A New Project Proposal

For the first part of the project I was aiming to replicate the results obtained last year during testing.

The diagram below shows a signal obtained from the equipment using this software.

The first part of the signal looks like it could be valid solar flare data.  However, when the signal levels in the area circled, are compared with a noise signal (shown below)  it is not certain whether real data is being measured or the system is just receiving noise.

The diagram above shows the noise floor signal obtained from the equipment when the antenna is unplugged.  As the y axis values show, the signal is close to the values seen for the noise signal. This indicates that the signal is weak.  There are a few different reasons why this may be the case which will now be explored.

The design is far from being optimal:

• The antenna may not be tuned correctly
• This will cause losses
• The radiation pattern may not be pointing skywards
• This will cause a weaker signal to be received
• The antenna may be receiving reflected signals from the roof
• The NASA recommended design is far too large for the department roof

The solution to these problems is to build a new antenna for the radio telescope with the aim of being able to obtain better quality signals using a Meanderline antenna.

A Meanderline antenna  works by having the same electrical length as a dipole antenna but reducing the overall size so that the antenna would not have to be 7 metres long but could be made smaller instead as shown in the diagram below.

Rather than use a 7 metre long dipole antenna as NASA suggest, in this project I will be investigating whether it is possible to use a Meanderline antenna.  The concept of Meanderline antennas is comparatively new so the simulations will help to validate the theory. 

Initial Testing

The equipment (shown below)  has been set up in the lab again and I have been testing the antenna.

The results from the Radio SkyPipe graphs I have seen look similar to those collected last year which is encouraging as the equipment is unchanged.  Below are some interesting patterns in the resulting graphs.

Continuing the Project

It has been decided that the project should continue for another year with the aim of being able to obtain more information.

As the group from last year have all now graduated, the project is being taken over by myself  (I'm Grace, a final year MEng student in electrical engineering and electronics).

Initially the aim is to replicate the results that the group saw last year myself and then to take the project further by either changing the design or to collect more data than last year and analyse it further.  One possible route for the project to follow is to use it to observe a pulsar.

A pulsar (portmanteau of pulsating star) is a highly magnetized, rotating neutron star that emits a beam of electromagnetic radiation  - from Wikipedia

Solar Storm - The Threat to Planet Earth

Here is a very interesting video broadcasted on BBC in March which is related to our project.

There is a new kind of weather to worry about, which comes from our nearest star, the sun.

Scientists are expecting a fit of violent activity on the sun which will propel billions of tonnes of superheated gas and pulses of energy towards our planet.

They have the power to close down our modern technological civilisation - e.g. in 1989, a solar storm cut off the power to the Canadian city of Quebec.

This video explained how solar burst happens and what the effect it will cause.

Courtesy by BBC Horizon: http://www.bbc.co.uk/i/b01d99vb/

16/Mar/2012 Record for Sun

The Chart above shows the data we have received from about 12 o'clock to 13:30. It is the best period for us to detect the solar burst in Liverpool.

During this process, we have got some classical wave forms for solar burst, which has been shown in the circles.

Type III Solar Burst

Rapidly drift from high to low frequencies. May exhibit harmonics.
Often accompany the flash phase of large flares.

The chart above was taken from the Winward Community College Jupiter Observatory receiver at 20.1 mHz on September 20, 2000. The times are local Hawaiian time so add 10 hours for UT. The burst is believed to be about 18 dB above the galactic background.

Type II Solar Burst

Slow drift from  high to slow frequencies.

The stripchart above was captured at the new Jupiter Observatory at Windward Community College on the Island of Oahu in Hawaii on July 28, 2000. The receiver is one of Dick Flagg's Jove Receivers attached to the standard in-phase version of the dual dipole Jove antenna. Primary beam pattern is to the zenith. The frequency is approximately 20.1 Mhz.