Milky Way Minis

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Do you wonder how many syns you have? If you have forgotten what your consultant told you or perhaps you are following the plan at home and don’t know how many syns you should have then I have an article of all you need to know about that. Around the same time, the young astronomer Harlow Shapley began measuring the distribution of globular clusters — compact and dense spheres of stars. By 1918, he had found that the clusters centered around the constellation Sagittarius, forming a halo around the Milky Way. He also made improved parallax measurements of Cepheid variables, which in turn improved the calibration of Leavitt’s relation.

We livein the Milky Way Galaxy. If you were looking down on the Milky Way, it would look like a large pinwheel rotating in space. Our Galaxy is a spiral galaxy that formed approximately 14 billion years ago. Contained in the Milky Way are stars, clouds of dust and gas called nebulae, planets, and asteroids. Stars, dust, and gas fan out from the center of the Galaxy in long spiraling arms. The Milky Way is approximately 100,000 light-years in diameter. Our solar system is 26,000 light-years from the center of the Galaxy. All objects in the Galaxy revolve around the Galaxy's center. It takes 250 million years for our Sun (and the Earth with it) to make one revolution around the center of the Milky Way.If you have your healthy extra b choice available still then you might consider having something on toast, there are lots of choices under 5 syns you could try. After achieving overnight fame in 1781 when he discovered Uranus, William Herschel was swiftly appointed as King George III’s court astronomer. The king gave him money to build telescopes, including his 40-foot-long (12 meters) telescope with a 48-inch mirror. The dust clouds of the Galaxy are narrowly limited to the plane of the Milky Way, though very low-density dust can be detected even near the galactic poles. Dust clouds beyond 2,000 to 3,000 light-years from the Sun cannot be detected optically, because intervening clouds of dust and the general dust layer obscure more distant views. Based on the distribution of dust clouds in other galaxies, it can be concluded that they are often most conspicuous within the spiral arms, especially along the inner edge of well-defined ones. The best-observed dust clouds near the Sun have masses of several hundred solar masses and sizes ranging from a maximum of about 200 light-years to a fraction of a light-year. The smallest tend to be the densest, possibly partly because of evolution: as a dust complex contracts, it also becomes denser and more opaque. The very smallest dust clouds are the so-called Bok globules, named after the Dutch American astronomer Bart J. Bok; these objects are about one light-year across and have masses of 1–20 solar masses.

Of course, there are many things you can break or cut a piece off to fall within five syns or less but these are actual bars you can get for this allowance. From our vantage point on Earth, the Milky Way looks like a band of diffuse light that arcs across the nighttime sky. This is where the English name comes from: The Romans called it Via Lactea and envisioned it as a band of spilled milk. Astronomers and philosophers debated the nature of the Milky Way until Galileo Galilei first observed it with a telescope and found that the light of the Milky Way comes from innumerable distant stars. The stars themselves are too far away to see all of them individually, but their combined light gives the familiar band.H II regions are found in the plane of the Galaxy intermixed with young stars, stellar associations, and the youngest of the open clusters. They are areas where very massive stars have recently formed, and many contain the uncondensed gas, dust, and molecular complexes commonly associated with ongoing star formation. The H II regions are concentrated in the spiral arms of the Galaxy, though some exist between the arms. Many of them are found at intermediate distances from the centre of the Milky Way Galaxy, with the largest number occurring at a distance of 10,000 light-years. This latter fact can be ascertained even though the H II regions cannot be seen clearly beyond a few thousand light-years from the Sun. They emit radio radiation of a characteristic type, with a thermal spectrum that indicates that their temperatures are about 10,000 kelvins. This thermal radio radiation enables astronomers to map the distribution of H II regions in distant parts of the Galaxy. The dust is accompanied by gas, which is thinly dispersed among the stars, filling the space between them. This interstellar gas consists mostly of hydrogen in its neutral form. Radio telescopes can detect neutral hydrogen because it emits radiation at a wavelength of 21 cm. Such radio wavelength is long enough to penetrate interstellar dust and so can be detected from all parts of the Galaxy. Most of what astronomers have learned about the large-scale structure and motions of the Galaxy has been derived from the radio waves of interstellar neutral hydrogen. The distance to the gas detected is not easily determined. Statistical arguments must be used in many cases, but the velocities of the gas, when compared with the velocities found for stars and those anticipated on the basis of the dynamics of the Galaxy, provide useful clues as to the location of the different sources of hydrogen radio emission. Near the Sun the average density of interstellar gas is 10 −21 gm/cm 3, which is the equivalent of about one hydrogen atom per cubic centimetre.