[IAU자료실]
IAU100] 특별전시자료 Decade2
2019-01-11
IAU100] Above & Beyond Exhibition Decade2 ai자료 압축파일 입니다.
D02.1.1.R_HBML What are stars
WHAT ARE STARS?
Stars are glowing spheres of gas. Cecillia Payne-Gaposchkin was the first to suggest that stars are primarily made of hydrogen and helium in 1925. At a star’s centre is a dense, burning core where nuclear fusion occurs. Anticipated by Arthur Eddington in the 1920s, the nuclear process that power stars would only be fully proven in the late 1930s by Hans Bethe.
STELLAR ENERGY
We long wondered what makes stars shine ? Fire? Coal? To explain what fuels a star, physicists first set out to understand the structure of atoms to uncover the hidden power of nuclear reactions. Stars shine because of these reactions at their core. In 1937, the work of Hans Bethe shed light on the different ways hydrogen can fuse into helium. This meant that the origin and nature of stars was no longer a complete mystery. Further studies contributed to developing the theory of stellar nucleosynthesis, which explains how different chemical elements are forged through different nuclear fusion reactions at different stages of a star’s life-cycle.
CHANDRASEKHAR LIMIT - 1,4 M
Named after the Indian-American astrophysicist Subrahmanyan Chandrasekhar, the Chandrasekhar limit is an important value for astronomy. He determined that a compact, evolved star (known as a white dwarf) is 1.4 times more massive than our Sun is too massive to remain stable. After this limit, the force of gravity causes the white dwarf star to collapse into a dense core remnant or even a black hole.
D02.1.2.INFO and others_HBML info board
(PREVIEW)
HUBBLE-LEMAITRE LAW
Thanks to Albert Einstein and his equations of General Relativity, we finally had the tools to study the Universe on the largest scales. Subsequent studies by Georges Lemaitre suggested that space is expanding: every point in space, for example every galaxy, grows further apart from each other as time passes. This was soon confirmed by the observations of Edwin Hubble and collaborators, who proved the expansion of the Universe in 1929. They observed that the further galaxies are, the faster they move apart. This relationship was called the "Hubble constant" and was initially estimated by Hubble at 500 km/s/Mpc*, but has since been narrowed to 73.5 km/s/Mpc at the turn of the 21st century.
*A parsec is a unit used to express distances in space. One parsec is equal to 3.26 light-years.
(PREVIEW)
HUBBLE-LEMAITRE LAW
Thanks to Albert Einstein and his equations of General Relativity, we finally had the tools to study the Universe on the largest scales. Subsequent studies by Georges Lemaitre suggested that space is expanding: every point in space, for example every galaxy, grows further apart from each other as time passes. This was soon confirmed by the observations of Edwin Hubble and collaborators, who proved the expansion of the Universe in 1929. They observed that the further galaxies are, the faster they move apart. This relationship was called Hubble law and introduced the Hubble constant, initially estimated at 500 km/s/Mpc*, since then narrowed to 73.5 km/s/Mpc at the turn of the 21st century.
*A parsec (pc) is a unit used to express distances in space. One parsec is equal to 3.26 light-years. A megaparsec (Mpc) is equal to a million parsecs.
D02.2.1.A._.D02.2.1.R_D02.2.2._Radioastronomy
UNIVERSE IN RADIO WAVES
KARL JANSKY EXPLAINING SOURCE OF RADIO EMISSION
Credit: Bell Laboratories / Nokia Corporation
ANTENNAS OF MEERKAT RADIO TELESCOPE WHICH IS A PRECURSOR TO THE SQUARE KILOMETRE ARRAY
Credit: South African Radio Astronomy Observatory (SARAO)
UNIVERSE IN RADIO WAVES
RADIO ANTENNA USED BY KARL JANSKY TO DISCOVER RADIO EMISSION AT THE CENTER OF THE MILKY WAY
There is more to the Universe than meets the eye. The development of radio astronomy became a key step in strengthening our toolkit for studying the Universe. In 1933, Karl Jansky
was busy developing the trans-Atlantic radio telephone service when he accidentally detected radio signals coming from a distance source: the centre of the Milky Way. This lead to important developments of radio techniques, primarily during World War II, that forged our modern telecommunications landscape and opened new ways of perceiving the Universe. As a result, we have since discovered pulsars, quasars, radio galaxies, and many other extreme cosmic environments and events.
Credit: Bell Laboratories / Nokia Corporation
D02.3.1._The War of the Worlds
THE WAR OF THE WORLDS
In 1938, the radio adaptation of H.G. Wells’ book "The War of the Worlds", narrated and directed by Orson Welles, allegedly caused widespread panic in the USA. The narration convinced listeners across the country that a Martian invasion of Earth was taking place. This realistic radio dramatisation of the 1897 science fiction novel describing the alien attack was taken by some as genuine news during the tension prior to World War II.
Credit:
01. Alvim Correa, 02. Chicago Herald Examiner, 03. Daily News,
04. Associated Press
D02.1.1.R_HBML What are stars
WHAT ARE STARS?
Stars are glowing spheres of gas. Cecillia Payne-Gaposchkin was the first to suggest that stars are primarily made of hydrogen and helium in 1925. At a star’s centre is a dense, burning core where nuclear fusion occurs. Anticipated by Arthur Eddington in the 1920s, the nuclear process that power stars would only be fully proven in the late 1930s by Hans Bethe.
STELLAR ENERGY
We long wondered what makes stars shine ? Fire? Coal? To explain what fuels a star, physicists first set out to understand the structure of atoms to uncover the hidden power of nuclear reactions. Stars shine because of these reactions at their core. In 1937, the work of Hans Bethe shed light on the different ways hydrogen can fuse into helium. This meant that the origin and nature of stars was no longer a complete mystery. Further studies contributed to developing the theory of stellar nucleosynthesis, which explains how different chemical elements are forged through different nuclear fusion reactions at different stages of a star’s life-cycle.
CHANDRASEKHAR LIMIT - 1,4 M
Named after the Indian-American astrophysicist Subrahmanyan Chandrasekhar, the Chandrasekhar limit is an important value for astronomy. He determined that a compact, evolved star (known as a white dwarf) is 1.4 times more massive than our Sun is too massive to remain stable. After this limit, the force of gravity causes the white dwarf star to collapse into a dense core remnant or even a black hole.
D02.1.2.INFO and others_HBML info board
(PREVIEW)
HUBBLE-LEMAITRE LAW
Thanks to Albert Einstein and his equations of General Relativity, we finally had the tools to study the Universe on the largest scales. Subsequent studies by Georges Lemaitre suggested that space is expanding: every point in space, for example every galaxy, grows further apart from each other as time passes. This was soon confirmed by the observations of Edwin Hubble and collaborators, who proved the expansion of the Universe in 1929. They observed that the further galaxies are, the faster they move apart. This relationship was called the "Hubble constant" and was initially estimated by Hubble at 500 km/s/Mpc*, but has since been narrowed to 73.5 km/s/Mpc at the turn of the 21st century.
*A parsec is a unit used to express distances in space. One parsec is equal to 3.26 light-years.
(PREVIEW)
HUBBLE-LEMAITRE LAW
Thanks to Albert Einstein and his equations of General Relativity, we finally had the tools to study the Universe on the largest scales. Subsequent studies by Georges Lemaitre suggested that space is expanding: every point in space, for example every galaxy, grows further apart from each other as time passes. This was soon confirmed by the observations of Edwin Hubble and collaborators, who proved the expansion of the Universe in 1929. They observed that the further galaxies are, the faster they move apart. This relationship was called Hubble law and introduced the Hubble constant, initially estimated at 500 km/s/Mpc*, since then narrowed to 73.5 km/s/Mpc at the turn of the 21st century.
*A parsec (pc) is a unit used to express distances in space. One parsec is equal to 3.26 light-years. A megaparsec (Mpc) is equal to a million parsecs.
D02.2.1.A._.D02.2.1.R_D02.2.2._Radioastronomy
UNIVERSE IN RADIO WAVES
KARL JANSKY EXPLAINING SOURCE OF RADIO EMISSION
Credit: Bell Laboratories / Nokia Corporation
ANTENNAS OF MEERKAT RADIO TELESCOPE WHICH IS A PRECURSOR TO THE SQUARE KILOMETRE ARRAY
Credit: South African Radio Astronomy Observatory (SARAO)
UNIVERSE IN RADIO WAVES
RADIO ANTENNA USED BY KARL JANSKY TO DISCOVER RADIO EMISSION AT THE CENTER OF THE MILKY WAY
There is more to the Universe than meets the eye. The development of radio astronomy became a key step in strengthening our toolkit for studying the Universe. In 1933, Karl Jansky
was busy developing the trans-Atlantic radio telephone service when he accidentally detected radio signals coming from a distance source: the centre of the Milky Way. This lead to important developments of radio techniques, primarily during World War II, that forged our modern telecommunications landscape and opened new ways of perceiving the Universe. As a result, we have since discovered pulsars, quasars, radio galaxies, and many other extreme cosmic environments and events.
Credit: Bell Laboratories / Nokia Corporation
D02.3.1._The War of the Worlds
THE WAR OF THE WORLDS
In 1938, the radio adaptation of H.G. Wells’ book "The War of the Worlds", narrated and directed by Orson Welles, allegedly caused widespread panic in the USA. The narration convinced listeners across the country that a Martian invasion of Earth was taking place. This realistic radio dramatisation of the 1897 science fiction novel describing the alien attack was taken by some as genuine news during the tension prior to World War II.
Credit:
01. Alvim Correa, 02. Chicago Herald Examiner, 03. Daily News,
04. Associated Press
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Decade2.zip