Home: http://radioastronomybd.com

How To Build Your Own Sudden Ionospheric Disturbance Monitor:

http://www.radioastronomybd.com/sidvlf.html

This is the partial map (from Galactic Longitude 60° to 100°, where Latitude is 0°) of our Galaxy- Milky Way in Hydrogen line (21cm). The dots you are seeing in the map are the hydrogen clouds into the spiral arms of the Galaxy. I connected them with the lines to make visible the spiral pattern of our galaxy. The values contain, are the H-cloud position, actually the H-cloud distance to the galactic center. I did this observation using the SALSA Radio Telescope (2.3m) of Onsala, Sweden, which can be operated remotely from anywhere in the world.

When a meteor falls  it burns up due to the friction with the atmosphere and creates ionized trail. It has an effect on radio propagation. It may amplify the radio signals coming from a station. using this effect we can detect the passing meteors. To do this we need to tune the radio to a distant radio station that can’t be heard normally from our location. When a meteor passes through the transmitting and receiving station its ionized trail may amplify the station signal and make the propagation successful and at that time we will hear the station for a few second. If the ionized trail gets longer the receiving time will be longer.

My setup:

Receiver: The receiver is a Toyota car FM/AM radio. I tuned the radio at 90MHz.

Antenna: 3 element Yagi Uda.

The recorded audio file is here:

Perseid on 12 August,2011 ( this audio file contains the summery of 4 hours recoding)

The waveform is here:

Today morning at 03:57 UT  an M9.3 class solar flare event has occurred. It starts at 03:41 UT with a B class flare and ends at 04:04 UT with a M4.5 class flare.

At that time RRT has detected this Radio burst event. The noise storm starts at 03:19 UT with some small level noise rising and falling and it continues several minutes. From 03:50 UT the level rises to high for several seconds. At 03:55 UT the noise level starts a rapid rising to a great height which lasts till 04:03UT. The peak of the noise level is at 04:00 UT.

Here is the strip chart of this M9.3 class flare:

The spectrogram of the Noise storm is here:

Listen to the M9.3 class burst:

M9.3 Flare

The GOES 15 X-Ray Plot is here:

After the big one another small M class flare rises which starts noise storm from 04:31 UT and it continues with several C class events. The strip chart is below:

The Sun is producing continuous storms in several days. Today we face two M class flare and two C class flare eruption. Lots of activity!

The RRT  has detected some continuous pulsing storm events.

Today’s Strip charts are here:

Strip chart01: 02:46-03:07 UT

The peak of the noise level is at 02:51 UT. An M class flare produced the event.

Strip chart02: 03:09-10:04 UT

The first fringe  is the part of the previous M class flare(see chart01). The peak of this part is at 4:15 UT, which begins at 04:03 UT and ends at 04:43 UT

The second fringe’s origin is from a C class flare. The storm starts at 06:11 UT, ends at 07:31 UT and Peaks at 06:47 UT.

The spectrum of the C class flare is here:

Listen to the storm produced by the C class flare-

Solar radio burst on 03july,2011

The reference of GOES satellite X-ray plot from NOAA is here:

Radhagobinda  Radio Telescope has detected a continuous solar radio burst on August 02, 2011 at 06:09 UT. The origin of this burst is from sunspot 1261 which produce an M1.4 class solar flare. 1261 and 1263, both sunspots have Beta-gamma-delta magnetic field that may produce X class flare in future.

The strip chart of the Burst is here:

The spectrogram of the burst is here:

Listen to the burst-

Solar radio burst

Reference NOAA Solar X-Ray Plot:

This is the third graph (19july):

I changed the frequency to 79 MHz instead of 80MHz to avoid local interference. Antenna is 3 element Yagi-Uda. The graph shows a nice pattern. It’s almost similar to the first graph, the sunset effect and then a growing up of signal level.

Some steps that may take:

1. Increasing data logging time,

2.It’s important to include a Low noise preamplifier to get growing lobe/ fringe.

3.Including another antenna with a distant base line/like interferometer.