Thermal X-ray radiation (PDF) - SRON

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Figure 3.3: The observed X-ray spectrum with the RGS of XMM-Newton of the flare star EQ Pegasi. The plot shows the so-called Ovii triplet, consisting of the resonance, intercombination and forbidden line. The relative line ratio’s of this triplet contain a wealth of physical information. Image courtesy of J. Schmitt, Hamburger Sternwarte, Germany and ESA. Figure 3.4: X-ray spectrum of the Seyfert 2 galaxy NGC 1068. From Kinkhabwala et al., ApJ, 575, 732 (2002). Figure 3.5: X-ray spectrum of the Seyfert 1 galaxy IRAS 13349+2438, obtained with the RGS of XMM-Newton. From: Sako et al., A&A 365, L168. 5
Figure 3.6: X-ray spectrum of the Seyfert 1 galaxy MCG 6-30-15, obtained with the RGS of XMM-Newton. 6
Page 1 and 2: High Energy Astrophysics Jelle Kaas
Page 3 and 4: 3.1 Introduction Thermal X-ray radi
Page 5: Figure 3.2: The observed X-ray spec
Page 9 and 10: series of alkaline spectra). The no
Page 11 and 12: • The first atomic shell (n = 1)
Page 13 and 14: Z El 1s 2s 2p 3s 3p 3d 4s Ground te
Page 15 and 16: m l1 s 1 m l2 s 2 M L M S +1 + +1
Page 17 and 18: 3.3 Energy levels We have seen the
Page 19 and 20: 3.4 Transitions between different l
Page 21 and 22: Figure 3.10: Transitions between a
Page 23 and 24: 3.5 Abundances of the elements With
Page 25 and 26: 3.6 Basic processes In order to be
Page 27 and 28: leading to Here the constant S 0 is
Page 29: 3.6.3 Radiative transition probabil
Page 32 and 33: Figure 3.12: Fluorescence yield as
Page 34 and 35: The formula of Younger While the Lo
Page 36 and 37: 3.6.6 Excitation-Autoionisation In
Page 38 and 39: 3.6.7 Photoionisation Figure 3.20:
Page 40 and 41: 3.6.9 Radiative recombination Radia
Page 42 and 43: 3.6.10 Dielectronic recombination T
Page 44 and 45: 3.7 The ionisation balance In order
Page 46 and 47: of computing time. Therefore one us
Page 48 and 49: 3.8 Continuum emission processes Af
Page 50 and 51: decays back to the 1s orbit by a ra
Page 52 and 53: Inner-shell ionisation The third li
Page 54 and 55: 3.9.3 Line width For most X-ray spe
Page 56 and 57:
Table 3.6: The strongest emission l
Page 58 and 59:
Table 3.8: Some important iron line
Page 60 and 61:
with τ(λ) = τ 0 ϕ(λ) (3.83) wh
Page 62 and 63:
Table 3.9: The most important X-ray
Page 64 and 65:
where the hydrogen column density N
Page 66 and 67:
source itself. Fortunately, with hi
Page 68 and 69:
Figure 3.35: Stability for the ioni
Page 70:
Table 3.10: Wavelengths in Å of th
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