Observing the Universe
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- Delilah Stewart
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1 Observing the Universe Let s talk about Stars!
2 Thank you! OAD East Asian Regional Node
3 Welcome!
4
5 Stars Massive, luminous ball of gas and plasma Produces its own energy through nuclear fusion Simplest type: H into He, that is how all stars start off and spend most of their life (main sequence) Astronomers can determine the mass, age, chemical composition and many other properties of a star by observing its spectrum, luminosity and motion through space. The total mass determines its evolution.
6 LIGHT YEARS AWAY... What is a light year?
7 Our Sun
8 How far?
9 AU: Astronomical Unit
10 Brightness and Magnitudes The first known catalogue: Hipparchus in about 120 BC It was later edited and increased to 1022 stars by Ptolemy in a famous catalogue known as the "Almagest (140 AD)
11 Brightness and Magnitudes Hipparchus listed the stars that could be seen in each constellation, described their positions, and rated their brightness on a scale of 1 to 6, the brightest being 1. This method of describing the brightness of a star survives today. Of course, Hipparchus had no telescope, and so could only see stars as dim as 6th magnitude Today we can see stars with large telescopes down to about 30th magnitude.
12 Brightness and Magnitudes Each magnitude is about 2.5 times brighter than the next greater magnitude. This means a difference in magnitudes of 5 units (from magnitude 1 to magnitude 6, for example) corresponds to a change in brightness of 100 times. With equipment to make more accurate measurements, astronomers were able to assign stars decimal values, like 2.75, rather than rounding off to magnitude 2 or 3.
13 Brightness and Magnitudes There are stars brighter than magnitude 1. The star Vega (alpha Lyrae) has a visual magnitude of 0. There are a few stars brighter than Vega. Their magnitudes will be negative. Astronomers usually refer to "apparent magnitudes", that is, how bright a star appears to us here at Earth. Apparent magnitudes are often written with a lower case "m" (like 3.24m).
14 Brightness and Magnitudes The brightness of a star depends not only on how bright it actually is, but also on how far away it is Therefore, astronomers developed the "absolute" brightness scale. Absolute magnitude is defined as how bright a star would appear if it were exactly 10 parsecs (about 33 light years) away from Earth.
15 Brightness and Magnitudes The brightness of a star depends not only on how bright it actually is, but also on how far away it is Therefore, astronomers developed the "absolute" brightness scale. Absolute magnitude is defined as how bright a star would appear if it were exactly 10 parsecs (about 33 light years) away from Earth. So what is a parsec??? After the light year and the AU, yet another distance unit...
16 Sun Earth Orbit 1 Parsec 1 arcminute 1
17 Distances for nearby stars: parallaxes Parallax of 1 corresponds to a distance of 1 pc. Sun Earth Orbit 1 Parsec (pc) = AU 1 AU = km 1 Parsec Proxima Centauri, p = 0,762 has the largest parallax 1 arcminute 1 Entfernung: d = 1/p = 1,3 pc
18 Brightness and Magnitudes
19 Brightness and Magnitudes Sun: apparent magnitude of (because it's very, very close) and an absolute magnitude of Absolute magnitudes are often written with a capital (upper case) "M".
20 Brightness and Magnitudes standard distance is 10 parsecs (about light years, or kilometres).
21 Brightness and magnitude Some examples: (apparent magnitudes) Sun: Full Moon: -12 Sirius: -1.5 With binoculars: down to +10 Pluto: +14 With large telescopes: down to +30
22 Stars
23 Our Sun
24 Our Star, the Sun Mass: Radius: Luminosity: Surface temperature: M = 1, kg R = km L = 3, Watt T surf = 5700 K Distance (from Earth): (Beginning of January) d MIN = 147, km (Beginning of July) d MAX = 152, km Diameter seen from Earth: a = bis Apparent magnitude: m v = -26 m,7 Absolute magnitude: M v = 4 m,87
25 Our Sun Local magnetic fields Solar spots K cooler Live up to a few months, Size up to km
26 Our Sun
27 Our Sun Mercury transits the Sun (2006)
28 Count the solar spots
29 Our Sun 11-year cycle Cycle start: activity minimum Sunspot number
30 Our Sun Solar cycle No. 1 Solar cycle No. 22 Sunspot number
31 Our Sun Solar cycle No. 1 Solar cycle No. 23 Solar cycle No. 22 Sunspot number
32 Our Sun Sunspot latitude and size
33 Our Sun
34 Our Sun
35 Our Sun
36 Aurora (borealis or australis)
37 Aurora (borealis or australis)
38
39 Light
40 Spectra Doppler effect
41 Spectra
42 Stars
43
44 Stars Betelgeuse ORION Rigel
45 The Hertzsprung-Russell diagram Brightness Temperature
46 The Hertzsprung-Russell diagram Used to classify stars Luminosity and Absolute Magnitude: how bright is the star? Spectral Class and Temperature: how hot is the star?
47 The Hertzsprung-Russell diagram Main Sequence
48 The Hertzsprung-Russell diagram
49
50 Our Sun Diamond ring
51 Our Sun Partial eclipse
52 Our Sun Annular eclipse
53 More on Stars tomorrow degree photographic panorama of our entire galaxy, the Milky Way, from the viewpoint of the solar system
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