مصير الأرض و الشمس و كل شيء | الدحيح

0:01 Dad, Dad. How was I made?

0:03 That was yesterday’s question. Ask another one.

0:06 How long will the sun keep shining?

0:08 Until the end of the world. Then it fades.

0:11 -Will the world really end? -Yes.

0:13 -Why? -Because everything has an end.

0:14 -Why? -Because physics says so.

0:16 -Why? -Physics is applied science.

0:18 Math is applied philosophy. And philosophers said so.

0:22 -Why? -They were bored in Ancient Greece.

0:26 Stop asking why. New questions!

0:29 So you and Mom will fade too?

0:32 Yes. Everything will fade.

0:34 Your mom, dad, grandpa, aunt, and uncle.

0:37 -Why? -Because biology follows physics.

0:41 What’s going on here? Why are you crying?

0:44 Dad said everything will end, even the sun and my uncle.

0:50 He’s lying. I said the sun will stop shining.

0:52 It’s burning gas. When it’s done, it goes dark.

0:56 Then comes an ice age. Then the uncle fades.

1:01 These are basic physics. What’s the problem?

1:04 He’s just a kid!

1:06 I told you a hundred times not to mention the end of the world!

1:08 Sorry, but it’s my right.

1:09 I agreed with your family to discuss it anytime.

1:15 Enough!

1:17 Come on, sweetheart. Don’t cry.

1:19 I’ll tell you about the multiverse.

1:21 There are lots of your uncle there. Let’s go.

1:32 Hello my dear viewers.

1:33 Welcome to a new episode of Al-Daheeh.

1:35 Let’s head to Vatican Palace

1:37 and look at one of the most famous murals ever painted.

1:41 The School of Athens.

1:42 It was painted by the Italian artist Raphael in the early 16th century.

1:45 The painting brings together the greatest philosophers and early scientists.

1:49 You see figures like Pythagoras, Heraclitus, and Euclid.

1:51 But the most important part is this exact scene.

1:55 The scene that brings Plato and Aristotle together.

1:57 Plato stands on the left and points his finger to the sky.

2:00 Aristotle stands on the right and points his hand to the ground.

2:02 Two gestures pointing in opposite directions.

2:04 Art here captures the biggest disagreement in philosophy.

2:08 Plato points upward to what is called the World of Forms.

2:12 In Plato’s philosophy, it is a perfect, unseen world.

2:16 Everything there exists in a state of absolute perfection.

2:19 Our earthly world is only a reflection of it.

2:21 It was created as an imperfect copy of an ideal world.

2:24 What matters to us is the word created.

2:27 It means our world did not exist, then suddenly came into being.

2:30 In the 4th century BC, Aristotle speaks to his students at the Lyceum in Athens.

2:35 He begins arguing an idea far stranger than Plato’s.

2:40 He sums it up in one bold sentence.

2:42 "Nature abhors a vacuum."

2:46 Nature hates a vacuum.

2:48 "What does that mean, Abu Hamid?"

2:50 It means nothing in the universe ever truly becomes nothing.

2:54 There was never a time of nothing before the universe existed.

2:57 There will never be a time when the universe ends into nothing.

3:00 The universe has no beginning and no end!

3:03 That is why Aristotle, in the painting, points down toward the earth.

3:07 He is saying the universe is made of eternal matter.

3:11 It has no beginning and no end.

3:13 The painting places both ideas side by side.

3:15 But which idea will eventually win?

3:18 At first, Aristotle’s students are completely shocked.

3:21 His idea contradicts Greek philosophy

3:24 and even contradicts his own teacher, Plato.

3:26 But gradually, Aristotle’s idea takes over philosophy and natural science

3:32 for almost two thousand years.

3:33 His idea created enemies everywhere.

3:35 Religious scholars in Europe and the Islamic world oppose it.

3:38 They reject Aristotle’s view and call it the eternity of the world.

3:41 They claimed the world had a beginning.

3:43 In religion, after all, the universe is created.

3:44 But the idea also finds supporters who want it to be true, like alchemists.

3:50 They dream of turning cheap metals into gold.

3:53 Aristotle’s idea says the matter of the universe is constant.

3:57 Only the forms of matter change from one state to another.

4:01 That gives them hope.

4:02 they believe gold and tin are just different forms of the same substance.

4:06 And maybe, one day, tin could become gold.

4:09 The eternity of the universe remains a major philosophical problem.

4:14 It is extremely hard to disprove with solid science.

4:19 Some people believe the universe was created and will one day come to an end.

4:22 Others believe the universe has no beginning and no ending at all.

4:27 But in the early 20th century, all of this changed.

4:31 On October 6, 1923, at the top of Mount Wilson in California.

4:36 The mountain hosts the Hooker Telescope, the largest in the world at the time.

4:40 It can observe stars anywhere in the Milky Way.

4:46 That day, a young American astronomer arrives to take a routine photo

4:51 of a spiral-shaped cloud in our galaxy, M31.

4:54 Like any young astronomer, he was monitoring the galaxy,

4:58 but then he noticed something very strange.

5:00 The photos he took that day looked different

5:03 from those taken the previous two days.

5:05 There’s a star in the image that isn’t a normal nova.

5:07 A nova lights up for a while then fades completely.

5:10 This star is completely different.

5:11 Astronomers call it a Cepheid variable.

5:14 This star becomes a key marker in studying space.

5:18 It lights up and dims in a regular pattern, as if it is giving pulses.

5:23 At that moment, the young astronomer changes the star’s symbol

5:26 from "N" for nova to "VAR" for variable.

5:32 This young astronomer is Edwin Hubble.

5:38 He is the one the Hubble Space Telescope is named after,

5:40 which gave us the most important images of the universe.

5:43 The photos Hubble took, later labeled H335H,

5:47 will become the most famous astronomical image in history.

5:50 -Wow! -Let me explain it to you.

5:52 When Hubble discovered the Cepheid variable in that cloud,

5:55 he could calculate the number of its pulses.

5:57 He then measured the time between each pulse,

6:01 and from that, determined the star’s brightness.

6:04 This allowed him to find the Cepheid’s distance from Earth.

6:08 "How did he do all this?"

6:10 Stellar calculations weren’t magic.

6:14 They were available at the time.

6:15 Thanks to astronomer Henrietta Swan Leavitt

6:18 and her team of researchers, known as Harvard Computers.

6:21 There wasn’t a machine back then,

6:22 but the word "computer" referred to anyone who did calculations manually.

6:26 Anyone doing calculations by hand.

6:30 Hubble finally calculated the distance to the star using Henrietta’s work.

6:35 He discovered the Cepheid was 800,000 light-years away.

6:39 The Milky Way galaxy is about 100,000 light-years across.

6:43 Here Hubble realized the star was in a completely different galaxy.

6:47 Later, we’d learn this galaxy is Andromeda.

6:51 He distance isn’t 800,000 light-years, it’s actually 2.5 million light-years.

6:56 That means light takes 2.5 million years to travel that distance.

7:03 This was the first time in history

7:06 humans knew there were other galaxies in the universe.

7:10 Because of this, Edwin Hubble is called

7:12 "The man who discovered the universe."

7:16 In 1929, Hubble began studying 12 galaxies beyond our own.

7:22 He noticed most of the light from these galaxies leaned red.

7:29 "Maybe they’re just shy?"

7:30 Galaxies? Shy? No, it’s the moon that hides its face!

7:33 The red color had another meaning.

7:35 Hubble applied the Doppler effect, which looks at frequency changes in light.

7:41 Through it, he could measure their motion in space.

7:44 If stars move closer, their light shortens and shifts blue.

7:50 If they move away, their light stretches and shifts red.

7:54 Hubble discovered that the galaxies with red light

7:58 were moving away from Earth and from the Milky Way.

8:02 He also noticed the farther a galaxy is, the faster it moves away.

8:08 To understand this better, imagine the universe as a balloon.

8:10 Dots on its surface represent galaxies.

8:14 The more you inflate the balloon, the farther apart the dots move.

8:18 But not all at the same speed.

8:20 Dots near the balloon’s edge move faster than those near the center.

8:26 "What does this have to do with the universe’s beginning, end, or Aristotle?

8:30 Do you know them personally or what?"

8:33 Just wait, and everything will make sense.

8:35 Hubble’s discoveries inspired Belgian physicist Georges Lemaître.

8:39 For the first time, he proposed it in the idea of the expanding universe.

8:42 Lemaître said if the universe expands steadily,

8:45 like a balloon inflating over time,

8:47 we can rewind to the beginning

8:50 and see the very moment it was born.

8:56 Did you catch the word "born"?

8:59 The universe had a beginning, contrary to Aristotle!

9:02 Its start was like the balloon inflating from the smallest possible point.

9:07 This moment would later be called the Big Bang.

9:11 Ironically, the moment science uncovered the universe’s beginning

9:15 also revealed the idea of its eventual end.

9:18 Georges Lemaître was a clergyman as well as a physicist.

9:23 The universe expanding over time, like its birth in the Big Bang,

9:28 revived an old 19th century idea called heat death.

9:33 This theory comes from one of physics’ most important laws,

9:36 the second law of thermodynamics.

9:39 Let’s imagine two glass cubes.

9:44 The first holds hot gas, with fast, energetic particles.

9:48 The second holds cold gas, with slow, calm particles.

9:51 Now connect the two cubes.

9:53 The hot cube with fast, energetic particles

9:58 starts to cool down,

10:00 while the cold cube heats up.

10:05 This continues until both reach the same temperature.

10:10 The second law of thermodynamics fully explains this process.

10:14 It says that in isolated systems, with no outside influence,

10:20 energy always flows from hotter systems to colder ones.

10:25 Here I need to introduce a term. Entropy.

10:29 It measures disorder and change in a system.

10:34 In our experiment, energy transfer continues

10:38 until entropy reaches its maximum.

10:43 At that point, temperatures become equal.

10:48 This process cannot be reversed

10:52 unless an external force steps in.

10:56 If you look closely, you’ll notice the second law of thermodynamics

10:59 is one of the very few laws in physics

11:02 where time shows up.

11:06 Let me explain it to you.

11:08 Matter changes from one state to another,

11:12 but time never runs backward.

11:15 In physics, most processes are time agnostic.

11:19 They don’t care about time.

11:22 They don’t have to move in one direction through time.

11:24 This law describes how particles, and everything in the universe,

11:28 move from an ordered state, with low entropy,

11:32 to a more random, chaotic state, with higher entropy.

11:36 Most importantly, this process cannot be reversed under the same conditions.

11:41 Most physical processes can run in either direction.

11:45 But with entropy, you can only do it from one side.

11:49 If you drop a cup of tea and it shatters into pieces,

11:51 the only law stopping it from reassembling itself like nothing happened,

11:55 is the second law of thermodynamics.

11:57 Now look at the whole universe. You’ll see the same law applies.

12:01 In 1852, the British physicist Lord Kelvin published a paper titled…

12:10 In it, he used the first and second laws of thermodynamics

12:15 to predict the fate of the universe.

12:18 If we assume the universe is a closed, isolated system,

12:22 then energy moves from its most dense, complex state,

12:27 the singularity, where the Big Bang began,

12:34 through the gradual expansion of the universe,

12:38 where stars, galaxies, and even life itself form.

12:41 As expansion continues, galaxies drift farther apart,

12:45 just as Hubble saw through his telescope.

12:47 Until the universe reaches a stage

12:49 where its temperature drops and energy dissipates.

12:53 When energy dissipates in an irreversible way,

12:59 the entire universe enters a state of equal temperature.

13:02 Or as Lord Kelvin called it, heat death.

13:07 Kelvin wrote:

13:10 If the finite universe is left to obey existing laws,

13:14 the inevitable result will be stillness and cold death.

13:21 Our universe will be like a corpse, cold and lifeless.

13:23 "The laws of physics are ruthless!"

13:26 Kelvin saw the idea of heat death as a paradox.

13:31 It could challenge the notion of an eternal universe.

13:34 It challenged the 19th-century idea

13:38 that the universe has no beginning or end.

13:43 If the universe were eternal, there shouldn’t be any motion.

13:46 Every movement consumes mechanical energy,

13:50 but our universe moves like stars, planets, everything we can observe.

13:55 With 20th century discoveries, Hubble’s contributions,

13:58 Einstein’s relativity, and others,

14:01 it was easy to bring back the heat death hypothesis

14:04 to fit the laws of physics.

14:09 But in the second half of the 20th century, the theory ran into problems.

14:13 If galaxies move quickly, as Hubble proved,

14:17 their speed could slow over time.

14:20 From this came a new idea, the Big Crunch.

14:24 Its proponents assumed the universe’s expansion would slow.

14:29 Over time, expansion would reverse,

14:35 galaxies would collapse and collide.

14:42 Gravity would compress them,

14:45 causing explosions and…

14:49 forming massive black holes.

14:53 The end of the universe would lead to a new singularity and Big Bang,

14:59 creating a whole new universe.

15:01 "Oh no! So we get our lives replayed,

15:05 back to school, work, and marriage?!"

15:10 Relax! These are just guesses.

15:12 We won’t live twice… as far as we know!

15:15 For years, scientists treated galaxy motion like a projectile,

15:22 like a football kicked into the sky.

15:24 Over time, it slows, stops briefly,

15:27 and then gravity reverses its motion,

15:29 sending it crashing back.

15:34 But in 1998, two teams of astronomers were shocked

15:39 while studying a supernova explosion.

15:42 They discovered the supernova was not just moving away from Earth,

15:45 it was accelerating.

15:49 This meant the galaxy it belonged to was also accelerating.

15:54 So the speed not only stays constant or slows down, but also accelerates.

16:00 Contrary to the Big Crunch idea,

16:05 which expected the universe’s expansion to slow down,

16:08 what actually happened was the opposite: the universe sped up its expansion.

16:11 What we have discovered is an unknown force in the universe

16:17 called Dark Energy

16:19 that pushes galaxies apart and drives cosmic expansion.

16:23 It is a force we know exists in the universe.

16:28 But we cannot measure it, or know its true value.

16:30 Is it positive or negative?

16:32 Will it stay within safe limits, or could it grow in the future?

16:35 Because if it does increase, the universe would expand at an extreme speed,

16:39 which could cause a tear in the fabric of space.

16:43 Imagine the universe ripping open, like a busted zipper, exposed to all realities.

16:48 A cosmic scandal across the multiverse.

16:49 This is known as the Big Rapture.

16:53 Even though recent scientific papers suggest

16:56 that dark energy changes strength over time, rising and falling,

16:59 the heat death theory remains the most realistic scenario so far.

17:06 So let us try to picture it using our most important energy source on Earth.

17:12 The Sun.

17:13 The Sun is a medium sized star.

17:16 It is roughly the same age as our planet, about 4.6 billion years old.

17:22 It is the main energy source for Earth and the planets orbiting it.

17:26 To remain a stable energy source, the Sun must burn hydrogen in its core.

17:31 This process causes two things.

17:32 First, it releases the energy we depend on, and a fraction of it reaches us.

17:35 Second, it produces helium, which slowly builds up in the Sun’s core.

17:41 But recently, we discovered something strange during this burning process.

17:44 As long as the Sun keeps holding everything inside,

17:48 helium builds up, and it slowly kills itself.

17:50 Why not just be like the Moon?

17:52 Cold, frozen, doing nothing, just borrowing sunlight and shining quietly.

17:56 Civilizations adore moonlight.

17:59 Meanwhile, the Moon is just sitting there doing nothing.

18:02 Every billion years, the Sun’s burning rate increases.

18:06 As a result, its brightness and energy output rise by 10 percent.

18:13 This is extremely dangerous.

18:16 Because the heat reaching Earth would increase dramatically.

18:20 As a result, the atmosphere protecting the planet would begin to erode.

18:24 Then rising temperatures would start evaporating oceans and water bodies.

18:28 Their vapor would gradually get trapped in the upper layers of the atmosphere.

18:32 When that happens, we would see the greenhouse gas effect,

18:36 raising the planet’s temperature to unprecedented levels.

18:41 All surface water would evaporate at extremely fast rates.

18:46 Once all the water is trapped in the upper atmosphere,

18:49 the Sun’s intense heat would break water molecules into hydrogen and oxygen,

18:54 which would escape the planet entirely.

18:57 In a short time, our planet would become a barren desert.

19:03 It would completely leave the habitable zone of the solar system.

19:07 Earth would leave the habitable zone,

19:12 and Mars would take its spot as the new planet within that zone.

19:16 "You have relieved me!"

19:18 Wait… the disaster hasn’t come yet.

19:20 "It still hasn’t, after all that?"

19:22 Unfortunately, after 4 billion years of our planet burning,

19:28 the Sun will reach its final days.

19:32 It will start transforming from a medium star into a massive red giant.

19:37 Its surface temperature will drop as it swells.

19:41 Remember when I told you burning hydrogen produces energy and helium?

19:45 Five billion years from now,

19:49 the Sun will exhaust all hydrogen in its core and turn it into helium.

19:53 Because the Sun is affected by gravity like everything else,

19:56 the pull on its outer layers will transfer inward, compressing the core.

20:00 To prevent collapse in its heart,

20:03 it will start burning the leftover hydrogen on the outer core.

20:05 Over 10 billion years, the Sun’s lifespan,

20:08 when it burns this hydrogen rapidly to save its core,

20:12 it will expand twenty times its normal size.

20:15 This swelling will swallow all the planets in its path,

20:20 including Earth, Mars, and others.

20:23 After swallowing all planets up to Mars,

20:25 it will burn all remaining core hydrogen, shrink down from that giant size,

20:31 but never return to its original form.

20:33 Gravity will keep pressing hard,

20:35 so it will start burning the accumulated helium.

20:38 Burning helium produces explosions and ejects parts of the Sun itself.

20:43 It will expand again, but this time for the last time,

20:50 until the Sun, which once cradled life on this planet,

20:57 detonates in its greatest explosion.

20:59 Its core temperature reaches 100,000 Kelvin

21:02 after exhausting all hydrogen and helium.

21:04 Only heavy elements remain, like carbon and oxygen,

21:07 whose fusion in the core will leave the Sun as a white dwarf,

21:12 a witness to the Sun’s death, like a gravestone.

21:15 These are the Sun’s final days.

21:19 That was the story of the Sun’s final days.

21:22 Now let us talk about our galaxy’s fate.

21:25 Remember the spiral cloud cluster,

21:28 that Hubble proved was a separate galaxy called Andromeda.

21:31 It is moving southeast from its current position in space.

21:36 When we calculated its speed, we found it travels at 110 kilometers per second.

21:41 Heading where?

21:44 "Do not say it is heading straight for us!"

21:46 Exactly. It is moving straight toward our Milky Way.

21:49 "Why are you smiling? That is a disaster!"

21:50 From 2000 to 2010, astronomers studied Andromeda’s stars

21:56 using the Hubble telescope.

21:58 They compared them to stars in distant galaxies

22:00 to calculate the distance between us and Andromeda.

22:03 By measuring its angles and speed with high precision,

22:07 they found a chance of a Milky Way collision.

22:12 "What? What if it hits us? How do we fix that?

22:16 Go ask if there is a way to save our galaxy!"

22:22 Calm down. That is still 10 billion years away.

22:27 Still, they will drift past like a cosmic wind!

22:29 In fact, we can already see Andromeda in the sky.

22:32 Over millions of years, it will become clearer and clearer,

22:35 like a car speeding straight toward a crash.

22:37 In 4 to 5 billion years, the first collision will occur.

22:41 Then each galaxy will pass by with little effect.

22:45 Over time, they will drift closer,

22:47 as if the two galaxies are dancing flamenco in space.

22:50 After 2 billion years, they collide again,

22:54 beginning full merger.

22:57 The black holes at their centers merge too,

23:00 forming a massive black hole,

23:04 the single giant core of a brand new galaxy.

23:07 "So if God gives us billions of years of life,

23:11 and we see the galaxies collide, what will happen to Earth?"

23:15 what optimism is this?

23:17 The Sun is already hot, and it will get even hotter in a billion years.

23:21 If we survive it, and manage to leave Earth

23:24 before the Sun swallows it turning into a red giant,

23:27 and move to a new planet in our solar system…

23:30 Even if we do all that, like a Nolan movie plot,

23:32 there’s a very high chance the new planet won’t feel the galaxy collision at all.

23:36 That’s because distances in space are unbelievably huge.

23:39 For example, the distance between Earth and the nearest star is 4 light-years.

23:44 Let me make it clearer to you.

23:47 Imagine the Sun as a ping-pong ball, and the closest star to Earth as a pea.

23:50 If we put the ping-pong ball here and the pea over there,

23:54 the distance between them would be 1,100 kilometers.

23:56 That’s an enormous distance for objects of that size.

23:58 Most calculations say stellar collisions are nearly impossible.

24:04 Most likely, our solar system will stay in the outer shell of the new galaxy,

24:08 without any noticeable change.

24:10 So we might witness the final days of Earth, the Sun, and the galaxy.

24:16 Next are the last days of the universe.

24:20 Unfortunately, the fate is the same: heat death,

24:24 the destiny of all elements in the cosmos according to physics.

24:30 From stars to galaxies, even black holes.

24:33 That’s because every element depends on energy to exist,

24:36 kinetic energy or stored potential energy.

24:42 When the universe reaches maximum entropy,

24:46 all this energy will disperse evenly across space,

24:50 after the universe reaches its maximum expansion.

24:53 Everything will die gradually and sequentially.

24:55 The Sun’s death will occur during the death of stars,

24:58 which begins 100 million years from now.

25:01 It will start with the death of red dwarfs,

25:04 the most common type of star.

25:09 At first, their fuel runs out, like I told you with the Sun.

25:12 Due to gravity, they collapse into black dwarfs, extremely dense remnants.

25:16 This process will continue for up to 100 billion years.

25:19 We will see stars disappearing from our sky, one by one.

25:23 The sky will turn into darkness.

25:25 No matter how we look with telescopes from anywhere,

25:28 we will see nothing.

25:30 Even radiation from the farthest places in the universe,

25:32 like the Big Bang’s glow, we won’t detect it.

25:35 Over time, we won’t be able to tell the universe’s age

25:37 or what happened at the beginning.

25:39 After a thousand trillion or quadrillion years, galaxies will start to break apart.

25:45 Planets will lose their orbital paths

25:47 and drift randomly through space,

25:50 marking the start of the era of galaxy death.

25:52 According to theoretical physicist Freeman Dyson,

25:55 after a quintillion years, 90 to 99% of planets will be scattered in space,

26:01 without any orbit or planetary system to belong to.

26:06 Smaller objects will drift randomly through the void.

26:09 Heavier objects will be drawn to the galaxy centers

26:13 and swallowed by black holes, making them even larger.

26:17 After that, very strange things happen.

26:19 At the end of the death of stars and galaxies,

26:24 the remaining basic elements are protons, black holes,

26:28 and star remnants turned into black dwarfs.

26:31 The proton is the core of every atom, giving matter its mass.

26:35 When a proton decays, it produces positrons and gamma-ray photons.

26:40 Until recently, the Standard Model,

26:43 the theory describing subatomic particles,

26:48 forbade proton decay under normal conditions.

26:52 A proton under normal conditions will not decay!

26:55 Unfortunately, after galaxies die, protons themselves will decay.

26:59 The assumption also says, for all protons in the universe to decay,

27:04 we need between 10^34 and 10^40 years,

27:09 that is, from 10 duodecillion to 10 quattuordecillion years.

27:12 Of course, you don’t know how many that is, and neither do I!

27:14 During that time, everything will decay:

27:19 planet remnants, stars turned into black dwarfs, even atomic dust itself.

27:25 If you think this is the end, not yet.

27:28 After proton decay, it’s the black holes’ turn,

27:31 which are dark, devouring, and expanding.

27:37 Even black holes lose mass and evaporate over time.

27:40 This is called Hawking radiation.

27:43 Black holes lose energy as very faint radiation from their event horizon.

27:49 Over time, they shrink, get smaller, and disappear completely.

27:55 For small black holes, say Earth-sized,

28:00 this takes about 10^67 years.

28:03 The largest black holes, swallowing matter at galaxy centers,

28:08 need 10^106 years to disappear,

28:12 a million googols of years.

28:16 After the last black hole dies, not much will remain in the universe.

28:19 Even dark matter will decay or already be swallowed by black holes.

28:24 All that’s left is vast empty space,

28:27 with energy evenly spread,

28:32 near absolute zero.

28:35 The universe dies.

28:37 Everything becomes dark and cold,

28:42 no vibrations, no motion, no energy.

28:44 Everything disappears.

28:46 Only random electrons and photons drift in infinite space.

28:52 In the end, the universe in our episode follows the rules of physics.

28:57 The universe is not as Aristotle imagined,

29:02 not eternal before or after us.

29:05 It appears like a living creature like us.

29:08 A child is born, grows, goes through adolescence,

29:12 and eventually weakens and dies.

29:16 We humans, every cell in our bodies is made of the universe’s elements.

29:20 Elements formed at its birth, like hydrogen and helium,

29:22 or later formed, like carbon, oxygen, and iron.

29:26 We are living witnesses to this universe.

29:29 Science can imagine its beginning and its end.

29:32 And what we experience is a cosmic death, just like our human death.

29:36 Just as the universe ends, our episode comes to an end.

29:39 Don’t forget to watch the new episodes and the old ones.

29:42 Check the sources below and subscribe if you're on YouTube.

29:44 Hope someone watching us in 10^67 or 10^106 years

29:50 can tell us if these predictions were right?

29:52 "But we will not be alive."

29:54 Speak for yourself. I am an idea, and ideas never die.

29:56 Physics never mentioned thoughts, so I am safe.

مصير الأرض و الشمس و كل شيء | الدحيح

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