The Most Extreme Temperatures In The Universe! From Hottest To Coldest
1,122Temperature by definition is a measure of how something is cold or hot but due to the lack of
scientific consistency in the terms “cold” or “hot” we use temperature with different scales to
describe the thermodynamic state of any object. In particular, temperature is a measurement of
the average kinetic energy of the particles at the molecular and atomic levels of an object, that
is the type of energy corresponding to the motion of these particles. The faster these particles
move, the more kinetic energy they have. Furthermore, these particles are constantly colliding
with each other resulting in many variations in the kinetic energy associated with each particle
therefore we take the average kinetic energy of the total number of particles to avoid such
variations. On being familiar with the concept of temperature, you may wonder what makes
objects hot and what makes them cold; in other words the limit between the cold and the hot
and based on what foundation we constructed such a limit?
In order to demonstrate that limit, scientists came up with two terms; the “absolute hot” which is
the upper limit of the highest temperature that is possible in the entire universe and the
“absolute zero” which is the lowest temperature ever at which the particles at the atomic level
stop moving and lose their vibrational motion hence their kinetic energy. Driven by the “Embrace
the Extremes” principle, in this video; we’re introducing the most extreme temperatures in the
universe both observed and man made.
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Here’s the list from hottest to coldest temperatures:
10- The highest possible theoretical temperature ever is the Planck temperature which is of
order 10^(32) Kelvin. it was the temperature of the universe 10^(-43) seconds after the moment
of the big bang, the big bang model states that our universe at its beginning, 13.7 billion years
ago, was in extremely hot and dense state which motivated the development of the standard
model of strong and electroweak interactions not to mention the extending and expanding the
original big bang model, where the fundamental particles including the quarks and leptons as
point like particles. Consequently, the early universe can be pictured as a dilute gas of weakly
interacting quarks, leptons and gauge bosons.
9- The hottest handmade temperatures ever, have been achieved by the physicists at CERN’s
large hadron collider near Geneva, Switzerland. They recorded 5.5 trillion Kelvin by colliding
Lead ions to momentarily create a quark-gluon plasma which is pretty much like a subatomic
plasma that is thought to have existed just moments after the big bang. The experiment was
performed by by the ALICE collider in 2012, by these results the physicists were able to create a
quark-gluon plasma that is 38% hotter than the Guinness record holder; the 4 trillion Kelvin
plasma achieved in 2010 by a similar experiment at the RHIC, Brookhaven New York. The
ability to achieve such high temperatures enables the physicists to map the early stages of our
universe through tracing the phase transitions of the quark-gluon plasma.
8- The core temperature of a dying massive star comes in the third place with approximately 10
to 100 billion Kelvin. As you probably already know, the star is a sphere of gas held together by
its own gravitational pull; its life is considered as a constant struggle against this gravitational
pull. Since gravity is constantly trying to cause the star to collapse. However, it’s not the only
force acting on the star during its lifetime; the star’s core is extremely hot and radiates heat from
the hydrogen fusion into helium which results in the radiation pressure that pushes outwards
counteracting the force of gravity and putting the star in a state of hydrostatic equilibrium. Most
of the star's lifetime is called the main sequence stage at which there’s an equilibrium between
the gravitational pull acting inward and the radiation pressure acting outward. During the main
sequence, the heat and radiation come from the nuclear reactions at the core, but eventually the
core runs out of its hydrogen fuel and transitions into other stages provided that the star is
massive enough to go through some other nuclear reactions. At first, the outer layers will swill
out into a red supergiant. Next, the core will shrink as it becomes more dense and hot. Then,
the helium fusion into carbon will begin and it will shrink again once it runs out of its helium fuel,
the massiveness of the core will allow for the carbon fusion into neon.
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