A Few Moments With CQ My Feline Buddy (2018 January 03)
Spending a few moments with my buddy, CQ the Feline -- he is over ten years of age, and still acts a bit like a kitten...
Thank you for watching, commenting, and most of all, for subscribing. By subscribing, you will be kept in the loop for new videos and more... my YouTube Channel: https://YouTube.com/NW7US
A two-way Olivia digital-mode radio conversation between station K8CJM and station NW7US on 12 November 2019 (UTC date). K8CJM is located in Dayton, Ohio, and NW7US is located in Lincoln, Nebraska. See http://OliviaDigitalMode.org for details about the digital mode, Olivia.
NOTE: Compression and ALC!?
Some have noted that it appears that I’ve left on the Compression of the transmitted audio. However, the truth is that compression was not being used (as is proof by carefully taking note of the zero meter movement of the Compression activity). I had the radio set for 20-Meter USB operation on the Sub VFO. Compression was set for standard USB operation. Note also that the radio was transmitting USB-D1, which means the first data/soundcard input to the radio.
Also, some complain about my use of ALC, because, in their view, ALC (automatic level control) is a no-no for data modes.
The notion that one must NEVER use ALC when transmitting digital modes is not accurate.
Multi-frequency shift keyed (MFSK) modes with low symbol rate–such as the Olivia digital modes–use a single carrier of constant amplitude, which is stepped (between 4, 8, 16 or 32 tone frequencies respectively) in a constant phase manner. As a result, no unwanted sidebands are generated, and no special amplifier (including a transmitter’s final stage) linearity requirements are necessary.
Whether the use of ALC matters or not depends on the transmitted digital mode.
For example, FSK (Frequency-Shift Keying; i.e., RTTY) is a constant-amplitude mode (frequency shift only). In such a case, the use of ALC will NOT distort the signal waveform.
PSK31 does contain amplitude shifts, as an example, therefore you don’t want any ALC action that could result in distortion of the amplitude changes in the waveform.
On the other hand, the WSJT manual says that its output is a constant-amplitude signal, meaning that good linearity is not necessary. In that case, the use of ALC will NOT distort the transmitted signal-amplitude waveform. You can use ALC or not, as you choose when you run WSJT modes, or Olivia (MFSK).
Clarification
Nowhere in this am I advocating running your audio really high, thinking that the ALC will take care of it. I am not saying that. I am saying that some ALC is not going to be an issue. You MUST not overdrive any part of the audio chain going into the transmitter!
Transmit audio out of the sound card remains at a constant amplitude, so there will be no significant change in power output if you adjust your input into the radio so that the ALC just stops moving the meter, or, you can have some ALC meter movement. You can adjust your audio to the transmitter either way.
If the transmitter filters have a significant degree of ripple in the passband then you may fin
...
https://www.youtube.com/watch?v=ur7-wHdLxBw
Demonstration of a two-way transmission using the Olivia digital mode on shortwave. I am in QSO (conversation) with KA5TPJ. There are two other Olivia QSOs just below our frequency. Just above us is a lot of FT8 activity. Below the two other Olivia QSOs are PSK31 QSOs. The band is active. And, Olivia is not dead.
-=-=-=-=-
Thank you for watching, commenting, and most of all, for subscribing. By subscribing, you will be kept in the loop for new videos and more... my YouTube Channel: https://YouTube.com/NW7US
-- Tomas, Amateur radio guy and space weather guru; NW7US
-- Home page: http://NW7US.us/ and http://SunSpotWatch.com
-- Contributing editor, propagation and space weather columns in
+ "CQ Amateur Radio Magazine", http://www.cq-amateur-radio.com/
+ "The Spectrum Monitor" http://www.thespectrummonitor.com/
-- Twitter: https://Twitter.com/NW7US (@NW7US)
-- Tumblr: http://blog.nw7us.us
-- Google+ http://nw7us.us/+
-- Instagram: https://instagram.com/nw7us
Linux User #32405 - Since 1996
Copyright, Tomas Hood / NW7US
...
https://www.youtube.com/watch?v=yAIhkaJN15o
How to set the Reed-Solomon Identification feature in Ham Radio Deluxe Digital Master 780 software. Reed-Solomon Identification is also known as RSID.
Please join our Olivia-mode email group:
https://groups.io/g/Olivia
Also, be aware that we have a Facebook group dedicated to instant communication for spotting, scheduling, and so on, at https://www.facebook.com/groups/olivia.hf/ -- please join this group, if you are on Facebook.
Voluntary channelization
Since Olivia signals can be decoded even when received signals are extremely weak, (signal to noise ratio of -14db), signals strong enough to be decoded are sometimes below the noise floor and therefore impossible to search for manually. As a result amateur radio operators have voluntarily decided upon channelization for this mode. This channelization allows even imperceptibly weak signals to be properly tuned for reception and decoding. By common convention amateur stations initiate contacts utilizing 8/250, 16/500, or 32/1000 configuration of the OLIVIA mode and then switch to other configurations to continue the conversation.
Note: some websites publish frequencies that are right on top of weak-signal FT8, JT65 and JT9 segments. Even if that is a matter of contention, follow the regulations and be kind: DO NOT QRM weak-signal QSOs! AGAIN: make sure that your signal does not cross into other sub-bands where weak-signal modes are active. For instance, do not have any part of your signal at x.074 or higher, as this is the sub-band for FT8, JT65A, and JT9.
Quick Reference: we suggest 8/250 as the starting settings when calling CQ on the USB dial frequency of 14.072 MHz with an offset of 700 Hz, on 20m, and on 40m, 7.072 dial with an offset of 700 Hz (and again 8/250). Do not switch to other modes without calling CQ for at least a five-minute window. It is really horrid when people call CQ and change settings, modes, bandwiths, tones, every time they call CQ!
DO NOT QRM WEAK-SIGNAL MODES such as WSPR, JT65A, and JT9! BE AWARE OF THE BAND PLANS FOR THOSE MODES!!
Operating OLIVIA
1. Please make sure you are using the RSID (Reed Solomon Identification - RSID or TXID, RXID) option in your software. RSID transmits a short burst at the start of your transmission which identifies the mode you are using.
When it does that, those amateur radio operators also using RSID while listening will be alerted by their software that you are transmitting in the specific mode (Olivia, hopefully), the settings (like 8/250), and where on the waterfall your transmission is located. This might be a popup window and/or text on the receive text panel. When the operator clicks on that, the software moves the waterfall cursor right on top of the signal and changes the mode in the software. This will help you m
...
https://www.youtube.com/watch?v=lBIacwD9nNM
This visualization shows the position of the Sun's magnetic fields from January 1997 to December 2013.
The field lines swarm with activity: The magenta lines show where the Sun's overall field is negative and the green lines show where it is positive. A region with more electrons is negative, the region with less is labeled positive. Additional gray lines represent areas of local magnetic variation.
The entire Sun's magnetic polarity flips approximately every 11 years (though sometimes it takes quite a bit longer) and defines what's known as the solar cycle. The visualization shows how in 1997, the Sun shows the positive polarity on the top, and the negative polarity on the bottom.
Over the next 12 years, each set of lines is seen to creep toward the opposite pole eventually showing a complete flip. By the end of the movie, each set of lines are working their way back to show a positive polarity on the top to complete the full 22-year magnetic solar cycle.
At the height of each magnetic flip, the Sun goes through periods of more solar activity, during which there are more sunspots, and more eruptive events such as solar flares and coronal mass ejections, or CMEs. The point in time with the most sunspots is called solar maximum.
Credit: NASA
More info: http://SunSpotWatch.com
...
https://www.youtube.com/watch?v=35Ot36WaJc8
From NASA's Scientific Visualization Studio. Solar flares may seem like far-away events, but they can damage satellites and even ground-based technologies and power grids. Every 11 years, as the sun reaches its maximum activity they become bigger and more common, and that increases the chances that one will significantly affect Earth.
So what are these solar eruptions? A solar flare is basically an explosion on the surface of the sun ranging from minutes to hours in length. Large flares can release enough energy to power the entire United States for a million years. Flares happen when the powerful magnetic fields in and around the sun reconnect. They're usually associated with active regions, often seen as sunspots, where the magnetic fields are strongest.
Flares are classified according to their strength. The smallest ones are B-class, followed by C, M and X, the largest. Similar to the Richter scale for earthquakes, each letter represents a ten-fold increase in energy output. So an X is 10 times an M and 100 times a C. Within each letter class, there is a finer scale from 1 to 9. C-class flares are too weak to noticeably affect Earth.
M-class flares can cause brief radio blackouts at the poles and minor radiation storms that might endanger astronauts. It's the X-class flares that are the real juggernauts. Although X is the last letter, there are flares more than 10 times the power of an X1, so X-class flares can go higher than 9. The most powerful flare on record was in 2003, during the last solar maximum. It was so powerful that it overloaded the sensors measuring it. They cut out at X17, and the flare was later estimated to be about X45.
A powerful X-class flare like that can create long lasting radiation storms, which can harm satellites, and even give airline passengers flying near the poles small radiation doses. X flares also have the potential to create global transmission problems and worldwide blackouts.
The seriousness of an X-class flare pointed at Earth is why NASA and NOAA constantly monitor the sun. NASA's Heliophysics fleet of spacecraft can now see the sun from every side and in many different wavelengths. This unprecedented coverage is enabling scientists to predict and detect space weather events like flares and CMEs with ever greater accuracy. With advance warning, governments and companies can take steps to protect their technological infrastructure, so that the worst scenarios will never happen.
Follow space weather here: http://SunSpotWatch.com
Please subscribe. Follow me on Twitter: @NW7US
And, get space weather tweets @hfradiospacewx
...
https://www.youtube.com/watch?v=mIsJO9UWSBg
The sun erupted with an X8 solar flare, one of the largest of the current solar cycle (Sept. 10, 2017). Its source was the same sunspot region that produced an X9 flare last week. We show this in two wavelengths of extreme ultraviolet light at the same time, and each reveals different features. Both are colorized to identify in which wavelength they were observed. The coils of loops after the flare are the magnetic field lines reorganizing themselves after the eruption. The video clip covers about six hours.
Credit: Solar Dynamics Observatory, NASA.
Visit SunSpotWatch.com on Facebook at https://fb.me/spacewx.hfradio
Thank you for watching, commenting, and most of all, for subscribing. By subscribing, you will be kept in the loop for new videos and more... my YouTube Channel: https://YouTube.com/NW7US
-- Tomas, Amateur radio guy and space weather guru; NW7US
-- Homepage: http://NW7US.us/ and http://SunSpotWatch.com
-- Contributing editor, propagation and space weather columns in:
+ "CQ Amateur Radio Magazine."
http://www.cq-amateur-radio.com/
+ "The Spectrum Monitor,"
http://www.thespectrummonitor.com/
+ "RadioUser" (UK)
-- Twitter: https://Twitter.com/NW7US (@NW7US)
-- Tumblr: http://blog.nw7us.us
-- Google+ http://nw7us.us/+
-- Instagram: https://instagram.com/nw7us
Linux User #32405 - Since 1996
Copyright, Tomas Hood / NW7US
...
https://www.youtube.com/watch?v=w66yDb-Ok1I
This high definition video shows the Sun in the 171-angstrom wavelength of extreme ultraviolet light. It covers a time period of January 2, 2015 to January 28, 2016 at a cadence of one frame every hour, or 24 frames per day.
This timelapse is then repeated with narration by solar scientist Nicholeen Viall and contains close-ups and annotations. The 171-angstrom light highlights material around 600,000 Kelvin and shows features in the upper transition region and quiet corona of the sun.
The Sun is always changing and NASA's Solar Dynamics Observatory is always watching. Launched on Feb. 11, 2010, SDO keeps a 24-hour eye on the entire disk of the Sun, with a prime view of the graceful dance of solar material coursing through the Sun's atmosphere, the corona. SDO's sixth year in orbit was no exception. This video shows that entire sixth year--from Jan. 1, 2015 to Jan. 28, 2016 as one time-lapse sequence. Each frame represents 1 hour.
SDO's Atmospheric Imaging Assembly (AIA) captures a shot of the Sun every 12 seconds in 10 different wavelengths. The images shown here are based on a wavelength of 171 angstroms, which is in the extreme ultraviolet range and shows solar material at around 600,000 Kelvin (about 1 million degrees F.) In this wavelength it is easy to see the Sun's 25-day rotation.
During the course of the video, the Sun subtly increases and decreases in apparent size. This is because the distance between the SDO spacecraft and the Sun varies over time. The image is, however, remarkably consistent and stable despite the fact that SDO orbits Earth at 6,876 mph and the Earth orbits the Sun at 67,062 miles per hour.
Scientists study these images to better understand the complex electromagnetic system causing the constant movement on the Sun, which can ultimately have an effect closer to Earth, too: Flares and another type of solar explosion called coronal mass ejections can sometimes disrupt technology in space. Moreover, studying our closest star is one way of learning about other stars in the galaxy. NASA's Goddard Space Flight Center in Greenbelt, Maryland. built, operates, and manages the SDO spacecraft for NASA's Science Mission Directorate in Washington, D.C.
Credit: SDO/NASA/NW7US
Live sun data, and radio propagation resources:
http://SunSpotWatch.com
Music:
Three tracks from YouTube's Free-to-use Music Audio Library:
- Behold the Sun by Topher Mohr and Alex Elena
- Eureka by Huma-Huma
- Malmo Sunrise by The 126ers
And,
"Tides" (ATMOS297) - licensed by SunSpotWatch.com / Tomas Hood from Killer Tracks, used by permission
Thank you for watching, commenting, and most of all, for subscribing. By subscribing, you will be kept in the loop for new videos and more... my YouTube Channel: https://YouTube.com/NW7US
-- Tomas, Amateur r
...
https://www.youtube.com/watch?v=HgP0e1VHBxc