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Astrophysics is Easy!: An Introduction for the Amateur by Michael Inglis

By Michael Inglis

I used to like day-dreaming approximately house while i used to be a child. This publication makes me think that feel of ask yourself and amazement back - and that i can comprehend so much of it! I spent an afternoon on the planetarium in ny, and that i felt like i may convey my very own lecture to the viewers. And the simplest factor is - i purchased this for my son, and we proportion our curiosity in and awe for the universe.

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9m F0 I −52 41 Nov-Dec-Jan Carina This is the second brightest star in the sky. Its color is often reported as orange or yellow, as it is usually seen low down in the sky, and hence it is more likely to be affected by the atmosphere. Its true color is white. 6m F3 I −46 39 Dec-Jan-Feb Vela This star is unremarkable except that its luminosity is estimated to be 180,000 times that of the Sun! 28 M An easily resolvable double star, nice faint yellow and pale blue. 7m F4 IV 1 −15 60 Apr-May-Jun Libra is a spectroscopic binary.

When hydrogen gas is heated to a high temperature, the number of collisions between atoms can continually bump electrons to higher energy levels, and an emission line spectrum results. This consists of the photons that are emitted as each electron falls back to lower levels. The origins of the absorption lines are due to the differing amounts of elements in the cooler atmosphere of the stars (recall that in addition to hydrogen and 24 Astrophysics is Easy helium, there are other elements, or metals, present, but in minute quantities).

This is called an objective spectroscope. , information about the stars), but initial measurements can be made. The transitions shown are only a few of the many that occur. The reason that stars follow the order OBAFGKM was discovered by a brilliant astronomer, Cecilia Payne-Gaposchkin. She found that all stars are made primarily of hydrogen and helium and that a star’s surface temperature determines the strength of its spectral lines. For instance, O stars have weak hydrogen lines because, due to their high temperature, nearly all the hydrogen is ionized.

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