The existence of long-lived rays of the coronal streamer belt - Radial density and velocity distributions of the solar wind flowing in them

Details The existence of long-lived rays of the coronal streamer belt - Radial density and velocity distributions of the solar wind flowing in them The existence of long-lived rays of the coronal streamer belt - Radial density and velocity distributions of the solar wind flowing in them

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001soph..200..259e&link_type=abstract

Solar Physics, v. 200, Issue 1/2, p. 259-281 (2001).

Physics

10

Scientific paper

A technique is proposed for separating the rays of the streamer belt with quasi-stationary and non-stationary solar wind (SW) flows. It is shown that the lifetime of rays with a quasi-stationary SW can exceed 20 days. A new method has been developed for measuring the relative density distribution of a quasi-stationary slow SW flowing along the streamer belt's ray of increased brightness, based on the LASCO/SOHO data. It is shown that the density n for such SW flows varies with the radius R according to the relationship n~R^-α, where α=α_1~3.3-3.9 within 4 R_0 <=R <= 6 R _0 (here R_0 is the solar radius), and decreases gradually further away. It is also shown that the V(R)-profiles in some rays of the streamer belt differ little from each other, although the value of the mass flow density, j_E, at the Earth's orbit in them can vary more than by a factor of 4. This distinguishes in a crucial respect a slow SW in the streamer belt's rays from a fast SW originating in coronal holes, for which j_E~constant and the dependences V(R) in different fast flows can differ greatly.

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