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Introduction to Astrophysics Ronald L. Westra Department Mathematics Maastricht University.

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Presentation on theme: "Introduction to Astrophysics Ronald L. Westra Department Mathematics Maastricht University."— Presentation transcript:

1 Introduction to Astrophysics Ronald L. Westra Department Mathematics Maastricht University

2 Introduction to Astrophysics

3 1. Astronomic Scales in Space and Time

4 Earth Sun Jupiter.

5 Galaxy M31, known as the Andromeda nebula

6 Collection of galaxies. The three fuzzy galaxies left merging, The crisp galaxy in the center is on the background

7 Large-scale map of the observable universe showing the the largest structures visible in the universe. Each point in this diagram represents one single galaxy


9 The Universe at the young age of 300,000 years. The colors represent temperature fluctuations in the Cosmic Background Radiation Wilkinson Microwave Anisotropy Probe

10 Subtle variations in the CBR.

11 The Giant Impact Theory suggests that a Mars-sized object crashed into the early Earth. Most of the debris thrown into space fell back on Earth, but a fraction aggregated into the Moon. This theory is supported by the similar composition of rocks on the Earth and Moon.

12 2. Stellar Evolution

13 Some characteristics of the sun radius (R  )7 10 10 cm mass (M  )2 10 33 g mean density (   )1.4 g/cm 3 total energy output (L  )3.82.10 26 Joule/sec age1.5 10 17 sec core temperature5 10 6 K surface temperature5 10 3 K distance to earth1.5 10 13 cm

14 Nuclear fusion in centre of sun

15 O – B – A – F – G – K – M – R – N – S Spectral Types

16 Absolute and Relative Luminosity

17 Original Hertzsprung-Russell Diagram ( HRD)

18 Binding energy per nucleon as function of mass number A.

19 Glowing gaseous streamers of an extinct titanic supernova explosion of a massive star in Cassiopeia A (Cas A)

20 Composite image of the Crab Nebula showing superimposed images of X-ray (blue) (by Chandra X-ray space telescope), and optical (red) (by the Hubble space telescope).

21 First published registration of a pulsar, Hewish et al., Nature 217, p. 710, 1968.

22 Path of the stellar evolution of a main sequence star of one solar mass in the Hertzsprung-Russell diagram log T eff in K log L/ L 

23 sun L/ L  surface temperature (K) The HRD for 10 stellar clusters. At right ordinate the age in billion years of the bifurcation point from the main sequence.

24 Abundances of chemical elements in the neighbourhood of our sun. The marks are from the intensities from spectral absorption lines in the sun’s atmosphere, the lines from meteorite and terrestrial data.

25 An example of an unstable – but not- periodic – star is this massive ‘Wolf- Rayet star’ NGC2359, that irregularly ejects large parts of its own outer envelope in gargantuan explosions. The star itself is in the central bubble, the clouds are remnants of previous ejections.

26 main sequence RR Lyrae Cepheids instability strip surface temperature Luminosity Variable stars in the HRD. Pulsating variable stars are found in the instability strip connecting the main sequence and the red- giant region. long period variables

27 Relation between luminosity and oscillation period for Cepheid type 1 variable stars.

28 Ronald L. Westra Systems Theory Group Department Mathematics Maastricht University

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