Gmat before the 1920s, there was a long-standing debate about the nebulae that are visible between galaxies. When viewed from a terrestrial telescope, they appear to be gas and dust emissions. In 1927, however, the team of edwin hubble theorized that these nebulae are actually star systems. The bulk of hubble’s evidence came from the analysis of gamma rays in the range of invisible light called 1019
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By the mid-1920s, most scientists thought that the Milky Way was the whole universe, and that the universe was static, immutable. With two discoveries announced in January 1925 and January 1929, astronomer Edwin Hubble originally changed our idea of the universe, indicating that the universe was bigger than the first thought, and the other is expanding it It was growing bigger and bigger all the time.
Edwin Hubble was born in Missouri in 188 9. As a young man, he was tall and athletic, specially known for his talent in boxing, basketball and track. He earned a bachelor's degree in mathematics and astronomy at the University of Chicago, and after his father's wishes, studied law at the Rhodes Scholarship in Oxford. Hubble returned to the US and joined the Kentucky bar, but quickly decided that the law was not for him. He taught high school Spanish for a year before returning to the University of Chicago to earn a PhD in Astronomy in 1917. After serving in the Army in World War I, he went to Southern California to work in Mount. Wilson Observatory, home of the 100-inch Hooker Telescope, is the largest in the world at the time.
In the beginning of the 1920s, many astronomers believed that objects going through the name of Obboola were the nearby gas clouds in our galaxy, and the galaxies were the whole universe, while others thought that the nebula was actually more The far "island universal" was different from our galaxy. In 1920, there was a famous debate on this issue by Harlo Shepali and Heber Curtis [Physics History, see this month in April 2000].
Wilson at Mount, Hubble began to measure the distance of Nebula to solve this issue by using a method based on Henrieta Levitt's first find. He had found that there was an approximate relationship between a type of star known as the Safed Variable, its brightness and its pulse rate. Measuring the duration of the star's fluctuation in brightness will give its full brightness, and compare it with a clear glow of the star and provide a measure of the star's distance.