geomagnetic activity are due to multiple, recurrent CH HSSs.

Don’t forget to visit our live space weather and radio propagation web site, at: http://ift.tt/17yXOGK

Live Aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users: + http://ift.tt/1iWH4ta + http://ift.tt/1wJXm19

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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XT2AW Burkina Faso. From DXNews.com

Harald, DF2WO will be active again from Burkina Faso 28 - 30 September 2017 as XT2AW.

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Today’s graph, plotting the SESC sunspot number, the...



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 
==========================================
2017/07/29 |     12   |     70       |   4
2017/07/28 | 0 | 70 | 7
2017/07/27 | 0 | 68 | 6
2017/07/26 | 0 | 69 | 11
2017/07/25 | 12 | 70 | 9
2017/07/24 | 0 | 70 | 12
2017/07/23 | 0 | 71 | 14
2017/07/22 | 0 | 70 | 16
2017/07/21 | 0 | 69 | 14
2017/07/20 | 0 | 70 | 7
2017/07/19 | 0 | 73 | 4
2017/07/18 | 0 | 78 | 7
2017/07/17 | 13 | 86 | 27
2017/07/16 | 26 | 87 | 41
2017/07/15 | 34 | 92 | 4
2017/07/14 | 58 | 94 | 4
2017/07/13 | 55 | 92 | 4
2017/07/12 | 43 | 90 | 4
2017/07/11 | 27 | 91 | 8
2017/07/10 | 32 | 95 | 9
2017/07/09 | 31 | 91 | 28
2017/07/08 | 24 | 87 | 3
2017/07/07 | 25 | 80 | 5
2017/07/06 | 16 | 76 | 7
2017/07/05 | 11 | 73 | 3
2017/07/04 | 0 | 72 | 4
2017/07/03 | 0 | 72 | 5
2017/07/02 | 11 | 71 | 18

For complete live data and images visit http://SunSpotWatch.com

Be sure to share this post, to spread the love!

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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

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Did you know? Here’s a space weather and radio...



Did you know? Here’s a space weather and radio propagation educational tidbit – from http://SunSpotWatch.com – at 14:00 UTC on 2017-07-31:

Our magnetosphere deflects much of the solar wind, around the Earth, generating energy. When this stored solar wind energy is released by the magnetosphere, a ‘geomagnetic substorm’ is triggered.

A geomagnetic storm is made up of many substorms, and the geomagnetic storm can have serious impact on the ionosphere.

Geomagnetic storms are almost always associated with a decreases in F-region electron density. Geomagnetic storms can result in a lowering of the maximum usable frequency of a radio path between two points on the Earth. In short, a geomagnetic storm can cause difficulties in communicating over long distances on shortwave radio frequencies.

Geomagnetic storms are rated by NOAA on a scale, G1 to G5, G5 being severe.

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:



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Today’s Sun (artificially-colored in yellow) seen at the...



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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Latest TEC map from NASA. What is TEC? Total Electron Content...



Latest TEC map from NASA. What is TEC? Total Electron Content (or TEC) is an important descriptive quantity for the ionosphere of the Earth. TEC is the total number of free electrons integrated between two points, along a tube of one meter squared cross section, i.e., the electron columnar number density. Affected by solar activity, Total Electron Content (TEC) describes the total number of free electrons present within one square meter between two points (i.e. between the receiver and satellite involved in measuring TEC).

These maps are also used to monitor ionospheric weather, and to nowcast ionospheric storms that often occur responding to activities in solar wind and Earth’s magnetosphere as well as thermosphere.

View live data and images at http://SunSpotWatch.com

Follow: http://ift.tt/1iWH4ta and http://ift.tt/1wJXm19

Facebook: http://NW7US.us/swhfr

And: 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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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3B8/PA3HGT Mauritius Island. From DXNews.com

Hans, PA3HGT will be active from Mauritius Island, IOTA AF - 049, 5 - 22 September 2017 as 3B8/PA3HGT.

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3B8/PA3HGT – Mauritius

Hans, PA3HGT will be active from Mauritius as 3B8/PA3HGT between September 5-22, 2017. QRV on 40-20-10m, QSL via H/c.

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[UPDATE] 3Y0Z – Bouvet 2018

As in any group, the moral compass, accountability, and integrity of amateur radio operators covers a wide spectrum. The best of these character qualities in the ham radio community came to light last week. FlexRadio Systems and Ranko Boka, 4O3A, of SKY SAT wanted to be absolutely positive that they would in no way compromise […]

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Ham Radio Operators to Hold 'Special Event' During Solar Eclipse:

ALTON -- The public is invited to observe members of the Lewis and Clark Radio Club, Inc. attempting to communicate with other amateur radio operators across the United States during the upcoming Solar Eclipse event from 11 a.m. to 2 p.m. on Monday, Aug. 21 at Riverview Park in Alton. Members of the Lewis and Clark Radio Club, Inc. will set up and operate a "special event" amateur radio station in the park and attempt contact with other ham radio operators across the country during the solar eclipse. "This will be a citizen's scientific experiment," said John Nell, chairman for the event. "Since hams are dependent upon layers of the ionosphere to communicate around the globe, and the sun affects each of those layers differently, we're not sure what (if any) effect the solar eclipse will have on our radio communication capabilities. We hope this experiment will shed some light on the subject."

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Seattle Community Hubs Drill for 'The Big One':

Almost a dozen communications hubs participated in a Seattle city-wide disaster drill Saturday. The exercise was in preparation for a magnitude 9.0 Cascadia Rising Subduction Zone earthquake. In all, 11 communications hubs participated. The city lists a total of 139 emergency hub locations. "You've got people all over the city doing what I'm doing right now with setups that are probably somewhat like this," said Tim Helming, an Auxiliary Communications Services (ACS) volunteer trained in operating ham radio. Helming ran the amateur radio at the Rainier Beach Community Center. "Which gives us point to point communication good for a few miles, but through repeater systems (it reaches) city-wide and even all over Western Washington," he said. The communication would be vital. The city could give notices to the neighborhoods, while the hubs can request or offer hel

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Sunday, July 30, 2017

Today’s Sun (artificially-colored in purple) seen at the...



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 monitore active regions.

View live data and images at http://SunSpotWatch.com

              • +

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NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Latest TEC map from NASA. What is TEC? Total Electron Content...



Latest TEC map from NASA. What is TEC? Total Electron Content (or TEC) is an important descriptive quantity for the ionosphere of the Earth. TEC is the total number of free electrons integrated between two points, along a tube of one meter squared cross section, i.e., the electron columnar number density. Affected by solar activity, Total Electron Content (TEC) describes the total number of free electrons present within one square meter between two points (i.e. between the receiver and satellite involved in measuring TEC).

These maps are also used to monitor ionospheric weather, and to nowcast ionospheric storms that often occur responding to activities in solar wind and Earth’s magnetosphere as well as thermosphere.

View live data and images at http://SunSpotWatch.com

Follow: http://ift.tt/1iWH4ta and http://ift.tt/1wJXm19

Facebook: http://NW7US.us/swhfr

And: 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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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New Book of Short Stories Highlights 'Magic of Ham Radio':

A new book by prolific, award-winning, and best-selling writer Don Keith employs short fictional stories to demonstrate what the author calls the "magic" still inherent in the century-old hobby of Amateur (or "Ham") Radio. Keith is also a long-time active participant in the hobby, holding the Amateur Extra-class license and the call letters N4KC.

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Amateur Radio Roundtable:

Join Katie Allen, WY7YL, Dave, and me Tuesday nights for Amateur Radio Roundtable. Our guest will be Rich Richard Moseson W2VU, editor of CQ magazine giving us some insight to next months edition. Dave and Tom will be talking about antennas. Plus lots of other great stuff.

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R24RRC – Shantar Islands AS-044

Members of the recent RI0C IOTA Dxpedition to Iony Island AS-069 are now on their way to Shantarskiye Islands AS-044 and will be active as R24RRC. QSL via R7AL, OQRS.

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JW/OM6TC – Svalbard

Jozef OM6TC will be active from Svalbard between September 15-20, 2017 as JW/OM6TC. He will work CW and SSB on HF with 100W, delta-loop on 80m and other wire antennas. QSL via OM6TC. Buro is prefered.

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5W0HA – Samoa

Bert, CX3AN will be active from Upolu, Samoa as 5W0HA between August 19-26, 2017. Focus on 30 & 40 CW and 20 & 17 SSB. QSL via H/c. Note: Bert will also be active from Vanuatu the week after his Samoa trip. Callsign not yet known.

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Today’s Sun (artificially-colored in red) seen at the...



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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources "on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Here is the current forecast discussion on space weather and...



Here is the current forecast discussion on space weather and geophysical activity, issued 2017 Jul 30 1230 UTC.

Solar Activity

24 hr Summary: Solar activity was very low. New Region 2669 (N18W31, Bxo/beta) emerged this period but was relatively simple and unproductive. No Earth-directed CMEs were observed in available coronagraph imagery.

Forecast: There is a chance for C-class flare activity on day one (30 Jul) with C-class flares likely on days two and three (31 Jul-01 Aug) due to the return of old Region 2665 (S06, L=113). There is a slight chance for M-class (R1-R2 (Minor-Moderate)) flares throughout the forecast period.

Energetic Particle

24 hr Summary: The greater than 2 MeV electron flux reached high levels this period with a peak flux of 8,288 pfu observed at 29/1510 UTC. The greater than 10 MeV proton flux was steady at near-background levels throughout the period.

Forecast: The greater than 2 MeV electron flux is expected to reach high levels on days one and three (30 Jul, 01 Aug). Normal to moderate electron fluxes are likely on day two (31 Jul) due to elevated geomagnetic field activity. The greater than 10 MeV proton flux is expected to persist at near-background levels throughout the forecast period.

Solar Wind

24 hr Summary: The near-Earth solar wind environment reflected a nominal solar wind environment this period and solar wind parameters were steady at near-background levels throughout the period.

Forecast: The near-Earth solar wind environment is expected to become enhanced beginning on day two through day three (31 Jul-01 Aug) due to the influence of a negative polarity CH HSS.

Geospace

24 hr Summary: The geomagnetic field was quiet under a nominal solar wind regime.

Forecast: The geomagnetic field is expected to be quiet on day one (30 Jul). The influence of a negative polarity CH HSS is expected to cause periods of active conditions on day two (31 Jul) and unsettled conditions on day three (01 Aug).

Don’t forget to visit our live space weather and radio propagation web site, at: http://ift.tt/17yXOGK

Live Aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users: + http://ift.tt/1iWH4ta + http://ift.tt/1wJXm19

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Daily solar report: Current Sunspot Cycle 24 Activity and Space...



Daily solar report: Current Sunspot Cycle 24 Activity and Space Weather

Sunspot count: Sun Spots: 12 as of 07/29/2017 10.7-cm Radio Flux: 70 SFU (SFU=Solar Flux Units) Estimated Planetary A-index (Ap): 4 | K-index (Kp): 0

Solar Wind: 340 km/s at 1.0 protons/cm3, Bz is -2.0 nT (Jul 30, 2017 at 1814 UT)

X-ray Solar Flares: 6h hi [none] 24h hi [none]

Background X-ray Level, Last Six Days

Jul 29 2017 :: A4.0 Jul 28 2017 :: A3.7 Jul 27 2017 :: A3.9 Jul 26 2017 :: A3.8 Jul 25 2017 :: A4.5 Jul 24 2017 :: A4.8

Global HF Propagation Conditions for 1800Z on 30 Jul, 2017 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 )

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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



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Amateur Radio News - Ham Radio Library

Amateur Radio News - Ham Radio Library

Today’s Sun, seen through a filter of...



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.

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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

Twitter feeds:
http://ift.tt/1iWH4ta and http://ift.tt/1wJXm19



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Today’s graph, plotting the SESC sunspot number, the...



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 
==========================================
2017/07/29 |     12   |     70       |   4
2017/07/28 | 0 | 70 | 7
2017/07/27 | 0 | 68 | 6
2017/07/26 | 0 | 69 | 11
2017/07/25 | 12 | 70 | 9
2017/07/24 | 0 | 70 | 12
2017/07/23 | 0 | 71 | 14
2017/07/22 | 0 | 70 | 16
2017/07/21 | 0 | 69 | 14
2017/07/20 | 0 | 70 | 7
2017/07/19 | 0 | 73 | 4
2017/07/18 | 0 | 78 | 7
2017/07/17 | 13 | 86 | 27
2017/07/16 | 26 | 87 | 41
2017/07/15 | 34 | 92 | 4
2017/07/14 | 58 | 94 | 4
2017/07/13 | 55 | 92 | 4
2017/07/12 | 43 | 90 | 4
2017/07/11 | 27 | 91 | 8
2017/07/10 | 32 | 95 | 9
2017/07/09 | 31 | 91 | 28
2017/07/08 | 24 | 87 | 3
2017/07/07 | 25 | 80 | 5
2017/07/06 | 16 | 76 | 7
2017/07/05 | 11 | 73 | 3
2017/07/04 | 0 | 72 | 4
2017/07/03 | 0 | 72 | 5
2017/07/02 | 11 | 71 | 18
2017/07/01 | 11 | 71 | 11

For complete live data and images visit http://SunSpotWatch.com

Be sure to share this post, to spread the love!

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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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

Get your copy of the self-study space weather and radio propagation course: http://nw7us.us/swc



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CQ Six - 50 MHz DX News, by OZ6OM

CQ Six - 50 MHz DX News, by OZ6OM

dxerhamnews

dxerhamnews

dxerhamnews

dxerhamnews

Made some Olivia signals, yesterday and today. Olivia is a great...



Made some Olivia signals, yesterday and today. Olivia is a great mode!

#hamr #hamradio #hobby #amateur #radio #radioamateur #amateurradio #swl #digital #fun



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Did you know? Here’s a space weather and radio...



Did you know? Here’s a space weather and radio propagation educational tidbit – from http://SunSpotWatch.com – at 14:00 UTC on 2017-07-30:

The ionosphere is strongly dependent on the condition of the geomagnetic field. Earth’s geomagnetic field wraps around the Earth and the ionosphere. The solar wind drags the geomagnetic field and creates the Earth’s magnetosphere.

Despite its name, the magnetosphere is distinctly non-spherical. Earth’s magnetosphere provides for our protection from the Sun and from space.

The Sun-side of the magnetosphere is compressed toward the Earth. The night-side of the magnetosphere is dragged far out into space away from the Sun. The magnetosphere’s shape is kind of like that of a comet, facing the Sun.

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:



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TA4/US7IGN Kargicak Turkey. From DXNews.com

Vlad, US7IGN will be active from Turkey 7 - 17 August 2017 as TA4/US7IGN.

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Today’s Sun (artificially-colored in yellow) seen at the...



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

              • +

BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

If you are on Twitter, please follow these two users:

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Latest TEC map from NASA. What is TEC? Total Electron Content...



Latest TEC map from NASA. What is TEC? Total Electron Content (or TEC) is an important descriptive quantity for the ionosphere of the Earth. TEC is the total number of free electrons integrated between two points, along a tube of one meter squared cross section, i.e., the electron columnar number density. Affected by solar activity, Total Electron Content (TEC) describes the total number of free electrons present within one square meter between two points (i.e. between the receiver and satellite involved in measuring TEC).

These maps are also used to monitor ionospheric weather, and to nowcast ionospheric storms that often occur responding to activities in solar wind and Earth’s magnetosphere as well as thermosphere.

View live data and images at http://SunSpotWatch.com

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And: 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

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W1NAS SES / NAS South Weymouth ARC:

On Saturday, August 19, 2017, from 0900-1500 EDT (1300-1900 UTC) W1NAS will again be operating on 20 and hopefully 40 meters phone to commemorate the flight of the blimp Snow Goose from NAS South Weymouth to Resolute Bay on the Arctic Circle, while the submarine USS "Nautilus" sailed beneath them under the polar ice cap.

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'Ham' Radio Operators Invade South Shore:

CHARLOTTETOWN, P.E.I. -- Is anyone noticing stepladders aplenty, strange looking aerials going up and wire being carefully strung across back gardens along the south shore? Amateur radio (aka ham) enthusiasts are up and running with renewed vigour. In its initial stages in the late 19th century, the term "ham" was coined to describe amateur radio operators. While there are different opinions of how the term was derived, the most popular appears to be that professional radio operators perceived their amateur counterparts as unskilled and inept; however, nothing could be further from the truth. Ham radio requires an understanding of how radio waves operate and "bounce", as well as knowledge in electronic components, wiring, math and much more in order to be licensed. Although there is no longer a requirement to learn Morse Code many operators still undertake that daunting challenge. Transatlantic radio "listening" communication first occurred in 1922, followed by the first two-way radio communication in 1923 between the U.K. and U.S. Although amateur radio communication was suspended during the Second World War, the war emergency radio service was developed by the military and interest resumed after the war. Over the past century, amateur radio has evolved from being a way for individuals to communicate to being the most effective way to communicate with individuals and emergency crews in disaster areas. A cell phone and landline might be inoperative (like during 9-11) and the electricity might be off, but the ham radio operator will be receiving and sending information.

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ARISS Marked its 20th Anniversary:

The Amateur Radio on the International Space Station (ARISS) had outstanding success with many receiving its Slow Scan TV images of the past and present. The images were collected from throughout the world and transmitted on a number of days starting with July 20. The ISS Russian Segment computer stored them and each were transmitted by a Kenwood TM-D710 transceiver. What resulted was a display of unique images sharing the accomplishments of ARISS over the last two decades. They traced development from the first meeting that led to ARISS being the voice link for school groups, to the modern era of Ham-TV delivering television contacts from the space station with students in some countries.

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Project Amelia Earhart Flight Nears its End:

The commemorative Amelia Earhart around the world flight by pilot Brian Lloyd WB6RQN crossed the Pacific Ocean, landing first at Pago Pago in American Samoa, then Hawaii via a symbolic flyover of Howland Island. The Mooney M20K 231 registration number N916BL named 'Spirit' has expanded fuel capacity, modern satellite avionics gear, and a Ham radio transceiver enabling WB6RQN Aeronautical Mobile to talk to hundreds of radio amateurs. At Pago Pago (July 23) he was greeted by a news reporter for an interview, then got the latest weather information, with Ellie from the National Weather Service finishing her shift and taking him to a downtown restaurant for a meal of Samoan Oka (rockfish). Brian WB6RQN said the next stage was the hardest leg of the trip that was going to "push both the plane and me to the limit of our abilities". He explained that the single engine propeller driven 'Spirit' was fully fuelled including three hours flying time of reserve fuel because "there are scant alternatives should problems mount up for any reason". Earlier the flight had magneto problems, a fuel vapouring scare that caused him to turn back to New Zealand, not to mention adverse weather with fierce winds, blasting sandstorms, severe tropical conditions, thunder snow and high altitude ice. After leaving Pago Pago just before sunrise with about 19 hours ahead there was the planned flyover of Howland Island dropping a floral wreath where Earhart and her navigator Fred Noonan tried unsuccessfully to land.

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HC8/G8OFQ Isabella Island, Galapagos SA-004

Geoffrey  G8OFQ will be active again from Isabela Island, Galapagos Islands IOTA SA-004, 1 August to 31 October 2017 as HC8/G8OFQ.
Working on HF bands, 6m and possibley doing some satellity activity on 2m and 70cm SSB.
QSL via home call direct, LOTW and ClubLog.



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OY/CT1BWW Faroe Islands EU-018

Marq CT1BWW will be active from Faroe Islands, IOTA EU-018, 1 to 10 August 2017 as OY/CT1BWW.
Working on 40 – 10m in CW, SSB and Digital modes.
QSL via EA4URE bureau or direct.

 



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6V/DC4CQ Senegal

Franz DC4CQ will be active from Senegal, 30 July to 11 August 2017 as 6V/DC4CQ.
Working on 40 – 15m SSB.

QSL via home call.



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V34AO Belize

Rob DL7VOA informs DxCoffee readers:

“Dear DXers,

Once again my wife and I plan to explore another exciting part of our small planet. This time we will follow the tracks of the Maya in Central America with a final recreation stay in Belize. I plan to be active as V34AO from Hopkins in Belize between Nov 18 and Nov 30, 2017. The QTH will be directly on the beach of Hopkins with every QSO made viewing over the Caribbean Sea. As usual, operating will take place in “holiday style” mainly in CW during the local evening and night hours (maybe some SSB, no digital).

I will have my little Elecraft K2 with me running 100 watts into a 10m fiberglass pole with vertical dipoles on 10/12/15/17/20m, groundplanes for 30m/40m or an Inverted L for 80m. I will join the CQWW CW Contest (single operator all band, low power) with the only focus on having fun in pile-ups. The contest weekend will be (mostly) mine but during the rest of the time please understand that during day time there are other important holiday activities to be undertaken with my wife like relaxing, snorkeling, flying my drone, etc. instead of conducting a 100% DXpedition (which does not mean that I never show up on the bands during day time).

I already have a licence for the regular callsign V31EO but I have also applied for the short term special callsign V34AO and I am very optimistic that it will be issued to me as well. Depending on the limitations I am planning to use the special call V34AO not only during the CQWW CW Contest but also throughout my stay.

All information (including a link with exact GPS coordinates and maybe later also some drone videos) can be found on the website: http://ift.tt/2vQeyY9

QSLs for V34AO (or V31EO) via bureau or direct to DL7VOA.

73 de Rob, DL7VOA



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Saturday, July 29, 2017

Today’s Sun (artificially-colored in purple) seen at the...



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 monitore active regions.

View live data and images at http://SunSpotWatch.com

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BOOK SALE: Space Weather and Sun Science - get these from Amazon, and help us stay online!

NOTICE: When you buy this (or any item after starting with this link), you are helping us keep our SunSpotWatch.com and other resources “on the air” (up and running!). In other words, you are helping the entire community. So, check out this book:

Here is the link to Amazon: http://g.nw7us.us/fbssw-aSWSC

              • +

Don’t forget: You can also get the space weather and radio propagation self-study course, today. Visit http://nw7us.us/swc for the latest sale and for more information!

              • +

Visit our live space weather and radio propagation web site, at: http://SunSpotWatch.com

See the live aurora mapping is at http://ift.tt/2lYUS2h

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



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