Radiative Transfer in Axial Symmetry

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$EinfÃ¼hrung in LATEX PD Dr. Thorsten Nagel - UniversitÃ¤t TÃ¼bingen$

$LaTeX Vorlesung - Typographie mit LaTeX -- Schriftarten und ...$

Where it can play the role? – edge-on view – opening angle ∼ 10 ◦ – not so small probability – self-shielding disc (e.g. V348 Pup) – occulting systems – some UX UMa or SW Ser systems – low luminosity – dust is not important in most CVs (in contrast to polars) – extended area – wind – important corona – polars, intermediate polars
conclusion – axial symmetry + wind + rotation =⇒ – rapidly rotating stars – extended stellar atmospheres – stellar winds – discs
Page 1 and 2: Radiative Transfer in Axial Symmetr
Page 3 and 4: description of the method method pr
Page 5 and 6: longitudinal planes whole radiation
Page 7 and 8: integration I (B) = I (A) e −∆
Page 9 and 10: solution in the central region C
Page 11 and 12: mean intensity rotation axis - the
Page 13 and 14: parallelization - MPI - memory × c
Page 15 and 16: method applicability - limb darkeni
Page 18 and 19: stellar rotation - rapidly rotating
Page 20 and 21: stellar wind - optically thick atmo
Page 22 and 23: discs - protostellar discs - catacl
Page 24 and 25: choice of the systems - the quiesce
Page 26 and 27: SS Cyg - quiescent phase - Hα y [R
Page 28 and 29: SS Cyg - quiescent phase - Hγ y [R
Page 30 and 31: an AM CVn star - P orb < 1 hour =
Page 32 and 33: an AM CVn star - HeI 4923Å relativ

Radiative Transfer in Axial Symmetry

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