p-modes and temperature waves in photosphere

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P-modes and P-modes and temperature waves temperature waves in photosphere in photosphere Yuzef D. Zhugzhda Yuzef D. Zhugzhda Puskov Institute of Puskov Institute of Terrestrial Magnetism, Terrestrial Magnetism, Ionosphere and Radiowave Ionosphere and Radiowave Propagation of Russian Propagation of Russian Academy of Sciences Academy of Sciences

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P-modes and temperature waves in photosphere. Yuzef D. Zhugzhda Puskov Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation of Russian Academy of Sciences. Darkening and visibility functions of p-modes Local approximation Inverse problem - PowerPoint PPT Presentation

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Page 1: P-modes and temperature waves in photosphere

P-modes and P-modes and temperature waves temperature waves

in photospherein photosphereYuzef D. ZhugzhdaYuzef D. Zhugzhda

Puskov Institute of Terrestrial Puskov Institute of Terrestrial Magnetism, Ionosphere and Magnetism, Ionosphere and Radiowave Propagation of Radiowave Propagation of

Russian Academy of SciencesRussian Academy of Sciences

Page 2: P-modes and temperature waves in photosphere

•Darkening and visibility functions of p-modes

•Local approximation

•Inverse problem

•True visibility and darkening function

•Explorations of Stodilka and Hidalgo et al

•Temperature waves in stratified atmosphere

•Brightness fluctuations of the Sun and stars and temperature waves

Page 3: P-modes and temperature waves in photosphere
Page 4: P-modes and temperature waves in photosphere

Expansion of intensity

P-modes produce small disturbances of the solar photosphere that makes possible to use expansion of intensity only up to the first order.

Opacity disturbances due to temperature and density

fluctuations

Adiabatic approximation

polar angle

darkening function

Page 5: P-modes and temperature waves in photosphere

Local approximation makes possible to take out of the integral temperature disturbance

After integration over the whole disk of the star we arrive to relative visibility function normalized on relative temperature disturbances

The advantage of the local approximation is that relative visibility function depends only on parameters

of undisturbed atmosphere

Page 6: P-modes and temperature waves in photosphere

Derivative of opacity with respect to temperature

Derivative of opacity with respect to density

Solid line – absolute visibility, long-dashed line –Plank function contribution, medium-dashed and short-dashed lines – contributions of opacity fluctuations due to temperature and density fluctuation

Page 7: P-modes and temperature waves in photosphere

Inverse problem

Multi-channel photometer DIFOS

Circles –DIFOS, squares –SPM(SOHO)

Page 8: P-modes and temperature waves in photosphere
Page 9: P-modes and temperature waves in photosphere

Darkening functions

Page 10: P-modes and temperature waves in photosphere

Temperature waves

Quasi-adiabatic approximation

Quasi-isothermal approximation

|||| aT kk

|||| aT kk

Page 11: P-modes and temperature waves in photosphere
Page 12: P-modes and temperature waves in photosphere

Coupling of p-modes and temperature waves

Optically thick

atmosphere

Optically thin

atmosphere

Isothermal atmosphere H-pressure

scale

It was found out analytical exact solution of the problem in terms of Generalized

Hypergeometrical functions

Wave coupling

P-

mod

es

Temperature waves

Page 13: P-modes and temperature waves in photosphere