Difference between revisions 7841176 and 7924744 on simplewiki

{{short description|Scientific projections regarding the far future}}
[[File:Red Giant Earth warm.jpg|thumb|274x274px|alt= A dark gray and red sphere representing the Earth lies against a black background to the right of an orange circular object representing the Sun| Artist's idea of the [[Earth]] several billion years from now, when the [[Sun]] is a [[red giant]].]]

The ultimate fate of our universe may be the [[heat death of the universe]]. Before that happens, it is possible to predict that the following will happen.

Some types of [[science]] can say what could happen far into the future.<ref>{{cite book| author= Rescher, Nicholas|  title = Predicting the future: An introduction to the theory of forecasting| date = 1998| publisher = State University of New York Press| isbn = 978-0791435533}}</ref> Before we go further, it is worth noting that our [[local group|local group of galaxies]] are bound by gravitation, and its changes and aging can be discussed separate from the rest of the universe.

For example, [[astrophysics]] can say how [[planet]]s and [[star]]s form, affect each other, and die; [[particle physics]] can say how [[atom]]s and other matter act over time; [[evolutionary biology]] can allow us to see how living things change over time; and [[plate tectonics]] can say how continents shift over time.  By observing the past and present, astrophysicists, particle physicists, evolutionary biologists and geologists can make guesses about what might happen in the future.  

The [[second law of thermodynamics]] is important to predictions about the future of Earth, of the Solar System, and the future of the expanding [[universe]]. The second law of thermodynamics says that [[entropy]] is always happening.  That means that the universe is slowly running out of the kind of energy that can do [[work (physics)|work]].<ref name="Nave"/> For example, stars will eventually run out of [[hydrogen]] fuel and burn out.<ref name="five ages"/>

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| 8 billion
| The Sun will become a carbon–oxygen [[white dwarf]] with about 54.05% its present mass.<ref name="Schroder 2008"/><ref name="nebula"/><ref name="apj676_1_594"/><ref name="dwarf group note">Based upon the weighted least-squares best fit on p. 16 of Kalirai et al. with the initial mass equal to a [[solar mass]].</ref> At this point, if somehow the Earth survives, it will become much colder very quickly bec
uause the white dwarf Sun will give off much less energy than the yellow dwarf Sun does today.
|-
| style="background: lavender;" | [[File:Five Pointed Star Solid.svg|16px|alt=Astronomy and astrophysics|Astronomy and astrophysics]]
| 22 billion
|-
| style="background: lavender;" | [[File:Five Pointed Star Solid.svg|16px|alt=Astronomy and astrophysics|Astronomy and astrophysics]]
| 50 billion
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|-
| style="background: #FFE4E1;" | [[File:Psi (greek letter).svg|16px|alt=Particle physics|Particle physics]]
| <math>10^{10^{50}}</math><ref name=prob group=note/><ref name=bignumber2 group=note/><wbr/><ref group="note"><math>10^{10^{50}}</math>is 1 followed by 10<sup>50</sup> (100 quindecillion) zeroes</ref>
| Estimated time for a [[Boltzmann brain]] to appear in the vacuum bec
uause there will be less spontaneous [[entropy]].<ref name="linde"/>
|-
| style="background: #FFE4E1;" | [[File:Psi (greek letter).svg|16px|alt=Particle physics|Particle physics]]
| <math>10^{10^{76}}</math><ref name=bignumber2 group=note/>
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<ref name=loeb_2016>{{cite journal |last1=Loeb |first1=Abraham |year=2016 |last2=Batista |first2=Rafael |last3=Sloan |first3=W. |title=Relative Likelihood for Life as a Function of Cosmic Time |journal=Journal of Cosmology and Astroparticle Physics |volume=2016 |issue=8 |pages=040 | arxiv = 1606.08448 |doi=10.1088/1475-7516/2016/08/040|bibcode=2016JCAP...08..040L }}</ref>

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[[Category:Time]]
[[Category:Science]]