DIRECT RADIO PROBING AND INTERPRETATION OF THE SUN’S DENSITY PROFILE

Details DIRECT RADIO PROBING AND INTERPRETATION OF THE SUN’S DENSITY PROFILE DIRECT RADIO PROBING AND INTERPRETATION OF THE SUN’S DENSITY PROFILE

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh44a..04c&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH44A-04

Physics

Plasma Physics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7534] Solar Physics, Astrophysics, And Astronomy / Radio Emissions, [7594] Solar Physics, Astrophysics, And Astronomy / Instruments And Techniques, [7847] Space Plasma Physics / Radiation Processes

Scientific paper

The Sun’s electron number density profile ne(r) is not well measured and understood from the Sun’s photosphere (r = RS) to the solar wind (say, r > 10 RS), despite its great importance for solar physics. A powerful new technique is developed and applied to extract ne(r) directly from the time-varying frequency of coronal type III radio bursts, for the first time. Unexpectedly, wind-like regions with ne = A (r - RS)-2 are common below 2RS, and coronal type III bursts often are almost linear in 1/f - t dynamic spectra. Indices lower and higher than 2 also occur, the former plausibly due to non-radial curved magnetic field lines. The profile ne = A (r - RS)-2 is consistent with the coronal radio data, type III simulations, and previous models based on eclipse and coronagraph observations. It gives a first physical basis for the previous models. A simple interpretation is in terms of conical flow from localized sources close to the photosphere, plausibly corresponding to UV funnels. The results also imply that solar wind acceleration occurs where 2 < r/RS < 10.

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