Another good novel to draw a film from would be Isaac Asimov's The End of Eternity. I'd adapt it though, expanding the range of characters, revising aspects of the lifestyle and personality types, incorporating the latest generation of gadgets into the societies of our future.
Perhaps too, have the ending completely rewritten.
The noble intention that ends the original text, proves not to work out, interference with time is in some ways, inescapable. The central characters are bounced back to Eternity once again, it proves not to have been ended by their action as they thought it might. But this version seems highly technologically advanced, a generation or two ahead, more controlling, more intrusive and manipulative.
Perhaps as if, sure, their big action maybe did work, but almost as soon as that happened, the same awareness sprang up again, and instead of the 50s outlook we get it cast in a 2010s outlook.
The characters continue to be time fugitives, and Eternity cannot be so easily destroyed. They will have babies and meet up with other fugitives as this incarnation of Eternity grows all powerful and develops itself militarily all the way up and down the time line.
Eternity is significantly upgraded, descended from Asimov's doughty 1950s infrastructure but now the latest 21st century computing and technical excellence.
Retain and bring out Asimov's details of social engineering and general time travel policies.
Describe the progress of the fugitives.
Have the time line smashed yet again, and returning yet again, this time highly military, highly stealthy, highly protected etc.
Sunday, 13 July 2008
Friday, 11 July 2008
The Horizon
An excellent view from 117 Victoria St:
Saturday, 17 May 2008
Reflections
Reflecting the rising sun, office blocks glow with palettes of smouldering yellowy orange.
Sunday, 17 February 2008
Sundry supplement
The more hotter and more massive the star, the shorter its main sequence and the time it takes to consume its primary fuel.
O class are hottest and shortest lived, bluish white and ultraviolet stars. They burn for only a few million years. They are as rare as 1 in 3 million in the solar region.
B class, luminous blue stars making up 1 in 800 of all stars. They are also short lived and static, clustering up with O class stars in their nurseries of molecular hydrogen and carbon monoxide.
A class, white or bluish white stars to the naked eye, 1 in 160 stars. They emit strong hydrogen and ionised metal spectral lines.
F class, white to yellow shining, 1 in 32 stars. They show spectral lines of hydrogen and neutral and ionized metals.
G class, our sun, like near neighbour Alpha Centauri A, is yellow in appearence. Surprisingly, 1 in 13 stars are yellow. Our Sol is estimated to be nearly halfway through its 10 billion year supply of hydrogen fuel. It emits spectral lines of hydrogen, ionised and neutral metals and carbon hydrogen (CH) molecules. The hydrogen fuel will run out in 5 to 6 billion years. Sol will use helium as fuel. Just as nuclear fusion of hydrogen produces helium, nuclear fusion of helium produces carbon. The sun swells as it uses a lower energy level of fuel each time, on its way to the lowest state of iron, reddening and brightening into a giant. After growing out to the orbit of Jupiter, ejecting mass, it will collapse into a brown dwarf mainly made of iron.
Below that is the K class, more orange looking than Sol. 1 in 8 stars is a K class. Their spectrum shows little or no hydrogen, plenty of neutral metals, a few molecular lines such as titanium oxide.
Below that is the most common, the M class of star. 80% of all stars are red or brown or black dwarfs. Like all other classes, there can be giant and supergiant versions. Dwarves in this class have all kinds of molecular lines, such as titanium and vanadium oxide, in their spectrum as well as elements, but no hydrogen lines.
O class are hottest and shortest lived, bluish white and ultraviolet stars. They burn for only a few million years. They are as rare as 1 in 3 million in the solar region.
B class, luminous blue stars making up 1 in 800 of all stars. They are also short lived and static, clustering up with O class stars in their nurseries of molecular hydrogen and carbon monoxide.
A class, white or bluish white stars to the naked eye, 1 in 160 stars. They emit strong hydrogen and ionised metal spectral lines.
F class, white to yellow shining, 1 in 32 stars. They show spectral lines of hydrogen and neutral and ionized metals.
G class, our sun, like near neighbour Alpha Centauri A, is yellow in appearence. Surprisingly, 1 in 13 stars are yellow. Our Sol is estimated to be nearly halfway through its 10 billion year supply of hydrogen fuel. It emits spectral lines of hydrogen, ionised and neutral metals and carbon hydrogen (CH) molecules. The hydrogen fuel will run out in 5 to 6 billion years. Sol will use helium as fuel. Just as nuclear fusion of hydrogen produces helium, nuclear fusion of helium produces carbon. The sun swells as it uses a lower energy level of fuel each time, on its way to the lowest state of iron, reddening and brightening into a giant. After growing out to the orbit of Jupiter, ejecting mass, it will collapse into a brown dwarf mainly made of iron.
Below that is the K class, more orange looking than Sol. 1 in 8 stars is a K class. Their spectrum shows little or no hydrogen, plenty of neutral metals, a few molecular lines such as titanium oxide.
Below that is the most common, the M class of star. 80% of all stars are red or brown or black dwarfs. Like all other classes, there can be giant and supergiant versions. Dwarves in this class have all kinds of molecular lines, such as titanium and vanadium oxide, in their spectrum as well as elements, but no hydrogen lines.
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