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    • 1 | 2 | 3 | 4 | След.

    1. Relativistic Jet Model
    ... in units of 10 ergs.s the radius of the photosphere is Thus, in order to bury the loss region of the jet along with its associated Bremsstrahlung photons below the electron scattering photosphere, the jet must interact with the wind at a radius of 2.10 cm ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/14_3/dopita/paper/node4.html -- 60.5 Кб -- 08.04.2016
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    2. Current redistribution model for flares
    ... is such that the currents through the photosphere do not have time to change over ... magnetic energy associated with the redistribution of currents above the photosphere ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/15_3/hardy/paper/node2.html -- 57.6 Кб -- 08.04.2016
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    3. Radiation-Pressure Driven Wind Model
    ... is produced by a reprocessing photosphere dominated by electron scattering opacity ... The effective temperature of the photosphere is then determined from Stefan's Law ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/14_3/dopita/paper/node3.html -- 61.8 Кб -- 08.04.2016
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    4. Introduction
    ... The structure suggested by these observations is that of the interaction of at least two current and flux carrying loops, each with a footpoint where current emerges from the photosphere and a footpoint where current reenters the photosphere. ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/15_3/hardy/paper/node1.html -- 53.0 Кб -- 08.04.2016
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    5. Introduction
    ... and the fraction of the stellar photosphere that it covers. ... model of a uniform cloud and photosphere, these parameters are obtained simply by ... The photosphere is limb darkened, so an ionic cloud of a given size blocks ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/17_3/barnes/paper/node1.html -- 60.5 Кб -- 08.04.2016
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    6. http://www.atnf.csiro.au/pasa/17_3/barnes/paper.pdf
    ... ionic cloud, K (= 2H), and the fraction of the stellar photosphere that it covers ... model of a uniform cloud and photosphere, these parameters are obtained simply by ... The photosphere is limb-darkened, so an ionic cloud of a given size blocks ...
    [ Текст ]  Ссылки http://www.atnf.csiro.au/pasa/17_3/barnes/paper.pdf -- 122.1 Кб -- 14.03.2001
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    7. http://www.atnf.csiro.au/pasa/15_3/hardy/paper.pdf
    ... The structure suggested by these observations is that of the interaction of at least two current- and flux-carrying loops, each with a footpoint where current emerges from the photosphere and a footpoint where current re-enters the photosphere. ...
    [ Текст ]  Ссылки http://www.atnf.csiro.au/pasa/15_3/hardy/paper.pdf -- 265.0 Кб -- 06.11.1998
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    8. The Role of Accretion
    ... scattering as well, and a hot electron-scattering photosphere can be produced ... Material below this photosphere serves to reprocess the hard radiation (EUV, X- and ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/14_3/dopita/paper/node2.html -- 71.0 Кб -- 08.04.2016
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    9. http://www.atnf.csiro.au/research/Astro2010/talks/wheatland.pdf
    ... photospheric map of B = (Bx , By , Bz ) Vertical current density Jz may be calculated at photosphere: Jz = 1 µ0 By Bx - x y at z = 0 (2) locally planar approximation to photosphere 3 For more details see e.g. Landi degl'Innocenti & Landolfi (2004 ...
    [ Текст ]  Ссылки http://www.atnf.csiro.au/research/Astro2010/talks/wheatland.pdf -- 1743.5 Кб -- 16.06.2010
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    10. Conclusions
    ... the ``big blue bump'' generated by an optically-thick electron scattering photosphere, and can this reproduce the observations ... What are the details of the jet / thermal wind interaction? Can we bury this interaction below a free-free photosphere? ...
    [ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/pasa/14_3/dopita/paper/node8.html -- 55.2 Кб -- 08.04.2016
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