Friday, 30 July 2010

Note: Where links are inserted they are preceeded by a number. At the end of the article the link addresses are listed by number, for those who don't trust blind links.

Image above: The shockwave from supernova 1987a ploughs into the surrounding interstellar gas and dust, producing a spectactular lightshow. Such events can be sources of creation as well as destruction: Image courtesy of NASA.


A whirling chaos:
After millions of years cold serenity the pre-solar nebula has been shattered by the violent death of one of its children- A [1] blue giant star has exploded in a supernova: The shock wave has broken the nebula into fragments dense enough to begin contracting under their own gravity.

One of these fragments is us - everything you experience day to day, except the stars in the night sky, and all of humanity, will eventually emerge from that shrinking fragment of cloud.

This fragment of the pre-solar nebula has [2] internal currents and eddies (this link takes some reading through to get to the relavent bit, but its well worth it) - slow and cold by our terrestrial standards, but important for the next stage of its journey from cloud to star system. As the fragment contracts these eddies begin to change; as some cancel out and some reinforce each other the overall motion of the cloud averages out into a rotation in one direction. This spin is about to be one of the main forces shaping our solar systems formation.
When the nebula fragment is huge - 40,000,000,000,000, km or about the same distance to the suns nearest stellar neighbour proxima centauri- the overall rotation is barely perceptible, the temperature barely above absolute zero. As it contracts a little and begins to glow dully in the infrared the cloud is known as a [3] Bok globule. It is denser and slightly less frigid, yet otherwise seems little different than the pre-solar nebula that existed before - but already its fate is sealed.


Image above: Vast Bok globules, believed to shelter nascent star systems, float against the background of the Orion Nebula. Image courtesy of NASA.


As it contracts it begins to spin faster. If you’ve ever spun yourself around on an office chair to make yourself dizzy you may have encountered the same effect; spin with your legs sticking straight out then bring them up to your chest; your spin gets faster. This is known as [4] conservation of angular momentum.

At the same time the cloud is becoming much denser, and collisions between dust particles and gas particles are turning the momentum of the disk, both its rotation and collapse, into energy, pumping heat into the cloud. The dust is also feeling friction from the gas, which heats it in the [5] same process as a space-shuttle re-entering earth atmosphere goes through.

This heat is slowing the contraction; the core of the cloud is now dense enough to be opaque to infra red radiation. The heat being generated inside it is given off as infra red photons, which are trapped within the layers of gas and exert an outwards pressure that slows the inwards crush of gravity, and growth of the dark central knot of matter. The cloud reaches a temporary, slowly decaying equilibrium; self-gravity balanced imperfectly against thermal energy, with gravity prevailing little by little. This comparative quiet may last for a million years as the cloud slowly contracts. Astronomers know this stage as a [6] proto-stellar cloud.

But by the time the cloud has contracted to 200 astronomical units (1AU is the average distance between the sun and Earth, or 149 598 000 km) across it is whirling madly. Fast enough, in fact, that the cloud isn’t a cloud anymore; it’s a flat disk of spinning gas and dust, known as a proto-planetary disk, or [7] propyld for short. As the temperature of the central regions reaches 1000 degrees Kelvin the dust there begins to vaporize. The dust was making the cloud there opaque to radiation, which was slowing the collapse, so without it the radiation dissipates and the central regions collapse faster. Ironically this makes them heat more quickly!

Image above: Four protoplanetary disks (propylds) snapped by the Hubble. The coloured background is caused by the glow from the surrounding [8] Orion Nebula. Image courtesy of NASA.

Now in the centre of this cosmic maelstrom a knot of collapsing matter, still as wide across as the orbit of Jupiter, with a temperature of thousands of degrees kelvin, is gorging itself of the yolk of the Bok globule, and will consume around 98%of the original cloud fragments weight. This the proto-star phase, and it will endure for a hundred thousand years as the core temperature climbs steadily.

A collapse to glory:
The core temperature hits a catastrophic point : 10,000 degrees Kelvin. Events begin to unfold more rapidly: At this temperature the hydrogen gas converts to [9] plasma: the hydrogen atoms themselves are being broken apart. The heat energy that was slowing the contraction is suddenly being absorbed by this process. As with the supernova described in the first chapter, with no thermal energy supporting the cloud it implodes: the contraction becomes a runaway collapse, incredible amounts of hydrogen and helium come crashing down, and once the last of the hydrogen is ionised to plasma the temperature and pressure can climb as much in a few years as it would otherwise have done in eons. At the end of the collapse the core temperature exceeds 100,000 degrees kelvin, and naked hydrogen and helium nuclei seethe through a sea of free floating electrons. In just a few years, a mosquito's heartbeat astronomically, the cloud collapses from nearly a thousand million km diameter to ‘just’ a hundred million kilometres.

If you were hanging in space above the disk, around this time, you would see a huge circular ‘hole’ in the background stars, ill defined around its edges, and with a hellish red-maroon glow growing rapidly in its center. And if you were to fly across the radius of the maelstrom of gas and dust towards its edge you would find the edges flared, blocking the ember-red glow of the core as you crossed from one side of the disk to the other. Towering above the disk on both sides are beams of light. These are stellar, or [10] Herbig-Haro jets. These colossal beams are fountains of matter, weighing as much as twenty planet Earths, that has been broken down into a plasma, and then spat violently away from the poles of the growing star. Where the plasma cuts into the surrounding gas it excites it, forming vast glowing shockwaves.


Above: Images of four Herbig - Haro objects. In several of these both the jets and the protoplanetary disks of the nascent star systems can be seen. Image courtesy of astronomyonline.org


That growing glow where the beams meet, at the center of the disk, that marks the spot where an immense power for both creation and destruction is about to give it’s first bellow. Our sun is beginning to shine:

The proto-sun has shrunk down to roughly the size of Mercury's orbit today. Within it the contraction- slower again now- is still turning gravitational potential energy into heat, and crushing pressure. As a result the ‘star’ has begun to shine, despite it’s core still being too cool to produce fusion energy. This is known as the [11] T-Tauri phase, after the first of its kind to be discovered. The star is rarefied titan compared to the modern sun, it would fill the orbit of the planet mercury, but weighs the same and so is much less dense.

It is an immature, ill tempered, monster too; T-Tauri stars are large, fast spinning, and have immensely strong magnetic fields. The electrically conductive plasma, together with the stars fast rotation gives it a field that dwarfs even [12] the immense magnetic power of the modern sun.
[13] Gigantic sunspots blotch the surface, and herald the activity of immense flares that can increase the suns intensity tenfold for days at a time. The frigidly calm cathedral of gas and dust that was the pre-solar nebula has become an altar of unpredictable violence.
The magnetic field is what is feeding the growing sun now; the innermost material of the disk is carved off and funnelled down to the surface in great globules by the gargantuan field lines. But the T-Tauri sun has numbered its own days of growth: Immensely strong solar winds roar out from the surface, scorching and stripping the disk of lighter dust and gas, and chasing the remnants of the Bok globule into interstellar space. This wind is believed to be the cause of the jets; the disk of dust and gas around the star squeezes the wind out from the gaps over the poles.

Only one thing remains for our new sun: The T-Tauri sun is shining by heat from contraction- so to continue to shine it must still be contracting. But that will change. The core temperature is still rising, and when it eventually reaches ten million degrees Kelvin something magical will start to happen....

How do we know all this?

All the stages of stellar life are laid out in the night sky for us, but actually making sense of them is hampered by the timescale over which they live. For example, the smallest slowest burning red dwarfs have lifespans so long that it is impossible to tell how they die, as the universe hasn't been in existence long enough for one to pop its clogs!

The precise mechanisms behind the origins of stars like our sun are especially hard to investigate, as they hide themselves within the protective cocoon of the remaining bok globule material. This isn't just the cosmos inconveniencing us; the globule cocoon shields the growing proto-star from being disrupted by any more supernova explosions, or the intense winds from unstable nearby stars.
However there are some ways to probe inside the protective husks of gas and dust: [14] infrared telescopes can percieve the embryonic stars, as most of the radiation emitted by them until the hydrogen ionisation catastrophy is in these wavelengths. Useing infrared spectroscopy we can begin to build up an idea of what these objects are made of. [15]Radio and [16] microwave telescopes can probe the gasses surrounding them. Using this data, and with the help of computer modelling, astronomers can then piece together the timeline of a stars birth and where the various objects seen in star forming regions fit into it. Observatories in space, like the [17]Planck and[18] Herschel space telescopes, are a great help in this, as they are above the layers of earths atmosphere, that absorb much of the radiation we are interested in. We can also learn from samples of pre-solar and early solar nebular bought back to earth by missions like stardust. But as with all science, what we 'know' is simply a theory that happens to fit the facts and evidence we currentlyave. Tomorrow something could be found in the sky that turns all our deas on their heads....
Next : The long road to worlds of rock and gas.


List of links:
[1]http://www.universetoday.com/24587/blue-giant-star/
[2]http://www.lpi.usra.edu/books/MESSII/9005.pdf
[3]http://www.universetoday.com/2009/02/02/journey-inside-a-bok-globule/
[4]http://www.lightandmatter.com/html_books/2cl/ch05/ch05.html
[5]http://www.archive.org/stream/atmosphericfric00zahmgoog#page/n7/mode/1up
[6]http://cseligman.com/text/stars/starevol2.htm
[7]http://www.spacetelescope.org/news/heic0917/
[8]http://hubblesite.org/gallery/tours/tour-orion/
[9]http://www.plasmaphysics.org.uk/
[10]http://www.daviddarling.info/encyclopedia/H/Herbig-Haro_object.html
[11]http://hubpages.com/hub/The-T-Tauri-Star-and-T-Tauri-Star-Evolution
[12]http://solar.physics.montana.edu/ypop/Spotlight/Magnetic/
[13]http://arxiv.org/PS_cache/arxiv/pdf/0711/0711.2505v1.pdf
[14]http://www.americanscientist.org/issues/pub/protostars/4
[15]http://www.nrao.edu/index.php/learn/radioastronomy
[16]http://www.esa.int/esaMI/Planck/SEMTS20YUFF_0.html
[17]http://www.esa.int/esaMI/Planck/index.html
[18]http://www.esa.int/esaMI/Herschel/index.html

Monday, 19 July 2010

Above: The Orion nebula, one of the most active star forming regions in this part of the galaxy. our solar system was born in a similar nursery. Image courtesy of NASA.



Note: Where links are inserted they are preceeded by a number. At the end of the article the link addresses are listed by number, for those who don't trust blind links.

An alien beginning:
It may be a strange thought, but 5 billion years ago none of what you see out of your window was here. There was no sun, no planets, asteroids, no earth, no rock water or wind. If you were taken back to that time you would find yourself in the heart of a vast cathedral of gas and dust; a place that scientists today call ‘[1]the pre-solar nebula’. This nebula was a [2]giant molecular cloud, a place where stars and other objects are born.


The pre-solar nebula was made of incredibly thin gas, mainly hydrogen and helium and [3]dust particles as fine as smoke (Sizes of hundredths of a millimetre or less), which are known to scientists as pre-solar (literally; before the sun) grains. It may have stretched for over a hundred light-years in every direction before it began to birth stars.
This vast near-void contains the matter that will build our entire 6,070,000,000,000,000,000,000 metric ton solar system, and many more besides, yet at first you would probably see fairly little with your naked eye, except distant stars: the cloud is incredibly tenuous, like all nebula. It is so rarefied that a sample of it on earth would be a high quality vacuum ( its density is estimated at 10^6 particles per cubic centimetre- by comparison earths air at sea level has around 10^16 particles per centimeter). So there is not much to block the view of the stars. The milky way stretches unbroken across the field of view. There are no recognizable constellations; the stars have not yet moved into their familiar positions. The temperature is far below freezing, only tens of degrees above absolute zero.

The clear view may seem odd if you have followed some of the stunning images produced by telescopes. Nebula images often seen in the press are the result of [4]many hours of exposing very sensitive detectors to the nebula light, allowing extremely faint colours to be enhanced.

As your eyes adjust to the dark you might begin to make out some more details, things that would mark the view as different from that seen from clear space: denser knots of gas known as [5]Bok globules, visible as dark ‘holes’ against the background mark the spots where new stars are forming. If your eyes could see into the infra red they would apear to glow an ultra-deep maroon. A few intense points of blue-white light are scattered amongst the dimmer stars. These are the biggest, fastest burning stars to be birthed by the nebula; [6]blue supergiants. They are many times larger, heavier, brighter, and hotter than our sun, and their intense radiation excites the gasses of the nebula, causing it to glow with multicoloured light. From within the nebula these glows are too diffuse to be visible but if you were to navigate away from the cloud to a distance of a light years the view would become spectacular.




Above: The Tarantula Nebula - an aweseome sight from afar. Courtesy of NASA.


Importantly, for the next chapter, some of those blue white points I mentioned are already nearing the end of their lives....



The dust......

Pluck one of the grains of dust from its place in the cloud and examine it with modern instruments and it would tell you its own [7]unique story: It may have been born gently in the atmosphere of an elderly [8]red giant star, or forged violently in the death throes of a dying [9]supergiant. It may be an ancient grain, that has wandered for many billions of years, or it might be almost new, and buzzing with radiation from unstable short lived isotopes.

Grains are rich in ‘metals’ which to astrophysicists means any element heavier than carbon. Although the exact composition depends on the grains origin they are generally rich in oxygen, carbon, iron, silicon, and magnesium. In short the chemical elements that go into building dense rocky planets like earth, Venus, Mars and Mercury. Most grains are [10]born in the atmospheres of old giant stars, and these come in two broad catagories- oxygen rich and carbon rich. Oxygen rich stars will form [11]grains of rich in silicates. Carbon rich stars will form [12]grains rich in carbides, graphite, diamond and other carbon bearing materials.

The grains are not all simple lumps of one material. Many grains may have onion like layers- with cores of materials with high melting points like silicates, surrounded by layers of carbon rich materials, and then ‘ices’ - relatively volatile materials like water coating it in progressive layers of decreasing melting point.

The grains are the only solid material in the pre-solar nebula for light years in every direction- and [13]on the chemical level interesting things are happening with them. Although the temperature may be as low as 10 degrees Kelvin ( - 263 degrees Celsius) the grains are exposed to high energy cosmic rays, and ultraviolet light and other radiation from nearby stars in the nebula. They pick up gasses from the surrounding cloud, and are bombarded by stellar winds. These provide enough energy and material to power [14]chemical reactions on the grain surfaces. Where the grains are carbon rich the chemistry is especially interesting- [15]the chemical processes can form precursors to the chemistry behind life . Things like [16]amino acid precursors and polycyclic aromatic hydrocarbon chains have been identified in star forming regions observed from earth, and laboratory experiments have shown that [17]amino acids can form under ultra cold space conditions.
In these tiny grains are present not only the silicate materials to make a rocky surface, the volatiles to build atmospheres and even bodies of surface liquid, but the chemical precursors that go towards making life.

This is why the ancient nebula is such an intruiging place; almost everything yo can see out your window can trace its origins there.

How do we know this?

How do we know about this vanished place, which by our solid standards can barely be said to have been there at all?
There are remnants of the nebula itself. Pre-solar grains, believed to be representatives of the particle of dust in the nebular, have been [18]found in primitive meteorites and in micrometeorites. Some micro meteorites are particles small enough to drift gently through earths atmosphere without a fiery re-entry. These tiny particles can be collected by high altitude aircraft, or as surface deposits in pristine areas such as the Antarctic. There have been dust detectors flown on many space missions - and missions such as[19] Stardust have flown with [20]aerogel collectors to capture grains from comets, thought to contain pre-solar material.

In fact Earth gains almost 40 tons of extraterrestrial material a day. These tiny specks are survivors; they survived the collapse of the solar nebular, and many were incorperated into asteroid to moon sized worlds known as planitesimals (more on them later). The planitesimals were mostly destroyed during the later stages of the solar systems creation, but fragments of them have survived to this day as meteors, and where conditions are right [21]pre-solar grains can be identified by their isotopic signature and studied.
There are also pristine remnants of the pre-solar nebula still in interstellar space, and at the outer edge of our solar system- in near absolute zero deep freeze conditions well beyond the orbits of Neptune and Uranus. These can be studied using techniques such as [22]infra red spectroscopy. By these methods we can build up a picture of the composition of grains still floating between stars.

Still more [23]examples of pre-solar material are believed to be incorporated into comets, deep frozen agglomerations of dust and ice that linger by our solar systems edge, and occasionally come sunwards leading spectacular tails of evaporating ices and dust. The stardust mission mentioned above was sent to fly through the coma of a comet and collect samples of it.
A further source of clues are the star forming regions visible from earth today, such as the well known Orion nebula (pictured at the top). Observing nebula like these in detail we can see not only stars in various stages of forming within the nebula, but the evolution of the star forming nebula themselves.
From these clues we can begin of piece together a picture of what was here before the sun shone or the planets circled it.


Back to the utterly distant past:
At the solar nebular: one of the blue white points of light has used up its hydrogen fuel. It is now swollen into a red supergiant, using helium fuel. It runs out of helium, and begins fusing progressively heavier elements, carbon, oxygen, silicon and so on - which provided less and less energy as the atomic weight increases. Eventually, in the energy producing core, only an ‘ash’ of iron is left. Nuclear fusion with iron does not produe any energy, so the core stops producing energy. That energy was holding up the vast weight of the star- so the core collapses on itself. Unfathomable amounts of material crash inwards, heating violently as the core collides with itself and a monstorous blast wave heats the stars surface to 200,000 degrees Kelvin – a supernova explosion which shatters the outer layers of the star and smears them across space. The core is converted into a dense ball of neutrons.... but [24]it’s ultimate fate is another story ......
The supernova produces a shockwave that rolles out through the nebula, changing everything it hits forever.....


Links:
1:http://www.lpi.usra.edu/books/MESSII/9005.pdf
2:http://www.daviddarling.info/encyclopedia/G/giant_molecular_cloud.html
3:href="http://www.stecf.org/~ralbrech/amico/intabs/ottu.html
4:http://www.farnham-as.co.uk/2009/12/why-cant-i-see-fabulous-coloured-nebulae-with-my-telescope/
5:http://www.universetoday.com/2009/02/02/journey-inside-a-bok-globule/
6:www.universetoday.com/guide-to-space/stars/blue-supergiant-star/
7:http://rsta.royalsocietypublishing.org/content/359/1787/1961.full.pdf
8:http://www.astronomycafe.net/qadir/q2958.html
9:http://www.universetoday.com/guide-to-space/stars/supergiant-star/">[9]supergiant
10:http://www.lpi.usra.edu/books/MESSII/9020.pdf
11:http://www.lpi.usra.edu/meetings/lpsc2010/pdf/1431.pdf
12:http://www.dtm.ciw.edu/users/lrn/psgtypes.html
13:http://www.rsc.org/delivery/_ArticleLinking/DisplayArticleForFree.cfm?doi=a827315z&JournalCode=CS
14:http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=311259
15:http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=311259
16:href="http://www.mpifr-bonn.mpg.de/public/pr/pr-nitril-en.html
17:href="http://www.astrochem.org/sci/Amino_Acids.php
18:http://www.lpi.usra.edu/meetings/stardust2003/pdf/6037.pdf
19:http://stardust.jpl.nasa.gov/home/index.html
20:href="http://stardust.jpl.nasa.gov/tech/aerogel.html
21:http://www.lpi.usra.edu/meetings/lpsc2005/pdf/1630.pdf
22:http://www.ipac.caltech.edu/Outreach/Edu/Spectra/spec.html
23:http://www.astrobiology.com/news/viewpr.html?pid=28009
24:http://imagine.gsfc.nasa.gov/docs/science/know_l1/pulsars.html