Re: [digitalradio] Re: jpskmail can now send a binary attachment
Just copy the javapskmail.jar file over the old one and leave everything else in place... Or use the new pskmail_0_3_5c.zip archive from Per... The pskmail mailing list has more info. 73, Rein Pa0R . -Ursprüngliche Nachricht- Von: Bill McLaughlin n9...@comcast.net Gesendet: 11.04.09 18:49:16 An: digitalradio@yahoogroups.com Betreff: [digitalradio] Re: jpskmail can now send a binary attachment I have not been able to get it to boot; no problems with the earlier release. 73, Bill N9DSJ --- In digitalradio@yahoogroups.com, Rick W mrf...@... wrote: Have you been able to get this alpha to boot up? (Note: you have to change erac to esrac in the main url to access the site.) 73, Rick, KV9U Andrew O'Brien wrote: --- In digitalradio@yahoogroups.com, Andrew O'Brien k3ukandy@ wrote: I saw this message jpskmail can now send a binary attachment, some tweaking necessary earlier this morning from Rein PA0R . Looks like an important step and will make playing with the Java PSKmail fun this weekend. Andy K3UK The new release is out... http://tinyurl.com/cdu7ha Announce your digital presence via our Interactive Sked Pages at http://www.obriensweb.com/sked Recommended digital mode software: Winwarbler, FLDIGI, DM780, or Multipsk Logging Software: DXKeeper or Ham Radio Deluxe. Yahoo! Groups Links -- http://pa0r.blogspirit.com Announce your digital presence via our Interactive Sked Pages at http://www.obriensweb.com/sked Recommended digital mode software: Winwarbler, FLDIGI, DM780, or Multipsk Logging Software: DXKeeper or Ham Radio Deluxe. Yahoo! Groups Links * To visit your group on the web, go to: http://groups.yahoo.com/group/digitalradio/ * Your email settings: Individual Email | Traditional * To change settings online go to: http://groups.yahoo.com/group/digitalradio/join (Yahoo! ID required) * To change settings via email: mailto:digitalradio-dig...@yahoogroups.com mailto:digitalradio-fullfeatu...@yahoogroups.com * To unsubscribe from this group, send an email to: digitalradio-unsubscr...@yahoogroups.com * Your use of Yahoo! Groups is subject to: http://docs.yahoo.com/info/terms/
[digitalradio] HELP!!!
I have a TS-2000 and a Rigblaster Plus. I had it fully operational for almost 5 years, not touching or changing a thing. I recently moved everything, and now, can't get the cables right. Can someone give me a connect this to that direction? I do have the manual, but it really is not much of a help. I have tried every possible configuration, except the right one. I have missed a couple of contests already. Don KA5DON DRCC #59 EPC #125 FeldHell #981 30M Digital Grp #0680
Re: [digitalradio] HELP!!!
Go back to the basics.Being a ham you should be able to do it.I have faith In you. K4YDI Al. On Sun, Apr 12, 2009 at 10:13 AM, Don Rand don.r...@gmail.com wrote: I have a TS-2000 and a Rigblaster Plus. I had it fully operational for almost 5 years, not touching or changing a thing. I recently moved everything, and now, can't get the cables right. Can someone give me a connect this to that direction? I do have the manual, but it really is not much of a help. I have tried every possible configuration, except the right one. I have missed a couple of contests already. Don KA5DON DRCC #59 EPC #125 FeldHell #981 30M Digital Grp #0680 Announce your digital presence via our Interactive Sked Pages at http://www.obriensweb.com/sked Recommended digital mode software: Winwarbler, FLDIGI, DM780, or Multipsk Logging Software: DXKeeper or Ham Radio Deluxe. Yahoo! Groups Links
[digitalradio] Re: picture packet prgm
Morning, I know this is unsolisted but have you considered Outpost or EcomScs? http://www.outpostpm.org/ http://www.qsl.net/kb2scs/ecomscs.html Just asking, currently I use WinPac but am looking for the next best thing !!! 73, Lee kd4gcf --- In digitalradio@yahoogroups.com, jim seeber wb3...@... wrote: Hi, new user here, Jim kw3u in NE Pa. our local ares/races group is putting a packet system together fm various tnc's and are now at the point where we would like everyone to use the same prgm. I have been checking out some of them and found an old one called picture packet that seems to work with all nicely, but a lot of the features are grayed out. If anyone has a full version it would be appreciated, I think it was in the 1990's. also any other simple to operate programs for windows. thanks Jim kw3u
Re: [digitalradio] HELP!!!
Just in case it helps, try this: Connect the microphone to the mic jack on the front of the Rigblaster; hook the microphone extension cable from the RJ45 on the back of the Rigblaster to the mic jack on the front of the TS-2000; hook a shielded audio cable from the 'Ext Sp2' jack on the back of the TS-2000 to the 'Line Input' jack on your sound card; (You may have to use 'Mic In' but 'Line In' is better.) hook a shielded audio cable from the 'Audio In' jack on the back of the Rigblaster to the 'Line Out' (or 'Speaker') on your sound card; hook a 12v power source to the Rigblaster power jack. If you are using hardware PTT (as opposed to VOX) to key the rig, hook a serial cable from the serial port on the Rigblaster to a serial port on the computer. Good luck, let us know how you come out. 73, Howard K5HB From: Don Rand don.r...@gmail.com To: digitalradio@yahoogroups.com Sent: Sunday, April 12, 2009 10:13:41 AM Subject: [digitalradio] HELP!!! I have a TS-2000 and a Rigblaster Plus. I had it fully operational for almost 5 years, not touching or changing a thing. I recently moved everything, and now, can't get the cables right. Can someone give me a connect this to that direction? I do have the manual, but it really is not much of a help. I have tried every possible configuration, except the right one. I have missed a couple of contests already. Don KA5DON DRCC #59 EPC #125 FeldHell #981 30M Digital Grp #0680
Re: [digitalradio] HELP!!!
Howard, Thanks, I'm sure that will get me going again. I had to leave for work (Army) but will be back home on Friday. I will certainly let you know when I am digital again. Don KA5DON
[digitalradio] HF and the Spotless Sun
All, Interesting read about solar output and HF propagation by Paul Harden, NA5N. Tony -K2MO Paul wrote: During the quiet sun, solar flux in the 60-100 range is typical. During the active sun, 150-200 is typical. The higher the solar flux, the more ionizing radiation that is striking our ionosphere, producing free electrons that stratify into the D, E and F layers. The more free electrons in the E and F layers, the more reflective they are to HF frequencies and the higher the MUF. Right now, with solar flux in the 60-100 range, the E and F layers are poorly ionized, yielding a lower MUF and not acting as a very good mirror for bouncing HF signals back to earth. Very generally, when the solar flux is around 100, 15M will be open; above 150 10M will be open. Below 100, 20M will usually die shortly after sunset. IMPORTANT: The MUF seldoms drops below 10MHz. Therefore, the solar flux has very little effect on 30, 40 and 80M propagation. These bands are fairly immune from the solar flux and the 11-year solar cycle. Magnetic disturbances on the sun produce sunspots (cooler areas). Occassionally, the magnetic field lines of the disturbance(s) grow to such an intensity that it produces a small hole in the solar surface, allowing hot solar mass to escape. This is a SOLAR FLARE. While this hole is present (usually in the order of minutes to tens of minutes), energetic electrons and ionozing radiation (that is, x-rays and sometimes gamma rays) are allowed to escape. This, of course, quickly increases the overall radiation output of the sun. The ionozing radiation, when it strikes the earth 8 minutes later, will ionize the E and F layers, making them more reflective to HF and raise the MUF, usually for the rest of the day until local sundown. The radiation from especially strong flares can penetrate into our ionosphere to the D-layer. When the D-layer is highly ionized, it becomes very absorptive to HF signals, and in extreme cases, can produce a temporary HF blackout. Most flares will not appreciably increase the daily solar flux; therefore, the solar flux alone is not a good indicator following a flare to increased E and F layer reflectivity (and hence, good skip DX). As the number of sunspots increases, there is a higher chance of solar flares, and the daily solar flux tends to increase. However, there is *no* direct mathematical relationship between sunspot count and the solar flux. They follow the same trend when plotted, but no one can say 10 sun spots equals xxx solar flux units. The solar flux will vary from a minimum to maximum value over 28-days, related to the solar rotation. It also varies from minimum to maximum over the 11-year solar cycle. Thus, it is a slowly varying indicator that is used to show the general trend of the sun for the current 28-day cycle, and for the current solar cycle. It is not used for an hourly or daily predictor. Propagation programs use solar flux values primarily for calculating the MUF and what bands will be open, or closed, at different times of the day. When a solar flare occurs, it often produces a shockwave carrying electrons and other solar mass away from the sun. This is called a coronal mass ejection or CME. If the solar flare is located towards the center of the sun (as opposed to the limbs or edges), the trajectory of the shockwave will intercept with the earth, usually about 50-55 hours later. When this happens, the shockwave will compress the Earth's geomagnetic field, triggering a GEOMAGNETIC STORM, generating huge electric currents flowing along the Earth's magnetic field lines, causing increased noise levels. IMPORTANT: This effect is more pronounced on the lower frequencies, such that 30M, 40M, 80M are more effected by the noise storm than is 20, 15 and 10M. The amount of wiggling or disturbance to our magnetic field is the K-Index. It is measured every 3 hours to show what the present state of our geomagnetic field is. K=1 to 3 is fairly quiet to unsettled. Higher numbers (K4) is a geomagnetic storm. K7 is a severe to extreme storm. The K-Indices throughout the day are averaged over the UTC day to form the A-Index. It basically tells you what our geomagnetic field did YESTERDAY. It is usually expressed as the Ap, or planetary A-index, being averaged over 24 hours and from all the reporting stations. THEREFORE, the SOLAR FLUX tells you the general radiation output of the sun. But, don't expect it to make a sudden jump to open up 15 or 10M. That takes years ... or an M or X-class solar flare. The A-Index tells you what our geomagnetic field did YESTERDAY. It tells you almost nothing about what the bands sound like TODAY. For that, find out what the current K-Index is. The lower the number, the better. Above about 6 or 7, conditions on the LOWER bands will be very rough. WHEN TO OPERATE For QRPers, a good time to operate is right after a
[digitalradio] Re: HF and the Spotless Sun
Bob NM7M's Propagation 101, 201, 301 is another good introduction to this topic. I placed a copy in this group's Files area. 73, Dave, AA6YQ --- In digitalradio@yahoogroups.com, Tony d...@... wrote: All, Interesting read about solar output and HF propagation by Paul Harden, NA5N. Tony -K2MO Paul wrote: During the quiet sun, solar flux in the 60-100 range is typical. During the active sun, 150-200 is typical. The higher the solar flux, the more ionizing radiation that is striking our ionosphere, producing free electrons that stratify into the D, E and F layers. The more free electrons in the E and F layers, the more reflective they are to HF frequencies and the higher the MUF. Right now, with solar flux in the 60-100 range, the E and F layers are poorly ionized, yielding a lower MUF and not acting as a very good mirror for bouncing HF signals back to earth. Very generally, when the solar flux is around 100, 15M will be open; above 150 10M will be open. Below 100, 20M will usually die shortly after sunset. IMPORTANT: The MUF seldoms drops below 10MHz. Therefore, the solar flux has very little effect on 30, 40 and 80M propagation. These bands are fairly immune from the solar flux and the 11-year solar cycle. Magnetic disturbances on the sun produce sunspots (cooler areas). Occassionally, the magnetic field lines of the disturbance(s) grow to such an intensity that it produces a small hole in the solar surface, allowing hot solar mass to escape. This is a SOLAR FLARE. While this hole is present (usually in the order of minutes to tens of minutes), energetic electrons and ionozing radiation (that is, x-rays and sometimes gamma rays) are allowed to escape. This, of course, quickly increases the overall radiation output of the sun. The ionozing radiation, when it strikes the earth 8 minutes later, will ionize the E and F layers, making them more reflective to HF and raise the MUF, usually for the rest of the day until local sundown. The radiation from especially strong flares can penetrate into our ionosphere to the D-layer. When the D-layer is highly ionized, it becomes very absorptive to HF signals, and in extreme cases, can produce a temporary HF blackout. Most flares will not appreciably increase the daily solar flux; therefore, the solar flux alone is not a good indicator following a flare to increased E and F layer reflectivity (and hence, good skip DX). As the number of sunspots increases, there is a higher chance of solar flares, and the daily solar flux tends to increase. However, there is *no* direct mathematical relationship between sunspot count and the solar flux. They follow the same trend when plotted, but no one can say 10 sun spots equals xxx solar flux units. The solar flux will vary from a minimum to maximum value over 28-days, related to the solar rotation. It also varies from minimum to maximum over the 11-year solar cycle. Thus, it is a slowly varying indicator that is used to show the general trend of the sun for the current 28-day cycle, and for the current solar cycle. It is not used for an hourly or daily predictor. Propagation programs use solar flux values primarily for calculating the MUF and what bands will be open, or closed, at different times of the day. When a solar flare occurs, it often produces a shockwave carrying electrons and other solar mass away from the sun. This is called a coronal mass ejection or CME. If the solar flare is located towards the center of the sun (as opposed to the limbs or edges), the trajectory of the shockwave will intercept with the earth, usually about 50-55 hours later. When this happens, the shockwave will compress the Earth's geomagnetic field, triggering a GEOMAGNETIC STORM, generating huge electric currents flowing along the Earth's magnetic field lines, causing increased noise levels. IMPORTANT: This effect is more pronounced on the lower frequencies, such that 30M, 40M, 80M are more effected by the noise storm than is 20, 15 and 10M. The amount of wiggling or disturbance to our magnetic field is the K-Index. It is measured every 3 hours to show what the present state of our geomagnetic field is. K=1 to 3 is fairly quiet to unsettled. Higher numbers (K4) is a geomagnetic storm. K7 is a severe to extreme storm. The K-Indices throughout the day are averaged over the UTC day to form the A-Index. It basically tells you what our geomagnetic field did YESTERDAY. It is usually expressed as the Ap, or planetary A-index, being averaged over 24 hours and from all the reporting stations. THEREFORE, the SOLAR FLUX tells you the general radiation output of the sun. But, don't expect it to make a sudden jump to open up 15 or 10M. That takes years ... or an M or X-class solar flare. The A-Index tells you what our geomagnetic field did
