grb absorption spectroscopy - Inaf

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Average [C/Fe] ratio is 0.08±0.24, consistent with values predicted for a galaxy younger than 1 Gyr undergoing star formation [C/Fe] of component 3 is 0.53±0.23, larger than in 2 (-0.15±0.13), with [C] roughly constant. GRB 050730 Since Fe dust grains are more efficiently destroyed than C dust grains by the GRB UV flux and blast wave (Perna, Lazzati & Fiore 2003), this suggests that component 2 is closer to the GRB than component 3.
FINE STRUCTURE FEATURES The gross structure of an atom is due to the principal quantum number n, giving the main electron shells of atoms. However, electron shells exhibit fine structure, and levels are split due to spin-orbit coupling (the energy difference between the electron spin being parallel or antiparallel to the electron's orbital moment). First fine structure excited level Fine structure splitting
Page 1 and 2: Absorption studies of GRB afterglow
Page 3 and 4: Suitable to: GRB ABSORPTION SPECTRO
Page 5 and 6: LOW - RES GRBs GRBs provide an inde
Page 7: Advantages: Piranomonte et al. 2008
Page 11: GRB 060418: VARIABILITY Fine struct
Page 14 and 15: CrII groud state line is decreasing
Page 18 and 19: OVI Lyβ SII NiII NV NiII Lyα OI/S
Page 20 and 21: MAIN SYSTEM METALLICITY Ly_α Missi
Page 26 and 27: CONCLUSIONS GRBs are a new tool to
Page 28 and 29: GRB explosion site Host gas far awa
Page 32 and 33: GRB 050730 The main system presents
Page 34 and 35: GRB 050730 Fine structure transitio
Page 36: GRB 050730 Second component: UV pum
Page 39 and 40: GRB080319B - MAIN SYSTEM: COMPONENT
Page 41 and 42: GRB080319B - MAIN SYSTEM: COMPONENT
Page 43 and 44: FINE STRUCTURE LINE VARIABILITY Fin
Page 45: GRB080319B - TIME DEPENDENT MODELIN
Page 48 and 49: GRB080330 - MAIN SYSTEM: COMPONENTS
Page 51 and 52: INTERVENING ABSORBERS GRB Strong Mg
Page 53 and 54: FINE STRUCTURE AND EXCITED LINES Id

grb absorption spectroscopy - Inaf

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