How far would you have to go to escape gravity? - Rene Laufer

574,765 views

2018-11-06 ใƒป TED-Ed


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How far would you have to go to escape gravity? - Rene Laufer

574,765 views ใƒป 2018-11-06

TED-Ed


์•„๋ž˜ ์˜๋ฌธ์ž๋ง‰์„ ๋”๋ธ”ํด๋ฆญํ•˜์‹œ๋ฉด ์˜์ƒ์ด ์žฌ์ƒ๋ฉ๋‹ˆ๋‹ค.

๋ฒˆ์—ญ: GAAE GANG ๊ฒ€ํ† : Tae Han Yoon
00:06
More than six thousand light years
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์ง€๊ตฌ ํ‘œ๋ฉด์—์„œ 6000๊ด‘๋…„ ์ด์ƒ ๋–จ์–ด์ง„
00:08
from the surface of the earth,
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00:10
a rapidly spinning neutron star
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๋ธ”๋ž™ ์œ„๋„์šฐ ํŽ„์„œ๋ผ ๋ถˆ๋ฆฌ๋Š” ๋น ๋ฅด๊ฒŒ ๋„๋Š” ์ค‘์„ฑ์ž ๋ณ„์€
00:12
called the Black Widow pulsar
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00:14
blasts its companion brown dwarf star with radiation
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9์‹œ๊ฐ„๋งˆ๋‹ค ์„œ๋กœ ๊ณต์ „ํ•˜๋Š” ๋™๋ฐ˜ ๊ฐˆ์ƒ‰์™œ์„ฑ์—
00:18
as the two orbit each other every 9 hours.
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๋ฐฉ์‚ฌ์„ ์„ ๋ฟœ์–ด๋ƒ…๋‹ˆ๋‹ค.
00:22
Standing on our own planet,
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์šฐ๋ฆฌ ํ–‰์„ฑ์— ์„œ ์žˆ๋Š” ๋‹น์‹ ์€
00:24
you might think youโ€™re just an observer of this violent ballet.
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์ด ๊ฒฉ๋ ฌํ•œ ์›€์ง์ž„์˜ ๋‹จ์ˆœํ•œ ๋ชฉ๊ฒฉ์ž์ผ ๋ฟ์ด๋ผ ์ƒ๊ฐํ• ์ง€๋„ ๋ชจ๋ฆ…๋‹ˆ๋‹ค.
00:27
But in fact, both stars are pulling you towards them.
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๊ทธ๋Ÿฌ๋‚˜ ์‹ค์ œ๋กœ๋Š” ์ค‘๋ ฅ์— ์˜ํ•ด ์ˆ˜์กฐ ํ‚ฌ๋กœ๋ฏธํ„ฐ๋ฅผ ๊ฑฐ์ณ
๋‘ ๋ณ„์€ ๋‹น์‹ ์„ ๊ทธ๋“ค ์ชฝ์œผ๋กœ ๋Œ์–ด๋‹น๊ธฐ๊ณ  ์žˆ๊ณ 
00:31
And youโ€™re pulling back,
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00:33
connected across trillions of kilometers
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๊ทธ๋ฆฌ๊ณ  ๋‹น์‹ ์€ ๋‘ ๋ณ„์„ ๋‹น์‹  ์ชฝ์œผ๋กœ ๋Œ์–ด๋‹น๊ธฐ๊ณ  ์žˆ์Šต๋‹ˆ๋‹ค.
00:35
by gravity.
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00:37
Gravity is the attractive force between two objects with massโ€”
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์ค‘๋ ฅ์€ ์งˆ๋Ÿ‰์„ ๊ฐ€์ง„ ๋‘ ๋ฌผ์ฒด ์‚ฌ์ด์˜ ์ธ๋ ฅ์ž…๋‹ˆ๋‹ค.
00:42
any two objects with mass.
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๊ทธ ์–ด๋– ํ•œ ๋‘ ๋ฌผ์ฒด๋“ ์ง€์š”.
00:44
Which means that every object in the universe attracts every other object:
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์ด๋Š” ์šฐ์ฃผ์— ์žˆ๋Š” ๋ชจ๋“  ๋ฌผ์ฒด๋Š” ์„œ๋กœ ๋Œ์–ด๋‹น๊ธด๋‹ค๋Š” ๊ฒƒ์„ ์˜๋ฏธํ•ฉ๋‹ˆ๋‹ค.
00:49
every star, black hole,
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๋ชจ๋“  ๋ณ„, ๋ธ”๋ž™ํ™€
00:51
human being, smartphone, and atom
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์ธ๊ฐ„, ์Šค๋งˆํŠธํฐ ๊ทธ๋ฆฌ๊ณ  ์›์ž๋„
00:54
are all constantly pulling on each other.
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๋Š์ž„์—†์ด ์„œ๋กœ๋ฅผ ๋Œ์–ด๋‹น๊น๋‹ˆ๋‹ค.
00:57
So why donโ€™t we feel pulled in billions of different directions?
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๊ทธ๋ ‡๋‹ค๋ฉด ์™œ ์šฐ๋ฆฌ๋Š” ์ˆ˜์‹ญ์–ต์˜ ๋ฐฉํ–ฅ์œผ๋กœ ๋Œ์–ด๋‹น๊ฒจ์ง€๋Š” ๊ฒƒ์„ ๋Š๋ผ์ง€ ๋ชปํ• ๊นŒ์š”?
01:01
Two reasons: mass and distance.
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๋ฐ”๋กœ ์งˆ๋Ÿ‰๊ณผ ๊ฑฐ๋ฆฌ ๋•Œ๋ฌธ์ž…๋‹ˆ๋‹ค.
01:05
The original equation describing the gravitational force between two objects
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๋‘ ๋ฌผ์ฒด ์‚ฌ์ด์˜ ์ค‘๋ ฅ์„ ์„ค๋ช…ํ•˜๋Š” ์ตœ์ดˆ์˜ ๋ฐฉ์ •์‹์€
01:09
was written by Isaac Newton in 1687.
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1687๋…„ ์•„์ด์ž‘ ๋‰ดํ„ด์— ์˜ํ•ด ๋งŒ๋“ค์–ด์กŒ์Šต๋‹ˆ๋‹ค.
01:13
Scientistsโ€™ understanding of gravity has evolved since then,
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๊ทธ ์ดํ›„ ์ค‘๋ ฅ์— ๋Œ€ํ•œ ๊ณผํ•™์ž๋“ค์˜ ์ดํ•ด๋„๋Š” ๊ณ„์† ์˜ฌ๋ผ๊ฐ”์ง€๋งŒ
01:17
but Newtonโ€™s Law of Universal Gravitation
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๋‰ดํ„ด์ด ๋งŒ๋“  ๋งŒ์œ ์ธ๋ ฅ์˜ ๋ฒ•์น™์€
01:20
is still a good approximation in most situations.
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๋Œ€๋ถ€๋ถ„์˜ ์ƒํ™ฉ์—์„œ ์—ฌ์ „ํžˆ ํ›Œ๋ฅญํ•œ ๊ทผ์‚ฟ๊ฐ’์ด ๋ฉ๋‹ˆ๋‹ค.
01:24
It goes like this:
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๊ทธ๊ฒƒ์€ ๋‹ค์Œ๊ณผ ๊ฐ™์Šต๋‹ˆ๋‹ค:
01:25
the gravitational force between two objects
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๋‘ ๋ฌผ์ฒด ์‚ฌ์ด์˜ ์ธ๋ ฅ์€
01:28
is equal to the mass of one
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ํ•œ ๋ฌผ์ฒด์˜ ์งˆ๋Ÿ‰์—
01:30
times the mass of the other,
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๋‹ค๋ฅธ ๋ฌผ์ฒด์˜ ์งˆ๋Ÿ‰์„ ๊ณฑํ•˜๊ณ 
01:31
multiplied by a very small number
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์—ฌ๊ธฐ์— ์•„์ฃผ ์ž‘์€ ์ˆ˜์ธ
01:34
called the gravitational constant,
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์ค‘๋ ฅ ์ƒ์ˆ˜๋ฅผ ๊ณฑํ•˜๊ณ 
01:36
and divided by the distance between them, squared.
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๋‘ ๋ฌผ์ฒด ์‚ฌ์ด ๊ฑฐ๋ฆฌ์˜ ์ œ๊ณฑ์œผ๋กœ ๋‚˜๋ˆˆ ๊ฐ’๊ณผ ๊ฐ™์Šต๋‹ˆ๋‹ค.
01:40
If you doubled the mass of one of the objects,
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๋ฌผ์ฒด ์ค‘ ํ•˜๋‚˜์˜ ์งˆ๋Ÿ‰์„ ๋‘ ๋ฐฐ๋กœ ํ•˜๋ฉด
01:42
the force between them would double, too.
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๊ทธ๋“ค ์‚ฌ์ด์˜ ํž˜์€ ๋‘ ๋ฐฐ๊ฐ€ ๋ฉ๋‹ˆ๋‹ค.
01:45
If the distance between them doubled,
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๊ฑฐ๋ฆฌ๊ฐ€ ๋‘ ๋ฐฐ๊ฐ€ ๋˜๋ฉด
01:47
the force would be one-fourth as strong.
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ํž˜์€ 1/4๋งŒํผ์ด ๋ฉ๋‹ˆ๋‹ค.
01:50
The gravitational force between you and the Earth pulls you towards its center,
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๋‹น์‹ ๊ณผ ์ง€๊ตฌ ์‚ฌ์ด์˜ ์ธ๋ ฅ์€ ๋‹น์‹ ๊ณผ ์ง€๊ตฌ๋ฅผ ํž˜์˜ ์ค‘์‹ฌ์œผ๋กœ ๋‹น๊น๋‹ˆ๋‹ค.
01:55
a force you experience as your weight.
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๋‹น์‹ ์ด ์ฒด์ค‘์ด๋ผ ๋Š๋ผ๋Š” ํž˜ ๋ง์ด์ง€์š”.
01:57
Letโ€™s say this force is about 800 Newtons
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์˜ˆ๋ฅผ ๋“ค์–ด, ๋‹น์‹ ์ด ํ•ด์ˆ˜๋ฉด์— ์„œ ์žˆ์„ ๋•Œ์˜ ํž˜์„
02:00
when youโ€™re standing at sea level.
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์•ฝ 800๋‰ดํ„ด์ด๋ผ ํ•ฉ์‹œ๋‹ค.
02:02
If you traveled to the Dead Sea,
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๋‹น์‹ ์ด ์‚ฌํ•ด๋กœ ์—ฌํ–‰์„ ๊ฐ”๋‹ค๋ฉด
02:04
the force would increase by a tiny fraction of a percent.
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๊ทธ ํž˜์€ ์•ฝ๊ฐ„ ์ฆ๊ฐ€ํ•ฉ๋‹ˆ๋‹ค.
02:08
And if you climbed to the top of Mount Everest, the force would decreaseโ€”
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์—๋ฒ ๋ ˆ์ŠคํŠธ์‚ฐ ์ •์ƒ์— ์˜ฌ๋ž๋‹ค๋ฉด
๊ทธ ํž˜์€ ์—ญ์‹œ ๊ทน์†Œ๋Ÿ‰ ๊ฐ์†Œํ•ฉ๋‹ˆ๋‹ค.
02:12
but again, by a minuscule amount.
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02:15
Traveling higher would make a bigger dent in gravityโ€™s influence,
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๋” ๋†’์ด ์—ฌํ–‰ํ•˜๋ฉด ์ค‘๋ ฅ์˜ ์˜ํ–ฅ์„ ๋”์šฑ ์•ฝํ•˜๊ฒŒ ํ•  ์ˆ˜ ์žˆ๊ฒ ์ง€๋งŒ
02:19
but you wonโ€™t escape it.
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์ ˆ๋Œ€ ๋ฒ—์–ด๋‚  ์ˆ˜๋Š” ์—†์Šต๋‹ˆ๋‹ค.
02:21
Gravity is generated by variations in the curvature of spacetimeโ€”
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์ค‘๋ ฅ์€ ์‚ผ์ฐจ์› ๊ณต๊ฐ„์—์„œ
์‹œ๊ฐ„์ด ๋”ํ•ด์ง„ ์‹œ๊ณต๊ฐ„์˜ ๊ณก๋ฅ  ๋ณ€ํ™”์— ์˜ํ•ด ๋ฐœ์ƒํ•ฉ๋‹ˆ๋‹ค.
02:25
the three dimensions of space plus timeโ€”
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02:28
which bend around any object that has mass.
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์งˆ๋Ÿ‰์„ ๊ฐ€์ง„ ๋ฌผ์ฒด ์ฃผ๋ณ€์ด๋ผ๋ฉด ํ•ญ์ƒ ํœ˜์–ด์ ธ ์žˆ์ง€์š”.
02:32
Gravity from Earth reaches the International Space Station,
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์ง€๊ตฌ์—์„œ์˜ ์ค‘๋ ฅ์€ ๊ฑฐ์˜ ์›๋ž˜์˜ ๊ฐ•๋„๋ฅผ ์œ ์ง€ํ•œ ์ฑ„
02:35
400 kilometers above the earth,
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400km ๋–จ์–ด์ง„ ๊ตญ์ œ ์šฐ์ฃผ ์ •๊ฑฐ์žฅ๊นŒ์ง€ ๋‹ฟ์Šต๋‹ˆ๋‹ค.
02:38
with almost its original intensity.
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02:40
If the space station was stationary on top of a giant column,
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์šฐ์ฃผ ์ •๊ฑฐ์žฅ์ด ํฐ ๊ธฐ๋‘ฅ์˜ ๊ผญ๋Œ€๊ธฐ์— ๊ณ ์ •๋˜์–ด ์žˆ๋‹ค๋ฉด
02:44
youโ€™d still experience ninety percent
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๋‹น์‹ ์€ ๋•… ์œ„์˜ ์ค‘๋ ฅ์˜ 90%๋ฅผ ๋Š๋‚„ ์ˆ˜ ์žˆ์Šต๋‹ˆ๋‹ค.
02:46
of the gravitational force there that you do on the ground.
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02:50
Astronauts just experience weightlessness
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์šฐ์ฃผ๋น„ํ–‰์‚ฌ๊ฐ€ ๋ฌด์ค‘๋ ฅ์„ ๊ฒฝํ—˜ํ•˜๋Š” ๊ฒƒ์€
02:52
because the space station is constantly falling towards earth.
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์šฐ์ฃผ ์ •๊ฑฐ์žฅ์ด ๋Š์ž„์—†์ด ์ง€๊ตฌ๋ฅผ ํ–ฅํ•ด ๋–จ์–ด์ง€๊ณ  ์žˆ์ง€๋งŒ
02:57
Fortunately, itโ€™s orbiting the planet fast enough that it never hits the ground.
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๋‹คํ–‰ํžˆ ๊ถค๋„๋ฅผ ๋„๋Š” ์†๋„๊ฐ€ ์ถฉ๋ถ„ํžˆ ๋นจ๋ผ์„œ ๋•…์— ๋–จ์–ด์งˆ ์ผ์€ ์—†์Šต๋‹ˆ๋‹ค.
03:02
By the time you made it to the surface of the moon,
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๋‹น์‹ ์ด ์•ฝ 400,000km ๋–จ์–ด์ง„ ๋‹ฌ ํ‘œ๋ฉด์— ์žˆ์„ ๋•Œ์—๋Š”
03:04
around 400,000 kilometers away,
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03:07
Earthโ€™s gravitational pull would be
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์ง€๊ตฌ์˜ ์ค‘๋ ฅ์€ ์ง€๊ตฌ์—์„œ ๋Š๋ผ๋Š” ๊ฒƒ์˜ 0.03%๋ณด๋‹ค ์ž‘์Šต๋‹ˆ๋‹ค.
03:09
less than 0.03 percent of what you feel on earth.
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03:14
The only gravity youโ€™d be aware of would be the moonโ€™s,
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๋‹น์‹ ์ด ๋Š๋‚„ ์ˆ˜ ์žˆ๋Š” ์ค‘๋ ฅ์€ ์˜ค๋กœ์ง€
03:17
which is about one sixth as strong as the earthโ€™s.
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์ง€๊ตฌ์˜ ์•ฝ 1/6 ์ •๋„์ธ ๋‹ฌ์˜ ์ค‘๋ ฅ๋ฟ์ž…๋‹ˆ๋‹ค.
03:20
Travel farther still
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๋” ๋ฉ€๋ฆฌ ์—ฌํ–‰ํ•œ๋‹ค๋ฉด
03:22
and Earthโ€™s gravitational pull on you will continue to decrease,
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์ง€๊ตฌ์˜ ์ค‘๋ ฅ์€ ๊ณ„์†ํ•ด์„œ ๊ฐ์†Œํ•˜๊ฒ ์ง€๋งŒ
03:26
but never drop to zero.
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์ ˆ๋Œ€ 0์œผ๋กœ ๋–จ์–ด์ง€์ง€ ์•Š์Šต๋‹ˆ๋‹ค.
03:28
Even safely tethered to the Earth,
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์‹ฌ์ง€์–ด ์ง€๊ตฌ์— ์•ˆ์ •์ ์œผ๋กœ ๋ถ™์–ด์žˆ์–ด๋„
03:31
weโ€™re subject to the faint tug of distant celestial bodies and nearby earthly ones.
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์šฐ๋ฆฌ๋Š” ๋จผ ์ฒœ์ฒด๋“ค๊ณผ ๊ฐ€๊นŒ์ด ์žˆ๋Š” ๊ฒƒ์— ์•ฝํ•˜๊ฒŒ๋‚˜๋งˆ ์žก์•„๋‹น๊ฒจ์ง€๋Š” ๋Œ€์ƒ์ž…๋‹ˆ๋‹ค.
03:38
The Sun exerts a force of about half a Newton on you.
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ํƒœ์–‘์€ 0.5๋‰ดํ„ด ์ •๋„์˜ ํž˜์„ ํ–‰์‚ฌํ•ฉ๋‹ˆ๋‹ค.
03:41
If youโ€™re a few meters away from a smartphone, you'll experience
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์Šค๋งˆํŠธํฐ์—์„œ ์ˆ˜ ๋ฏธํ„ฐ ๋–จ์–ด์ ธ ์žˆ๋‹ค๋ฉด
03:44
a mutual force of a few piconewtons.
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๋‹น์‹ ์€ ์ž‘์€ ํ”ผ์ฝ”๋‰ดํ„ด์˜ ํž˜์„ ๋ฐ›์Šต๋‹ˆ๋‹ค.
03:48
Thatโ€™s about the same as the gravitational pull
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์ด๊ฒƒ์€ 250๋งŒ ๊ด‘๋…„ ๋–จ์–ด์ง„
03:50
between you and the Andromeda Galaxy,
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ํƒœ์–‘์˜ 1์กฐ๋ฐฐ์— ๋‹ฌํ•˜๋Š” ํฌ๊ธฐ๋ฅผ ๊ฐ€์ง„
03:53
which is 2.5 million light years away
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์•ˆ๋“œ๋กœ๋ฉ”๋‹ค ์„ฑ์šด๊ณผ ๋‹น์‹  ์‚ฌ์ด์˜ ์ธ๋ ฅ๊ณผ ๊ฐ™์Šต๋‹ˆ๋‹ค.
03:56
but about a trillion times as massive as the sun.
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04:00
But when it comes to escaping gravity,
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๊ทธ๋Ÿฌ๋‚˜ ์ค‘๋ ฅ์œผ๋กœ๋ถ€ํ„ฐ ๋ฒ—์–ด๋‚  ์ˆ˜ ์žˆ๋Š”
04:02
thereโ€™s a loophole.
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ํ•œ ๋ฐฉ๋ฒ•์ด ์žˆ์Šต๋‹ˆ๋‹ค.
04:04
If all the mass around us is pulling on us all the time,
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์šฐ๋ฆฌ ์ฃผ์œ„์— ์žˆ๋Š” ๋ชจ๋“  ์งˆ๋Ÿ‰์ด ํ•ญ์ƒ ์šฐ๋ฆฌ๋ฅผ ๋Œ์–ด๋‹น๊ธฐ๊ณ  ์žˆ๋‹ค๋ฉด
04:07
how would Earthโ€™s gravity change
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๋งŒ์•ฝ ํ‘œ๋ฉด ์•„๋ž˜๋กœ ๊นŠ์ด ํ„ฐ๋„์„ ๋šซ์œผ๋ฉด
04:09
if you tunneled deep below the surface,
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์ง€๊ตฌ์˜ ์ค‘๋ ฅ์€ ์–ด๋–ป๊ฒŒ ๋ณ€ํ• ๊นŒ์š”?
04:11
assuming you could do so without being cooked or crushed?
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๊ตฌ์›Œ์ง€๊ฑฐ๋‚˜ ์ฐŒ๊ทธ๋Ÿฌ์ง€์ง€ ์•Š๊ณ  ํ•ด๋‚ผ ์ˆ˜ ์žˆ๋‹ค๋ฉด ๋ง์ด์ง€์š”.
04:15
If you hollowed out the center of a perfectly spherical Earthโ€”
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์ง€๊ตฌ๊ฐ€ ์™„๋ฒฝํ•˜๊ฒŒ ๋‘ฅ๊ธ€๋‹ค๊ณ  ๊ฐ€์ •ํ•˜๊ณ  ๋งŒ์•ฝ ๊ทธ ์ค‘์‹ฌ์„ ํŒŒ์„œ ๋“ค์–ด๊ฐ„๋‹ค๋ฉด
04:19
which it isnโ€™t, but letโ€™s just say it wereโ€”
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04:22
youโ€™d experience an identical pull from all sides.
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๋‹น์‹ ์€ ๋ชจ๋“  ๋ฐฉํ–ฅ์—์„œ ๋™์ผํ•œ ์ค‘๋ ฅ์„ ๊ฒฝํ—˜ํ•  ์ˆ˜ ์žˆ์Šต๋‹ˆ๋‹ค.
04:25
And youโ€™d be suspended, weightless,
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๊ทธ๋ฆฌ๊ณ  ๋‹น์‹ ์€ ๋ฌด์ค‘๋ ฅ ์ƒํƒœ๋กœ ์ •์ง€๋  ๊ฒƒ์ด๊ณ 
04:28
only encountering the tiny pulls from other celestial bodies.
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๋‹ค๋ฅธ ์ฒœ์ฒด๋กœ๋ถ€ํ„ฐ์˜ ์ž‘์€ ๋‹น๊น€๋งŒ ๋Š๋‚„ ์ˆ˜ ์žˆ์Šต๋‹ˆ๋‹ค.
04:32
So you could escape the Earthโ€™s gravity in such a thought experimentโ€”
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๋”ฐ๋ผ์„œ ์ค‘๋ ฅ์„ ํƒˆ์ถœํ•˜๋ ค๋ฉด
04:36
but only by heading straight into it.
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์ •๋ฉด๋ŒํŒŒ ํ•˜๋Š” ๋ฒ•๋ฐ–์— ์—†๊ฒ ๊ตฐ์š”.
์ด ์›น์‚ฌ์ดํŠธ ์ •๋ณด

์ด ์‚ฌ์ดํŠธ๋Š” ์˜์–ด ํ•™์Šต์— ์œ ์šฉํ•œ YouTube ๋™์˜์ƒ์„ ์†Œ๊ฐœํ•ฉ๋‹ˆ๋‹ค. ์ „ ์„ธ๊ณ„ ์ตœ๊ณ ์˜ ์„ ์ƒ๋‹˜๋“ค์ด ๊ฐ€๋ฅด์น˜๋Š” ์˜์–ด ์ˆ˜์—…์„ ๋ณด๊ฒŒ ๋  ๊ฒƒ์ž…๋‹ˆ๋‹ค. ๊ฐ ๋™์˜์ƒ ํŽ˜์ด์ง€์— ํ‘œ์‹œ๋˜๋Š” ์˜์–ด ์ž๋ง‰์„ ๋”๋ธ” ํด๋ฆญํ•˜๋ฉด ๊ทธ๊ณณ์—์„œ ๋™์˜์ƒ์ด ์žฌ์ƒ๋ฉ๋‹ˆ๋‹ค. ๋น„๋””์˜ค ์žฌ์ƒ์— ๋งž์ถฐ ์ž๋ง‰์ด ์Šคํฌ๋กค๋ฉ๋‹ˆ๋‹ค. ์˜๊ฒฌ์ด๋‚˜ ์š”์ฒญ์ด ์žˆ๋Š” ๊ฒฝ์šฐ ์ด ๋ฌธ์˜ ์–‘์‹์„ ์‚ฌ์šฉํ•˜์—ฌ ๋ฌธ์˜ํ•˜์‹ญ์‹œ์˜ค.

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