Thermal X-ray radiation (PDF) - SRON

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Figure 3.1: The predicted X-<strong>ray</strong> spectrum of Capella. The picture illustrates the remarkable increase in sensitivity and resolution afforded by the Reflection Grating Spectrometer (RGS) of XMM-Newton by comparing the predicted RGS spectrum of the star Capella with that obtained with the EXOSAT gratings (inset). The throughput is three orders of magnitude, and the spectral resolution more than a factor of 20, better than achieved with EXOSAT. ( c○ G. Branduardi-Raymont, www.mssl.ucl.ac.uk/www astro/rgs/rgs impact.html) 3
Figure 3.2: The observed X-<strong>ray</strong> spectrum of Capella. The spectrum is taken with the Reflection Grating Spectrometer (RGS) of XMM-Newton. The plot shows the wealth of emission lines in this source. From Audard et al., A&A, 365, L329 (2001). 4
Page 1 and 2: High Energy Astrophysics Jelle Kaas
Page 3: 3.1 Introduction Thermal X-ray radi
Page 7 and 8: Figure 3.6: X-ray spectrum of the S
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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