Lecture 36

1. Telescopes (continued). Basic Properties of Stars. Observatories and Spacecrafts Stellar Brightness, Distances, Luminosities Lecture 36 Chapter 17.8  17.16

2. Refractors

3. Refractors

4. Reflectors

5. Reflectors

6. Types of Telescopes Optical and Infrared telescopes Radio telescopes (use metal “mirrors”) Interferometeres (link several separate telescopes together to improve angular resolution)

7. Observatories

8. Radiotelescopes

9. Satellites • The first satellite  1957 Soviet Sputnik • First astronomical satellites  late 1960’s • The Hubble Space Telescope (HST)  1990 • The X-ray Chandra Observatory  1999 • The Spitzer Space (IR) Observatory  2003

10. Satellites

11. Important Stellar Parameters Stars have similar internal structures and energy sources. The most important parameter, which causes differences in a star’s appearance, is its mass. The mass determines the star’s lifetime, surface temperature, radius, and luminosity at any moment. Astronomers classify stars according their luminosities and surface temperatures.

12. Stellar Luminosity Luminosity is the total amount of power the star radiates into space. It is measured in power units (Watts). Brightness of a star in the sky depends on the distance towards a star and its luminosity. The apparent brightness is the amount of light reaching us per unit area.

13. Apparent Brightness Apparent brightness obeys an inverse square law with distance. At the distance of Jupiter is 5 A.U., the Sun is 25 times dimmer than on Earth. Alpha Centauri radiates almost the same amount of light as the Sun, but it is located 27,000 times further away from Earth than the Sun. Thus, its apparent brightness is 70 billion times less than that of the Sun.

14. The Inverse Square Law for Light

15. Luminosity – Distance Relation Luminosity Apparent brightness = ------------------- 4 π (distance)2 The units of apparent brightness are Watts per square meter. Luminosity is also measured in the units of solar luminosity (LSun = 3.8 1026 Watts).

16. Measuring the Apparent Brightness Stars emit radiation of all wavelengths. No detector is sensitive to the entire spectrum. Usually we measure apparent brightness in a small range of the complete spectrum. Eyes are sensitive to visible light. When we measure the apparent brightness in the visible region, we can calculate only the visiblelight luminosity.

17. Stellar Parallax Parallax is the annual shift in a star’s apparent position in the sky due to the Earth’s orbital motion. The parallax angle is half the annual shift. The parallax angle of the nearest star, Proxima Centauri, is 0.77 arcseconds.

18. Parsec An object with a parallax of 1 arcsecond is located at the distance of 1 parsec. 1 pc = 3.26 light-years = 3.09 1013 km 1 d (in parsecs) = -------------------------- p (in arcseconds)

19. Stellar Magnitudes Historically stellar brightness is described in magnitudes suggested by Hipparchus. The brightest stars received the designation ‘’first magnitude’’, the next brightest ‘’second magnitude’’, etc. The faintest stars visible by the naked eye are ‘’sixth magnitude’’.

20. Stellar Magnitudes The modern magnitudes system is more precisely defined. Since a star may have any brightness, fractional apparent magnitudes are possible. For example, a star of magnitude 1.00 is 2.5 times brighter than a star of magnitude 2.00. The brightest star in the sky is Sirius with an apparent brightness of –1.46. The faintest stars observed with HST are of ~ 30th magnitudes.

21. Surface Temperature Surface temperature determines a star’ color. The coolest stars are red, the hottest ones are blue. Only the brightest star colors can be recognized by the naked eye. The color can be determined better by comparing a star’s brightness in different filters. Betelgeuse has a temperature of ~3,400 K, Sirius ~9,400 K, the hottest stars – up to 100,000 K.

22. Spectral Type The surface temperature also determines the line spectrum of a star. Hot stars display lines of highly ionized elements, while cool stars show molecular lines. Stars are classified by assigning a spectral type. The hottest stars are called spectral type O, followed by B, A, F, G, K, M as the surface temperature declines. Oh Be A Fine Girl, Kiss Me

23. Stellar Masses It is harder to measure stellar masses. The best method is to apply Kepler’s third law in combination with Newton’s law of gravity. This procedure can only be applied to orbiting objects: Visual binary – a resolved pair of stars (Mizar) Eclipsing binary – a pair orbiting in the plane of our line of sight Spectroscopic binary – an object with regularly moving spectral lines or with 2 line systems.

24. The Hertzsprung-Russell Diagram Invented by Ejnar Hertzsprung (Denmark) and Henry Norris Russell (USA) in 1912. The diagram is a plot of stellar luminosities against their surface temperatures. Temperature increases leftward. Luminosity increases upward. H-R diagram

25. Patterns in the H-R diagram Main sequence – location of the most stars (from upper left to lower right corner) Luminosity class V Supergiant branch – along the top (class I) Giant branch – just below the supergiants (class III) White dwarfs – near left corner (small size, high temperature)

26. Star Clusters Open clusters and globular clusters. Open clusters contain a few thousands stars and span ~30 light-years (10 pc). Pleiades Globular clusters can contain more than a million stars and span 60-150 light-years. Stars in clusters are at the same distance from the Sun and are formed at about the same time. It is easy to determine clusters’ ages.

27. Star Clusters Age of cluster = lifetime of stars at main-sequence turnoff point. Most open clusters are relatively young (<5 billion years). Globular clusters are typically old objects (12-16 billion years), the oldest objects in the galaxy. They place a limit on the possible age of the Universe.

28. Summary The differences between stars are due to their initial mass and current age. The HR diagram is one of the most powerful tools of astronomers. Stars spend most of their lives at the main sequence. The most massive stars live a few million years, while the least massive stars live more than the current Universe age.