Sirius Petroleum Share Discussion Threads

[quid for cash] 16/5/2015 10:57

Doc its shocking mate, they know full well the consequences of there actions even though some of them have become remote(I think wealth can do that to you)

Needs must they might say and we it seems we are merely collateral damage.

I am full of mottos and one of my favs is....Lets keeps our eyes on the prize.

Doc I love your rendition of I did it my way lol atb and maybe we will have a curry in the Rose of India day mate.MY TREAT.

[bronislav] 16/5/2015 10:56

I,ll try to make this my last post ,good post quid for cash and I do share the frustrations along with many others who are sitting on losses ....If I have come across as judging then that was not my intention....Everyone is in their rights to have a pop at the way we have been treated by the board ,in particular the imfo that leaves a lot to be desired ,there are lots of ways to vent our anger ,frustration disappointment but perhaps discussing bobo,s toilet habits are not the right way and as you say we haven't walked in bobo,s shoes....When this is all over I am sure we will smile when we look back at the twists and turns and hopefully this will make any rewards more the sweeter ...The quality of posters on the threads is at times top drawer and as I,ve mentioned before I am gratefull for their experience and knowledge that no doubt has taught and is still teaching me......hopefully we are clearer in the coming weeks on what the future holds and for me personally a big relief......Friday's buying may well signal a change in trading and the start of the release of imfo that will get this share price moving north.

[bronislav] 16/5/2015 09:57

Tucker....depends how we vent and why...no doubting share price is dire and in my book it's been manipulated and the top table have looked after themselves but it's them that set the company up and there is an argument to say good luck to them and would we do anything different ...We have to trust the board because if we don't trust them it's better for all of us to sell up,I have to believe that they will get it over the line and know what they are doing because the alternative affects us all and some have serious amounts of cash in here even though amounts are relative .....I think we will all know soon enough where Sirius is going,time is ticking on and hand over of governence is at hand .....perhaps it's the right time to give advfn a miss for me as it's all been said many times over with not much new to discuss ...best of luck mate.

[tuckerjenkins1] 16/5/2015 09:41

Broni, I don't think the board the has feed any one at moment???? more like the other way round. People invested here are fully justified to have vent.

[the drewster] 16/5/2015 08:57

Cannot quite believe how well the price is holding up. Calvert presumably selling heavily to get the money together for the next few tranches while the price holds

[thundercat1] 16/5/2015 08:11

Chronology of the universe
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(Redirected from History of universe)

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Diagram of Evolution of the universe from the Big Bang (left) - to the present.
Part of a series on
Physical cosmology
Full-sky image derived from nine years' WMAP data
Big Bang · Universe
Age of the universe
Chronology of the universe
Early universe[show]
Expansion · Future[show]
Components · Structure[show]
Experiments[show]
Scientists[show]
Subject history[show]
Category Category
Portal icon Cosmology portal
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v t e
External Timeline A graphical timeline is available at
Graphical timeline of the Big Bang
The chronology of the universe describes the history and future of the universe according to Big Bang cosmology, the prevailing scientific model of how the universe developed over time from the Planck epoch, using the cosmological time parameter of comoving coordinates. The model of the universe's expansion is known as the Big Bang. As of 2013, this expansion is estimated to have begun 13.798 ± 0.037 billion years ago.[1] It is convenient to divide the evolution of the universe so far into three phases.

Contents [hide]
1 Summary
2 Very early universe
2.1 Planck epoch
2.2 Grand unification epoch
2.3 Electroweak epoch
2.3.1 Inflationary epoch
2.3.2 Baryogenesis
3 Early universe
3.1 Supersymmetry breaking (speculative)
3.2 Electroweak symmetry breaking and the quark epoch
3.3 Hadron epoch
3.4 Lepton epoch
3.5 Photon epoch
3.5.1 Nucleosynthesis
3.5.2 Matter domination
3.5.3 Recombination
3.5.4 Habitable epoch
3.5.5 Dark Ages
4 Structure formation
4.1 Reionization
4.2 Formation of stars
4.3 Formation of galaxies
4.4 Formation of groups, clusters and superclusters
4.5 Formation of the Solar System
4.6 Today
5 Ultimate fate of the universe
5.1 Fate of the Solar System: 1 to 5 billion years
5.2 Big Rip: ≥20 billion years from now
5.3 Big Crunch: ≥102 billion years from now
5.4 Big Freeze: ≥105 billion years from now
5.5 Heat Death: 101000 years from now
5.6 Vacuum metastability event
6 See also
7 References
8 External links
Summary[edit]
In the first phase, the very earliest universe was so hot, or energetic, that initially no matter particles existed or could exist perhaps only fleetingly. According to prevailing scientific theories it was at this time that the forces we see around us today merged into one unified force. Space-time itself expanded during an inflationary epoch due to the immensity of the energies involved. Gradually the immense energies cooled – still to a temperature inconceivably hot compared to any we see around us now, but sufficiently to allow forces to gradually undergo symmetry breaking, a kind of repeated condensation from one status quo to another, leading finally to the separation of the strong force from the electroweak force and the first particles.


History of the Universe - gravitational waves are hypothesized to arise from cosmic inflation, a faster-than-light expansion just after the Big Bang (17 March 2014).[2][3][4]
In the second phase, this quark–gluon plasma universe then cooled further, the current fundamental forces we know take their present forms through further symmetry breaking – notably the breaking of electroweak symmetry – and the full range of complex and composite particles we see around us today became possible, leading to a gravitationally dominated universe, the first neutral atoms (~ 80% hydrogen), and the cosmic microwave background radiation we can detect today. Modern high energy particle physics theories are satisfactory at these energy levels, and so physicists believe they have a good understanding of this and subsequent development of the fundamental universe around us. Because of these changes, space had also become largely transparent to light and other electromagnetic energy, rather than "foggy", by the end of this phase.

The third phase started after a short dark age with a universe whose fundamental particles and forces were as we know them, and witnessed the emergence of large scale stable structures, such as the earliest stars, quasars, galaxies, clusters of galaxies and superclusters, and the development of these to create the kind of universe we see today. Some researchers call the development of all this physical structure over billions of years "cosmic evolution". Other, more interdisciplinary, researchers refer to "cosmic evolution" as the entire scenario of growing complexity from big bang to humankind, thereby incorporating biology and culture into a grand unified view of all complex systems in the universe to date.[5]

Beyond the present day, scientists anticipate that the Earth will cease to be able to support life in about a billion years, and will be drawn into the Sun in about 5 billion years. On a far longer timescale, the Stelliferous Era will end as stars eventually die and fewer are born to replace them, leading to a darkening universe. Various theories suggest a number of subsequent possibilities. If particles such as protons are unstable then eventually matter may evaporate into low level energy in a kind of entropy related heat death. Alternatively the universe may collapse in a big crunch, although current data shows the rate of expansion is still increasing. If this is correct then it may end in a "big freeze" as matter and energy become very thinly spread and cool down. Alternative suggestions include a false vacuum catastrophe or a Big Rip as possible ends to the universe.

Very early universe[edit]
All ideas concerning the very early universe (cosmogony) are speculative. No accelerator experiments have yet probed energies of sufficient magnitude to provide any experimental insight into the behavior of matter at the energy levels that prevailed during this period. Proposed scenarios differ radically. Some examples are the Hartle–Hawking initial state, string landscape, brane inflation, string gas cosmology, and the ekpyrotic universe. Some of these are mutually compatible, while others are not.

Planck epoch[edit]
0 to 10−43 second after the Big Bang
Main article: Planck epoch
The Planck epoch is an era in traditional (non-inflationary) big bang cosmology wherein the temperature was so high that the four fundamental forces—electromagnetism, gravitation, weak nuclear interaction, and strong nuclear interaction—were one fundamental force. Little is understood about physics at this temperature; different hypotheses propose different scenarios. Traditional big bang cosmology predicts a gravitational singularity before this time, but this theory relies on general relativity and is expected to break down due to quantum effects.

In inflationary cosmology, times before the end of inflation (roughly 10−32 second after the Big Bang) do not follow the traditional big bang timeline.

Grand unification epoch[edit]
Between 10−43 second and 10−36 second after the Big Bang[6]
Main article: Grand unification epoch
As the universe expanded and cooled, it crossed transition temperatures at which forces separate from each other. These are phase transitions much like condensation and freezing. The grand unification epoch began when gravitation separated from the other forces of nature, which are collectively known as gauge forces. The non-gravitational physics in this epoch would be described by a so-called grand unified theory (GUT). The grand unification epoch ended when the GUT forces further separate into the strong and electroweak forces.

Electroweak epoch[edit]
Between 10−36 second (or the end of inflation) and 10−32 second after the Big Bang[6]
Main article: Electroweak epoch
According to traditional big bang cosmology, the Electroweak epoch began 10−36 second after the Big Bang, when the temperature of the universe was low enough (1028 K) to separate the strong force from the electroweak force (the name for the unified forces of electromagnetism and the weak interaction). In inflationary cosmology, the electroweak epoch ends when the inflationary epoch begins, at roughly 10−32 second.

Inflationary epoch[edit]
Unknown duration, ending 10−32(?) second after the Big Bang
Main article: Inflationary epoch
Cosmic inflation was an era of accelerating expansion produced by a hypothesized field called the inflaton, which would have properties similar to the Higgs field and dark energy. While decelerating expansion would magnify deviations from homogeneity, making the universe more chaotic, accelerating expansion would make the universe more homogeneous. A sufficiently long period of inflationary expansion in our past could explain the high degree of homogeneity that is observed in the universe today at large scales, even if the state of the universe before inflation was highly disordered.

Inflation ended when the inflaton field decayed into ordinary particles in a process called "reheating", at which point ordinary Big Bang expansion began. The time of reheating is usually quoted as a time "after the Big Bang". This refers to the time that would have passed in traditional (non-inflationary) cosmology between the Big Bang singularity and the universe dropping to the same temperature that was produced by reheating, even though, in inflationary cosmology, the traditional Big Bang did not occur.

According to the simplest inflationary models, inflation ended at a temperature corresponding to roughly 10−32 second after the Big Bang. As explained above, this does not imply that the inflationary era lasted less than 10−32 second. In fact, in order to explain the observed homogeneity of the universe, the duration must be longer than 10−32 second. In inflationary cosmology, the earliest meaningful time "after the Big Bang" is the time of the end of inflation.

On March 17, 2014, astrophysicists of the BICEP2 collaboration announced the detection of inflationary gravitational waves in the B-mode power spectrum which was interpreted as clear experimental evidence for the theory of inflation.[2][3][4][7][8][9] However, on June 19, 2014, lowered confidence in confirming the cosmic inflation findings was reported [8][10][11] and finally, on February 2, 2015, a joint analysis of data from BICEP2/Keck and Planck satellite concluded that the statistical “significance [of the data] is too low to be interpreted as a detection of primordial B-modes” and can be attributed mainly to polarized dust in the Milky Way.[12][13][14][15]

Baryogenesis[edit]
Main article: Baryogenesis
There is currently insufficient observational evidence to explain why the universe contains far more baryons than antibaryons. A candidate explanation for this phenomenon must allow the Sakharov conditions to be satisfied at some time after the end of cosmological inflation. While particle physics suggests asymmetries under which these conditions are met, these asymmetries are too small empirically to account for the observed baryon-antibaryon asymmetry of the universe.

Early universe[edit]

Cosmic History
After cosmic inflation ends, the universe is filled with a quark–gluon plasma. From this point onwards the physics of the early universe is better understood, and less speculative.

Supersymmetry breaking (speculative)[edit]
Main article: Supersymmetry breaking
If supersymmetry is a property of our universe, then it must be broken at an energy that is no lower than 1 TeV, the electroweak symmetry scale. The masses of particles and their superpartners would then no longer be equal, which could explain why no superpartners of known particles have ever been observed.

Electroweak symmetry breaking and the quark epoch[edit]
Between 10−12 second and 10−6 second after the Big Bang
Main articles: Electroweak symmetry breaking and Quark epoch
As the universe's temperature falls below a certain very high energy level, it is believed that the Higgs field spontaneously acquires a vacuum expectation value, which breaks electroweak gauge symmetry. This has two related effects:

The weak force and electromagnetic force, and their respective bosons (the W and Z bosons and photon) manifest differently in the present universe, with different ranges;
Via the Higgs mechanism, all elementary particles interacting with the Higgs field become massive, having been massless at higher energy levels.
At the end of this epoch, the fundamental interactions of gravitation, electromagnetism, the strong interaction and the weak interaction have now taken their present forms, and fundamental particles have mass, but the temperature of the universe is still too high to allow quarks to bind together to form hadrons.

Hadron epoch[edit]
Between 10−6 second and 1 second after the Big Bang
Main article: Hadron epoch
The quark–gluon plasma that composes the universe cools until hadrons, including baryons such as protons and neutrons, can form. At approximately 1 second after the Big Bang neutrinos decouple and begin traveling freely through space. This cosmic neutrino background, while unlikely to ever be observed in detail since the neutrino energies are very low, is analogous to the cosmic microwave background that was emitted much later. (See above regarding the quark–gluon plasma, under the String Theory epoch.) However, there is strong indirect evidence that the cosmic neutrino background exists, both from Big Bang nucleosynthesis predictions of the helium abundance, and from anisotropies in the cosmic microwave background

Lepton epoch[edit]
Between 1 second and 10 seconds after the Big Bang
Main article: Lepton epoch
The majority of hadrons and anti-hadrons annihilate each other at the end of the hadron epoch, leaving leptons and anti-leptons dominating the mass of the universe. Approximately 10 seconds after the Big Bang the temperature of the universe falls to the point at which new lepton/anti-lepton pairs are no longer created and most leptons and anti-leptons are eliminated in annihilation reactions, leaving a small residue of leptons.[16]

Photon epoch[edit]
Between 10 seconds and 380,000 years after the Big Bang
Main article: Photon epoch
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by photons. These photons are still interacting frequently with charged protons, electrons and (eventually) nuclei, and continue to do so for the next 380,000 years.

Nucleosynthesis[edit]
Between 3 minutes and 20 minutes after the Big Bang[17]
Main article: Big Bang nucleosynthesis
During the photon epoch the temperature of the universe falls to the point where atomic nuclei can begin to form. Protons (hydrogen ions) and neutrons begin to combine into atomic nuclei in the process of nuclear fusion. Free neutrons combine with protons to form deuterium. Deuterium rapidly fuses into helium-4. Nucleosynthesis only lasts for about seventeen minutes, since the temperature and density of the universe has fallen to the point where nuclear fusion cannot continue. By this time, all neutrons have been incorporated into helium nuclei. This leaves about three times more hydrogen than helium-4 (by mass) and only trace quantities of other light nuclei.

Matter domination[edit]
70,000 years after the Big Bang
At this time, the densities of non-relativistic matter (atomic nuclei) and relativistic radiation (photons) are equal. The Jeans length, which determines the smallest structures that can form (due to competition between gravitational attraction and pressure effects), begins to fall and perturbations, instead of being wiped out by free-streaming radiation, can begin to grow in amplitude.

According to ΛCDM, at this stage, cold dark matter dominates, paving the way for gravitational collapse to amplify the tiny inhomogeneities left by cosmic inflation, making dense regions denser and rarefied regions more rarefied. However, because present theories as to the nature of dark matter are inconclusive, there is as yet no consensus as to its origin at earlier times, as currently exist for baryonic matter.

Recombination[edit]
ca. 377,000 years after the Big Bang
Main article: Recombination (cosmology)

9 year WMAP data (2012) shows the cosmic microwave background radiation variations throughout the universe from our perspective, though the actual variations are much smoother than the diagram suggests.[18][19]
Hydrogen and helium atoms begin to form as the density of the universe falls. This is thought to have occurred about 377,000 years after the Big Bang.[20] Hydrogen and helium are at the beginning ionized, i.e., no electrons are bound to the nuclei, which (containing positively charged protons) are therefore electrically charged (+1 and +2 respectively). As the universe cools down, the electrons get captured by the ions, forming electrically neutral atoms. This process is relatively fast (and faster for the helium than for the hydrogen), and is known as recombination.[21] At the end of recombination, most of the protons in the universe are bound up in neutral atoms. Therefore, the photons' mean free path becomes effectively infinite and the photons can now travel freely (see Thomson scattering): the universe has become transparent. This cosmic event is usually referred to as decoupling.

The photons present at the time of decoupling are the same photons that we see in the cosmic microwave background (CMB) radiation, after being greatly cooled by the expansion of the universe. Around the same time, existing pressure waves within the electron-baryon plasma — known as baryon acoustic oscillations — became embedded in the distribution of matter as it condensed, giving rise to a very slight preference in distribution of large scale objects. Therefore the cosmic microwave background is a picture of the universe at the end of this epoch including the tiny fluctuations generated during inflation (see diagram), and the spread of objects such as galaxies in the universe is an indication of the scale and size of the universe as it developed over time.[22]

Habitable epoch[edit]
See also: Abiogenesis
The chemistry of life may have begun shortly after the Big Bang, 13.8 billion years ago, during a habitable epoch when the Universe was only 10-17 million years old.[23][24][25]

Dark Ages[edit]
See also: Hydrogen line
Before decoupling occurred, most of the photons in the universe were interacting with electrons and protons in the photon–baryon fluid. The universe was opaque or "foggy" as a result. There was light but not light we can now observe through telescopes. The baryonic matter in the universe consisted of ionized plasma, and it only became neutral when it gained free electrons during "recombination", thereby releasing the photons creating the CMB. When the photons were released (or decoupled) the universe became transparent. At this point the only radiation emitted was the 21 cm spin line of neutral hydrogen. There is currently an observational effort underway to detect this faint radiation, as it is in principle an even more powerful tool than the cosmic microwave background for studying the early universe. The Dark Ages are currently thought to have lasted between 150 million to 800 million years after the Big Bang. The October 2010 discovery of UDFy-38135539, the first observed galaxy to have existed during the following reionization epoch, gives us a window into these times. The galaxy earliest in this period observed and thus also the most distant galaxy ever observed is currently on the record of Leiden University's Richard J. Bouwens and Garth D. Illingsworth from UC Observatories/Lick Observatory. They found the galaxy UDFj-39546284 to be at a time some 480 million years after the Big Bang or about halfway through the Cosmic Dark Ages at a distance of about 13.2 billion light-years. More recently, the UDFj-39546284 galaxy was found to be around "380 million years" after the Big Bang and at a distance of 13.37 billion light-years.[26]

Structure formation[edit]
See also: Large-scale structure of the cosmos and Structure formation

The Hubble Ultra Deep Fields often showcase galaxies from an ancient era that tell us what the early Stelliferous Age was like.

Another Hubble image shows an infant galaxy forming nearby, which means this happened very recently on the cosmological timescale. This shows that new galaxy formation in the universe is still occurring.
Structure formation in the big bang model proceeds hierarchically, with smaller structures forming before larger ones. The first structures to form are quasars, which are thought to be bright, early active galaxies, and population III stars. Before this epoch, the evolution of the universe could be understood through linear cosmological perturbation theory: that is, all structures could be understood as small deviations from a perfect homogeneous universe. This is computationally relatively easy to study. At this point non-linear structures begin to form, and the computational problem becomes much more difficult, involving, for example, N-body simulations with billions of particles.

Reionization[edit]
150 million to 1 billion years after the Big Bang
See also: Reionization and 21 centimeter radiation
The first stars and quasars form from gravitational collapse. The intense radiation they emit reionizes the surrounding universe. From this point on, most of the universe is composed of plasma.

Formation of stars[edit]
See also: Star formation
The first stars, most likely Population III stars, form and start the process of turning the light elements that were formed in the Big Bang (hydrogen, helium and lithium) into heavier elements. However, as yet there have been no observed Population III stars, and understanding of them is currently based on computational models of their formation and evolution. Fortunately observations of the Cosmic Microwave Background radiation can be used to date when star formation began in earnest. Analysis of such observations made by the European Space Agency's Planck telescope, as reported by BBC News in early February, 2015, concludes that the first generation of stars lit up 560 million years after the Big Bang. [27] [28]

Formation of galaxies[edit]
See also: Galaxy formation and evolution
Large volumes of matter collapse to form a galaxy. Population II stars are formed early on in this process, with Population I stars formed later.

Johannes Schedler's project has identified a quasar CFHQS 1641+3755 at 12.7 billion light-years away,[29] when the universe was just 7% of its present age.

On July 11, 2007, using the 10-metre Keck II telescope on Mauna Kea, Richard Ellis of the California Institute of Technology at Pasadena and his team found six star forming galaxies about 13.2 billion light years away and therefore created when the universe was only 500 million years old.[30] Only about 10 of these extremely early objects are currently known.[31] More recent observations have shown these ages to be shorter than previously indicated. The most distant galaxy observed as of October 2013 has been reported to be 13.1 billion light years away.[32]

The Hubble Ultra Deep Field shows a number of small galaxies merging to form larger ones, at 13 billion light years, when the universe was only 5% its current age.[33] This age estimate is now believed to be slightly shorter.[32]

Based upon the emerging science of nucleocosmochronology, the Galactic thin disk of the Milky Way is estimated to have been formed 8.8 ± 1.7 billion years ago.[34]

Formation of groups, clusters and superclusters[edit]
See also: Large-scale structure of the cosmos
Gravitational attraction pulls galaxies towards each other to form groups, clusters and superclusters.

Formation of the Solar System[edit]
9 billion years after the Big Bang
Main article: Formation and evolution of the Solar System
The Solar System began forming about 4.6 billion years ago, or about 9 billion years after the Big Bang. A fragment of a molecular cloud made mostly of hydrogen and traces of other elements began to collapse, forming a large sphere in the center which would become the Sun, as well as a surrounding disk. The surrounding accretion disk would coalesce into a multitude of smaller objects that would become planets, asteroids, and comets. The Sun is a late-generation star, and the Solar System incorporates matter created by previous generations of stars.

Today[edit]
13.8 billion years after the Big Bang
The Big Bang is estimated to have occurred about 13.8 billion years ago.[35] Since the expansion of the universe appears to be accelerating, its large-scale structure is likely to be the largest structure that will ever form in the universe. The present accelerated expansion prevents any more inflationary structures entering the horizon and prevents new gravitationally bound structures from forming.

Ultimate fate of the universe[edit]
Main article: Ultimate fate of the universe
As with interpretations of what happened in the very early universe, advances in fundamental physics are required before it will be possible to know the ultimate fate of the universe with any certainty. Below are some of the main possibilities.

Fate of the Solar System: 1 to 5 billion years[edit]
Main articles: Formation and evolution of the Solar System § Future, Stability of the Solar System, Future of the Earth § Solar evolution and Red giant § The Sun as a red giant

Relative size of our Sun as it is now (inset) compared to its estimated future size as a red giant
Over a timescale of a billion years or more, the Earth and Solar System are unstable. Earth's existing biosphere is expected to vanish in about a billion years, as the Sun's heat production gradually increases to the point that liquid water and life are unlikely;[36] the Earth's magnetic fields, axial tilt and atmosphere are subject to long term change; and the Solar System itself is chaotic over million- and billion-year timescales;[37] Eventually in around 5.4 billion years from now, the core of the Sun will become hot enough to trigger hydrogen fusion in its surrounding shell.[36] This will cause the outer layers of the star to expand greatly, and the star will enter a phase of its life in which it is called a red giant.[38][39] Within 7.5 billion years, the Sun will have expanded to a radius of 1.2 AU—256 times its current size, and studies announced in 2008 show that due to tidal interaction between Sun and Earth, Earth would actually fall back into a lower orbit, and get engulfed and incorporated inside the Sun before the Sun reaches its largest size, despite the Sun losing about 38% of its mass.[40] The Sun itself will continue to exist for many billions of years, passing through a number of phases, and eventually ending up as a long-lived white dwarf. Eventually, after billions more years, the Sun will finally cease to shine altogether, becoming a black dwarf.[41]

Big Rip: ≥20 billion years from now[edit]
See also: Big Rip
This scenario is possible only if the energy density of dark energy actually increases without limit over time.[citation needed] Such dark energy is called phantom energy and is unlike any known kind of energy. In this case, the expansion rate of the universe will increase without limit. Gravitationally bound systems, such as clusters of galaxies, galaxies, and ultimately the Solar System will be torn apart. Eventually the expansion will be so rapid as to overcome the electromagnetic forces holding molecules and atoms together. Finally even atomic nuclei will be torn apart and the universe as we know it will end in an unusual kind of gravitational singularity. At the time of this singularity, the expansion rate of the universe will reach infinity, so that any and all forces (no matter how strong) that hold composite objects together (no matter how closely) will be overcome by this expansion, literally tearing everything apart.

Big Crunch: ≥102 billion years from now[edit]
See also: Big Crunch
If the energy density of dark energy were negative or the universe were closed, then it would be possible that the expansion of the universe would reverse and the universe would contract towards a hot, dense state. This is a required element of oscillatory universe scenarios, such as the cyclic model, although a Big Crunch does not necessarily imply an oscillatory universe. Current observations suggest that this model of the universe is unlikely to be correct, and the expansion will continue or even accelerate.

Big Freeze: ≥105 billion years from now[edit]
Main articles: Future of an expanding universe and Heat death of the universe
This scenario is generally considered to be the most likely,[citation needed] as it occurs if the universe continues expanding as it has been. Over a time scale on the order of 1014 years or less, existing stars burn out, stars cease to be created, and the universe goes dark.[42], §IID. Over a much longer time scale in the eras following this, the galaxy evaporates as the stellar remnants comprising it escape into space, and black holes evaporate via Hawking radiation.[42], §III, §IVG. In some grand unified theories, proton decay after at least 1034 years will convert the remaining interstellar gas and stellar remnants into leptons (such as positrons and electrons) and photons. Some positrons and electrons will then recombine into photons.[42], §IV, §VF. In this case, the universe has reached a high-entropy state consisting of a bath of particles and low-energy radiation. It is not known however whether it eventually achieves thermodynamic equilibrium.[42], §VIB, VID.

Heat Death: 101000 years from now[edit]
See also: Heat death of the universe
The heat death is a possible final state of the universe, estimated at after 101000 years, in which it has "run down" to a state of no thermodynamic free energy to sustain motion or life. In physical terms, it has reached maximum entropy (because of this, the term "entropy" has often been confused with Heat Death, to the point of entropy being labelled as the "force killing the universe"). The hypothesis of a universal heat death stems from the 1850s ideas of William Thomson (Lord Kelvin)[43] who extrapolated the theory of heat views of mechanical energy loss in nature, as embodied in the first two laws of thermodynamics, to universal operation.

Vacuum metastability event[edit]
See also: False vacuum
If our universe is in a very long-lived false vacuum, it is possible that a small region of the universe will tunnel into a lower energy state (see Bubble nucleation). If this happens, all structures within will be destroyed instantaneously and the region will expand at near light speed, bringing destruction without any forewarning.

See also[edit]
Portal icon Cosmology portal
Cosmic Calendar (age of universe scaled to a single year)
Cyclic model
Dark-energy-dominated era
Dyson's eternal intelligence
Entropy (arrow of time)
Graphical timeline from Big Bang to Heat Death
Graphical timeline of the Big Bang
Graphical timeline of the Stelliferous Era
Illustris project
Matter-dominated era
Radiation-dominated era
Timeline of the far future
Ultimate fate of the universe
References[edit]
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^ Jump up to: a b Staff (17 March 2014). "BICEP2 2014 Results Release". National Science Foundation. Retrieved 18 March 2014.
^ Jump up to: a b Clavin, Whitney (17 March 2014). "NASA Technology Views Birth of the Universe". NASA. Retrieved 17 March 2014.
^ Jump up to: a b Overbye, Dennis (17 March 2014). "Detection of Waves in Space Buttresses Landmark Theory of Big Bang". The New York Times. Retrieved 17 March 2014.
Jump up ^ Chaisson, E., (2001). Cosmic Evolution: The Rise of Complexity in Nature, Harvard University Press, ISBN 0-674-00987-8; see also Cosmic Evolution
^ Jump up to: a b Ryden B: "Introduction to Cosmology", pg. 196 Addison-Wesley 2003
Jump up ^ Overbye, Dennis (March 24, 2014). "Ripples From the Big Bang". New York Times. Retrieved March 24, 2014.
^ Jump up to: a b Ade, P.A.R. (BICEP2 Collaboration) et al. (June 19, 2014). "Detection of B-Mode Polarization at Degree Angular Scales by BICEP2" (PDF). Physical Review Letters 112: 241101. arXiv:1403.3985. Bibcode:2014PhRvL.112x1101A. doi:10.1103/PhysRevLett.112.241101. PMID 24996078. Retrieved June 20, 2014.
Jump up ^ hxxp://www.math.columbia.edu/~woit/wordpress/?p=6865
Jump up ^ Overbye, Dennis (June 19, 2014). "Astronomers Hedge on Big Bang Detection Claim". New York Times. Retrieved June 20, 2014.
Jump up ^ Amos, Jonathan (June 19, 2014). "Cosmic inflation: Confidence lowered for Big Bang signal". BBC News. Retrieved June 20, 2014.
Jump up ^ BICEP2/Keck, Planck Collaborations (2015). "A Joint Analysis of BICEP2/Keck Array and Planck Data (Provisionally accepted by PRL)". arXiv. arXiv:1502.00612v1. Retrieved 13 February 2015.
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Exploring Time from Planck time to the lifespan of the Universe
Cosmic Evolution is a multi-media web site that explores the cosmic-evolutionary scenario from big bang to humankind.
Astronomers' first detailed hint of what was going on less than a trillionth of a second after time began
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Sean Carroll on the arrow of time (Part 1), The origin of the universe and the arrow of time, Sean Carroll, video, CHAST 2009, Templeton, Faculty of science, University of Sydney, November 2009, TED.com
A Universe From Nothing, video, Lawrence Krauss, AAI 2009, YouTube.com
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Cosmic Evolution through Time - an interactive timeline explains the main events in the history of our Universe

[bronislav] 16/5/2015 07:23

I,m not having a go at Chris but just possibly board members could be looking in and we want the board on our side .We all want the same result here and Sirius coming off would change all our lives so perhaps not worth rocking the boards boat ....If we have another AGM then that would be a good place to vent our frustrations .....enjoy the weekend folks .....

[topgun1000] 16/5/2015 07:18

With people down thousands of pounds now on here its time to get some answers and have some serious debate, posting complete nonsense is of no help and doesnt look good to new investors who may read these boards.
I for one am considering a visit to the agm this year if there is one and i'm not over seas with work, it would be nice to get some real answers face to face as to why my holding has been decimated along with a lot of others who are heavily invested here.

[sherl0ck] 16/5/2015 06:55

Whatever happened to F13ldstone? I used to enjoy his insights and debate on here and LSE, and think he had a pretty sizeable holding at one point. He still occasionally posts about WRN but nothing on Sirius for months.....maybe he's just had enough and sold up by now. No more sightings & smiley faces from Adoc since the last RNS either.

C'mon guys - if you still peruse here from time to time and continue to hold some SRSP shares, your thoughts, ideas & concerns would be most welcome, especially after recent developments.

[chris shiherlis] 16/5/2015 06:42

The only pathetic thing here is you, never trust a man with long hair.

How would it bite back I would be interested to know?

You have no idea what I have in the bank so keep your mouth shut.

[bronislav] 16/5/2015 06:38

chris .......if anyone was in any doubt that you are the same avatar as rich 80 last nights pathetic posts takes away any doubts .....pointless having a go at the board because reality is they are your only hope of a few quid in the bank ,my theory is don't bite the hand that could very likely feed you or it might bite you back.

[thundercat1] 16/5/2015 06:35

I enjoyed the meeting video ten hours or nothing I stayed up all night watching that.

[thundercat1] 16/5/2015 06:30

Up early granny gotta get your weekend nasty snipe first thing I guess hey!

[chris shiherlis] 16/5/2015 01:50

Bobo was busy sharpening another truck load of pencils (with an extremely small pencil sharpener) he was actually unaware of the meeting, Bligh told him the date but Bobo was clever enough (just) to work out he could be lying - again.

Although a recording of the meeting was played back to Bobo afterwards to keep him up to speed, below is the video of the meeting.



He was instructed to watch the full video and did so whilst sharpening more pencils.

Pathetic Weasels.

[tuckerjenkins1] 15/5/2015 22:36

Haha, u forgot bobo.