We are rapidly approaching the end of another session of lectures and we hope that you have enjoyed the topics explored since last September. The Programme Secretary strives to cover as wide a spectrum as possible for subjects in the lecture programme but wishes to remind you that he is always open to suggestions for lecture subjects.
There are now only two meetings to come in this session. The final lecture of the session will be on Thursday May 17th at 8:15 pm, when Professor Richard Nelson (Queen Mary, University of London) will talk about: PLANETARY SYSTEMS IN THE GALAXY: ARCHITECTURE, FORMATION & EVOLUTION. And on the same subject, you might be interested in Peter Wallis's article that follows.
The final meeting on June 21st at 8:00 pm will be THE ANNUAL GENERAL MEETING and as usual will be preceded by wine & cheese and if time allows, followed by a scientific entertainment.
The agenda will include reports from officers and section leaders and the election of officers and five ordinary members of Council for the coming year. Council proposes the following:
|Secretary||Dr. Julie Atkinson|
|Treasurer & Membership Secretary||John Tennant|
|Programme Secretary||Jim Brightwell|
|Ordinary Members (max 5)||Martin Williams, Roger O'Brien, Peter Stern, Julia Daniels and Dr. Kevin Devine|
Council invites further nominations to the above posts. Such nominees shall be duly proposed and seconded and will have agreed to serve if elected.
Peter R. Wallis
Most of the known extrasolar planets, those in orbits around other stars than our Sun, have been discovered by two different methods. One method is to observe the small reduction in the parent star's light when the planet transits the star's disc. Obviously only a small proportion of planetary orbits will be orientated for this to occur. The reduction may be easy to see if the planet is large like Jupiter, but may be missed if it is small like the Earth or if it orbits at a large distance from the star.
The other method observes the frequency shift of known lines in the spectrum of the star as it "recoils" from the planet's revolution. Again, it will be easier to detect a massive planet like Jupiter, which has 318 times the mass of the Earth, particularly if it is close to its parent star where it has a greater orbital velocity.
These methods are consequently biased in favour of finding hot massive planets in close orbits. They are not likely to present much possibility of hosting extrasolar life – at least life as we know it.
There is however a third method based upon Einstein's General Theory of Relativity, published in 1916. This predicted, amongst other things, that light passing near a massive body, such as a star, will be deflected. Sir Arthur Eddington led an expedition a few years later to confirm this; it was necessary to use a solar eclipse as only then would it be possible to observe the altered position of stars seen close to the sun. There was another consequence of the theory which Einstein himself reported  in 1936. If two stars happen to lie in the same direction, one a long way away and the other nearer, the gravitational mass of the nearer star will bend the light from the more distant star and act like a lens. When the two stars are precisely aligned, the light of the further star will be magnified and appear as a bright ring around the nearer star: this is called an "Einstein Ring". If the stars are slightly misaligned the ring may be split or distorted. The phenomenon is called gravitational microlensing.
Now when we use lenses in a microscope or a telescope, we use them to magnify or study the distant object. But in stellar microlensing it is not the distant star we are studying: we use that merely as a point of light. Our interest here is in the structure of the gravitational mass which forms the lens. For example, if the lensing star has a planet, the Einstein ring will be further distorted. We are now able to compute the mass distribution from the observed distortion.
We can now use such microlensing to study the probability of planetary systems around the stars in our own galaxy, called the Milky Way. The advantage of the system is that it can detect planets over a wide range of orbital distances from the parent star, typically 0.5 to 10 AU, and at any orientation. A disadvantage is that microlensing events are rare. Perhaps only one in a million stars has a lensing event at any one time, but there are many stars. We cannot pick and choose, but we can reach a general conclusion. A recent paper  reports on the conclusions from 7 years of microlensing events seen in the Milky Way (2002-2007) and concludes that on the average, every star hosts one or more planets in an orbital distance range of 0.5 – 10AU and mass from a few times Earth to Jupiter and more. For those of us who are interested in the possibility of extraterrestrial and extrasolar life, this is an encouraging result.
But there is more. The microlensing technique has also been used to study galaxies, not stars . The lensing galaxy is an elliptical galaxy at red shift z=0.88 and is seen to have a bright Einstein ring. The background galaxy is at red shift z=2.06, imaged by the Keck telescope in Hawaii. The authors found that the distortion of the Einstein ring was caused by a dark satellite galaxy near the main lensing galaxy; it would not be possible to see it directly with current technology.
The objective of the authors in studying this lies in problems in understanding how galaxies form. The current theory is that galaxies form initially from dark matter and then they attract normal matter, which in due course coalesces into stars. But the theory seems to predict many more satellites around the Milky Way galaxy than we have yet found. So Vegetti and her team have demonstrated that it is possible to detect such elusive objects even at enormous distances where they could not possibly be seen visually. There is reason to think that such dark satellites are dominated by dark matter.
 Einstein, A "Lens-like action of a star by the deviation of light in the gravitational field" Science 84,506-7 (1936). Back
 Cassan, A et al "One or more bound planets per Milky Way star from microlensing observations", Nature 481, 167-169, 12 Jan. 2012. Back
 Vegetti,S et al,"Gravitational detection of a low-mass dark satellite galaxy at cosmological distance", Nature b>481, 341-343, 19 Jan. 2012. Back
 See also, 271-2, loc cit. Back
Just in case the conclusion reached by the authors in footnote 2 did not fully 'sink in', I should like to repeat it: "after 7 years of research using 'microlensing' techniques, the conclusion is that "every star hosts one or more planets". This is a profound piece of research and it has huge implications for the search for 'extra terrestrial life forms'. I have long held the view that if the present theories of star formation are correct, then it should be expected that the majority of galactic 'metal rich' population 1 stars ought to possess planetary systems. But then we learned that the first multiple planet system to be discovered was that surrounding a Pulsar: PSR 1257+12 – a most unlikely candidate for a planetary system. Recently, Kepler has discovered planets in orbit around the star KIC 05807617, a star that has passed the Red Giant phase – another unlikely candidate. All this adds considerable weight to this research which appears to push the boundaries even further by suggesting that 'every' star should host a planetary system. If this should prove to be correct, then in our own Galaxy alone there must be upwards of one hundred billion planetary systems, and in the observable Universe --- well, at the moment that's anyone's guess but it will be a lot!
For those of us interested in the existence of extraterrestrial and extra-solar life, Peter's observation that this is "an encouraging result" is something of an understatement! In a Universe consisting of billions of galaxies and trillions of stars and therefore by inference, trillions of planetary systems, the idea that just one planet orbiting an average star in an average galaxy could be the only abode of life is totally illogical and to quote the late Carl Sagan (Contact) it would seem to be "an awful waste of space".
Kepler's discoveries continue and recently it has detected a system containing two planets just 1.03 and 0.87 earth radii orbiting the G8 star Kepler-20. This system also contains previously detected planets of x2 and x3 earth radii. With diameters close to that of the Earth, Kepler 20e and Kepler 20f, could have similar compositions to Earth i.e. an iron core and silicate mantle, but at present an accurate determination of their masses has yet to be made and this determination will also indicate the chances of these planets possessing atmospheres and perhaps even liquid water.
Just two decades have passed since the first giant hot exoplanets were discovered. Now as our techniques become more refined we are beginning to detect the smaller rocky Earth sized planets and if the conclusions resulting from the technique of gravitational microlensing are correct, we can confidently expect to discover a whole lot more of them.
Those who attended last years' AGM and studied the Hon. Treasurer's financial report will have observed that we suffered an excess of expenditure over income. I regret to report that a similar state of affairs will occur this year. Clearly, we cannot allow this to continue. Venue rental, postage, printing, insurance premiums, the web site and other expenses have all increased in cost and to mitigate these rises Council have reluctantly decided that the Annual Subscription will have to rise from October 2012.
The new rates that will apply are as follows:
|Ordinary membership:||(cash) £15,||(standing order) £14|
|Family membership:||(cash) £23,||(standing order) £20|
|Junior membership: (students)||£5|
Those members who pay by standing order will need to contact their Banks to make the necessary arrangements.
Members can greatly assist the Hon. Treasurer's cash flow by paying their subscription promptly.
It is many years since it became necessary to raise the subscription and Council hopes that these new rates will allow us to remain in a healthy financial state for the foreseeable future. We believe that these new rates still represent excellent value for money in these troubled financial conditions and have been calculated to ensure that Junior members and students are the least affected.
Doug Daniels President.
Last updated 14-Jun-2012