This post was originally produced as an Object of the Day for the Galaxy Zoo forum.
In this post I will be looking at three star systems that share a common theme, they are PSR B1620-26, Kepler-16 and Kepler-47 with the common tie being that all three systems are centred on a binary pair of stars – two stars orbiting one another.
Lets begin by taking a look at PSR B1620-26. The system is located 12400 light years away in the direction of the constellation Scorpius – The Scorpion – within the globular cluster M4. M4 is a reasonably loose association of stars that is around 75 light years across. M4 holds the honour of being the first globular cluster to have any of its component stars resolved into isolated objects. M4 is one of the brightest globular clusters in the sky located just west of the α Scorpii – Antares – taking up roughly as much space in the sky as the full moon.
The PSR B1620-26 is a highly evolved system containing both a white dwarf and a pulsar (spinning neutron star), indeed the system is estimated to be around 12.2 billion years old (compared to our own solar system which is estimated to be about 4.5 billion years old) potentially making it one of the oldest planet containing star systems in the Milky Way (or perhaps even the universe as a whole).
The planet (PSR B1620-26 b) orbits both stars making it a circumbinary planet. It was first announced in 1993 by a team that was studying the Doppler shifts of the system. At first they thought they were looking at a binary pulsar system (with the white dwarf being identified later) though their results showed that there was a third body within the system. When they calculated this unknown object’s mass they found that it was too small to be a star and thus identified it as a planet – one of the first outside our own solar system to be announced though official confirmation had to wait until 2000 (the first planets detected outside our own solar system orbit PSR B1257+12 – another pulsar).
PSR B1620-26 b is about two and a half times the mass of Jupiter and takes about a hundred years to orbit its parent stars.
The star system as a whole is thought to have had a rather unusual history that you can see documented in this NASA graphic.
The system’s pulsar is 1.35 solar masses and is rotating at about 100 times a second! The white dwarf is considerably less massive (0.35 solar masses) and the pair of stars orbit each other at an average distance of one AU.
The system faces an uncertain future, it is continuing its approach to the core of M4 and as it does so the density of stars surrounding the system will increase. Why is this so you may be thinking? A common way of thinking about globular clusters is that they are essentially self contained spheres of stars. Whilst this is broadly accurate, the stars are not spread evenly through the sphere. Stars are most densely clustered in the centre and become more widely spaced moving out.
As the surrounding area becomes more and more crowded the chances of a close encounter between two star systems also increases. Within the next billion or so years the system is very likely to have another such encounter with the most likely scenario being that the planet (as it is the least massive body in the system) being ejected into deep space fated to wander the stars alone.
Next lets continue with Kepler-16 (I should here note that if we are to follow the full naming convention, the system should be refereed to as Kepler-16 (AB) to show that we are taking about both stars though that is going to rapidly become tedious for everyone involved I shall keep to the shortened version and you can assume that I am referring to both stars when I don’t identify otherwise). Kepler-16 located 196 light years from Earth in the direction of the constellation Cygnus – The Swan.
The system is centred on two small, dim stars – The primary (16A) is an orange dwarf of spectral class KV. it is just 69% the mass of Sol and only a fraction of the brightness. It counterpart is even smaller at only a fifth the mass of Sol making it a MV class red dwarf.
The pair orbit one another in just 41 days and are separated by just 0.22AU – 22% of the average distance between the Earth and the Sun – which is smaller than Mercury’s orbit which sits between 0.31-0.47AU (the range is due to Mercury’s rather eccentric orbit).
Now to the planet itself Kepler-16 (AB) – b catchy isn’t it ::) so for brevity – 16b
16b is a gas giant a third of the mass of Jupiter and 3/4 its radius. This was the first circumbinary planet detected via the transit method – the reduction in the amount of light coming from the parent star as the planet passes in front of it as observed from Earth.
16b transits both of its systems stars, and they themselves transit each other, I admit that is more than slightly challenging to visualise so here is a visual representation with the two stars in the centre and 16b shown as a small blue\purple dot.
Our final system of the day – Kepler 47
This system has only recently had its planets confirmed by the team working on the Kepler mission and marks their first discovery of a multiple star system with more than one transiting planet.
The system can be found at a distance of 4900 light years from Earth in the direction of Cygnus. Both planets are circumbinary orbiting their parent stars. Both of which are smaller than the Sun with the secondary star just 1% as bright as Sol
The innermost planet (47b) orbits once every 50 days and would thus be much too hot for life as we know it to survive on. The outer planet (47c) orbits once every 303 days and this places it at the outer edge of the systems habitable zone. Life like ours is not expected to have developed on 47c as it is predicted to be a gas giant similar in size to Neptune, though perhaps one of its moons (if it has any!) could be suitable.
The most important aspect of the discovery is that it proves that multiple planet systems can indeed form around binary stars. Under current planetary formation models such systems are very difficult to form and suffer from stability issues throughout their existence. Furthermore, as at least one such planet is within its systems habitable zone it is evidence that such orbital configurations are potentially stable and thus the number of locations for life similar to our own to develop has just been increased!
For those interested you can read more about binary stars and the various types that exist from my post for the Young Astronomers – Binary Stars Blitzed.
It has been a month since anything has been posted on the blog and for that I am truly sorry.
All our editors have been busy with other matters for the last while, I for one am still getting settled into life at university, so as I’m sure you understand our attention has been focused elsewhere.
Hopefully we will be able to get some new content up soon, I for one will be aiming to get a post up sometime this weekend.
Thanks for staying with us!
The ESO has released a stunning image of the nebula NGC 2736 better known to many as the Pencil Nebula
The nebula is the brightest component of the much larger Vela supernova remnant, unsurprisingly centred on the Vela pulsar. The supernova that created the nebula occurred about 11000 years ago giving the resulting nebula plenty of time to expand and diffuse from the typical appearance of an SNR – a sphere of brightly glowing material.
The nebula is located about 815 light years from Earth in the direction of the southern constellation Vela – the sails.
The initial detonation of the star send the debris that now forms the nebula streaming away at several million kilometres an hour. During the extended time between the initial event and today the material has collided with other components of the interstellar medium – ISM – (the gas and dust found between the stars) slowing it considerably. Despite this the pencil nebula is still hurtling through space at 644,000 kilometres per hour!
The interaction between the nebula and the ISM has produced beautiful twists and folds within the nebula’s structure with the end result being the gorgeous spectacle we see today.
The nebula is about three quarters of a light year in length and was first documented by the British Astronomer John Herschel during his trip to the Cape of Good Hope in South Africa.
You can read more here
NASA’s Chandra X-ray Observatory (along with optical data provided by the ESO and infra-red data supplied by the Spitzer space telescope) has produced a truly amazing image of the star cluster NGC 1929 located within the nebula N44.
The nebula and its star cluster are located in the Milky Way’s largest satellite galaxy – the Large Magellanic Cloud (LMC) – at a distance of 160,000 light years from Earth - 940.6 quadrillion miles.
The star cluster is composed of primarily newborn stars that have only recently been forged from the surrounding material.A great number of these are many times the mass of the sun and produce a precipitous amount of hard radiation and vicious solar winds, before burning out in (on the time scales of the universe) sort order as supernovae generating incredible outpourings of energy.
These shockwaves along with the continual bombardment from radiation and particle stream gouges out massive ‘bubbles’ in the surrounding nebula. The x-ray data provided by Chandra (shown in blue) shows the regions of the nebula that are at the highest temperatures – the areas under the heaviest onslaught of radiation or reeling from one or more shockwaves . The cooler gas and dust as detected by Spitzer is displayed in red with the yellow regions show where the radiation is actually causing the surrounding material to glow in the visible range (this data was collected by the ESO’s Max-Planck telescope).
Astronomers have been having a problem with N44 and other similar ‘superbubbles’ in the LMC for sometime now – they are producing too many x-rays.
Before anyone panics, this is not a medical problem (we aren’t all going to suffer radiation poisoning thanks to a few over-active nebulae in another galaxy), it only refers to the measurements pointing to such nebulae producing more x-rays than could be explained using current knowledge – our knowledge of such objects must be incomplete.
A previous study had suggested that the shockwaves of supernovae impacting the bubble’s walls along with the evaporation of hot material from the sides of the bubble could perhaps explain this anomaly. This set of observations at least doesn’t find any supporting evidence for these ideas though it has been the first time that the observations have been sensitive to distinguish between these and other possibilities so progress is being made.
You can read more here
This post is part of the Young Astronomers Databank Project.
In the first part of this guide I looked at the basics of spectra with particular focus on black-body spectra. In this section I will take a look at a few specific emission features and what they can tell us about an object.
So lets begin our journey …
As each element and ion produces its own set of spectral lines scientists have created a standard notation of showing which line is produced by each atom or ion.
Any produced by an atom is labelled as – (x)I where (x) is the chemical symbol of the atom involved e.g. a line produced by the atom sulphur would be labelled as SI on a spectral chart.
As mentioned above ions also produce spectral lines. In astronomy we are nearly always dealing with positive ions (those which have had one or more electrons knocked off) even with those elements, that under normal circumstances on Earth, would take on additional electrons to become negative. This is because in astronomy where emission lines are produced the energies involved are much higher than on Earth and so it is much more likely that an electron (or perhaps two or even three) is knocked off rather than attracted towards the atom. As such ions with a positive are much more common in astronomy than those with a negative charge.
An ion with a +1 charge (one electron has been stripped off) produces lines labelled as (x)II with (x) again standing for the chemical symbol of the atom involved.
An ion with a +2 charge follows the same pattern – (x)III
and so the pattern continues
Let’s now look at two specific elements:
Hydrogen produces a series of emission lines that fall within the visible section of the electromagnetic spectrum (it also produces several others that lie outside the visible range). This set of lines is called the Balmer series after the scientist who first described them Johann Jakob Balmer.
They are all produced by electron transitions to the second energy level. When displayed using a hydrogen discharge tube (a cylinder of pure hydrogen through which an electric current is passed to excite the atoms) and a spectroscope the lines can be seen like so:
As is typical in science the rule we just learned about spectral notation doesn’t apply in this case.
For historical reasons the lines of atomic hydrogen in the visible region are named as H followed by a Greek letter. Hα is the lowest energy transition – red- moving through Hβ – which is a blue-green – and then Hγ, Hδ and Hε all being shades of purple (Hδ and Hε are sometimes classed as being ultraviolet rather than visible spectral features but still follow the same naming pattern).
Hydrogen Alpha – Hα
This emission feature occurs at 6562.8 Angstroms (656.28 nm). It is produced when an electron in a hydrogen atom decays from the third energy level to the second producing a photon with 1.9 eV (where one eV is 1.66×10-23 J) of energy.
Hα is a hallmark of star forming regions. It appears pink to the human eye (its the bright red line in the image above), and is displayed as such in most professionally produced images such as this one captured by the ESO’s MPG telescope of the Large Magellanic Cloud (LMC)
Hα is also a marker for AGN activity, with most such galaxies (including quasars) display strong Hα emission.
Oxygen is the third most common element in the Milky Way making up about 10,400 parts per million in terms of mass.
As oxygen has eight electrons rather than hydrogen’s solitary one, oxygen’s spectrum is much more complex with a great deal more lines than that of hydrogen ( hydrogen has 5 spectral lines between 4000-7000 Å (roughly the visible range) compared to oxygen’s 73! Using simplistic terms because oxygen has more electrons there are more available energy levels for those electrons to jump into, that in turn means more energy level transitions are possible and so giving rise to more spectral lines, as each line represents a possible transition.
The visible spectrum of oxygen looks like:
Doubly Ionised Oxygen – OIII
Another hallmark of star forming and active regions. A blue-green line that can be exceptionally intense in certain circumstances and can completely dominate the colour of some galaxies.
In most images containing OIII data it is displayed as either green or blue such as this Hubble image of the nearby active galaxy NGC 6822 (OIII is shown as green in this particular example)
In the next post in this series I will be taking a look at a few specific absorption features and what the colour of an object in general can reveal.
- The Worlds with Two Suns | The Young Astronomers on Binary Stars Blitzed – Updated
- Ed.A on Image of the Week – A Peculiar Pencil – 18/09/2012
- Saint on SS 433 – A Magnificent Microquasar
- SS 433 – A Magnificent Microquasar » The Young Astronomers on Binary Stars Blitzed – Updated
- John Fairweather on A Star’s Death Giving Life to a Monster – Recovered
TagsAGN Astronomy Astrophysics Big Bang Black Holes Cassini Chandra Curiosity Emission Nebulae ESA ESO Exoplanets Galaxies Gravity High Mass Stars HST Hubble Hubble Space Telescope Image of the Week Infra-red IOTW ISS Kepler Life LMC Mars NASA Nebula Nebulae Planets Russia Saturn Solar System Spacecraft Spitzer Starbirth Star death Star Formation Stars Star Sailor Podcast Supernova Supernovae VLT WISE Young Astronomers