Henry Norris Russell Lectureship
Henry Norris Russell Lectureship
Henry Norris Russell oor Spaans
Henry Norris Russell
en
United States astronomer who developed a theory of stellar evolution (1877-1957)
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Henry Norris Russell
In 1924, Henry Norris Russell was the dean of American astronomers, having made major contributions to our understanding of the stars.
En 1924, Henry Norris Russell era el decano de los astrónomos estadounidenses, tras hacer grandes contribuciones a nuestro entendimiento de las estrellas.
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But in 1910, Princeton astronomer Henry Norris Russell noticed something that cast doubt on that rule.
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Princeton’s Henry Norris Russell felt drawn to the same pursuit.
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John Wheeler, Henry Norris Russell, John Von Neumann, Wolfgang Pauli, gathered to hear Feynman.
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In 1937 it went to Charlotte Moore Sitterly, who was Henry Norris Russell’s personal computer.
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As Henry Norris Russell put it, "Nebulium has vanished into thin air."
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Henry Norris Russell was born in Oyster Bay, New York, on 25 October 1877.
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“We’ve all been affected,” said Henry Norris Russell.
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He dedicated the book “To the memory of Henry Norris Russell.”
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Henry Norris Russell, the great, famous astronomer of the day was coming to the lecture!
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The woman next to Miss Cannon is Lucy May Russell, wife of Henry Norris Russell, who is at her side.
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By 1913, Henry Norris Russell had developed the theory of eclipsing binaries, and Stebbins realized that there were many undiscovered ones.
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In 1924, Henry Norris Russell was the dean of American astronomers, having made major contributions to our understanding of the stars.
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In the early 20th century, Henry Norris Russell proposed that rather than being a new element, the line at 500.7 nm was due to a familiar element in unfamiliar conditions.
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Fowler won the Henry Norris Russell Lectureship of the American Astronomical Society in 1963, the Vetlesen Prize in 1973, the Eddington Medal in 1978, the Bruce Medal of the Astronomical Society of the Pacific in 1979, and the Nobel Prize in Physics in 1983 for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe (shared with Subrahmanyan Chandrasekhar).
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The Hertzsprung-Russell diagram is named after its creators, astronomers Ejnar Hertzsprung and Henry Norris Russell.
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Ejnar Hertzsprung and Henry Norris Russell independently constructed the first such plots nearly a century ago, and they are therefore today called Hertzsprung-Russell diagrams, or H-R diagrams.
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In the early 20th century, Henry Norris Russell proposed that rather than being a new element, the line at 500.7 nm was due to a familiar element in unfamiliar conditions.[7]
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Notable awards Gold Medal of the Royal Astronomical Society Henry Norris Russell (October 25, 1877 – February 18, 1957) was an American astronomer who, along with Ejnar Hertzsprung, developed the Hertzsprung–Russell diagram (1910).
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The diagram was created circa 1910 by Ejnar Hertzsprung and Henry Norris Russell and represents a major step towards an understanding of stellar evolution or "the way in which stars undergo sequences of dynamic and radical changes over time".
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The hottest stars are class O, while the coolest are class T. Two astronomers, Ejnar Hertzsprung and Henry Norris Russell, independently started to wonder what would happen if they compared stars' luminosities to their spectral classifications (or, alternatively, to their temperatures).
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Fowler won the Henry Norris Russell Lectureship of the American Astronomical Society in 1963, the Vetlesen Prize in 1973, the Eddington Medal in 1978, the Bruce Medal of the Astronomical Society of the Pacific in 1979, and the Nobel Prize in Physics in 1983 for his theoretical and experimental studies of the nuclear reactions of importance in the formation of the chemical elements in the universe (shared with Subrahmanyan Chandrasekhar).
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The first white dwarf discovered was in the triple star system of 40 Eridani, which contains the relatively bright main sequence star 40 Eridani A, orbited at a distance by the closer binary system of the white dwarf 40 Eridani B and the main sequence red dwarf 40 Eridani C. The pair 40 Eridani B/C was discovered by William Herschel on 31 January 1783.[10] In 1910, Henry Norris Russell, Edward Charles Pickering and Williamina Fleming discovered that, despite being a dim star, 40 Eridani B was of spectral type A, or white.[11] In 1939, Russell looked back on the discovery:[3], p.
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22 sinne gevind in 12 ms. Hulle kom uit baie bronne en word nie nagegaan nie.