Issue |
A&A
Volume 529, May 2011
|
|
---|---|---|
Article Number | A148 | |
Number of page(s) | 6 | |
Section | The Sun | |
DOI | https://doi.org/10.1051/0004-6361/201116668 | |
Published online | 22 April 2011 |
Solar winds along curved magnetic field lines
1
Shandong Provincial Key Laboratory of Optical Astronomy &
Solar-Terrestrial Environment, School of Space Science and Physics, Shandong
University at Weihai,
264209
Weihai,
PR China
e-mail: bbl@sdu.edu.cn
2
State Key Laboratory of Space Weather, Chinese Academy of
Sciences, 100190
Beijing, PR
China
Received:
7
February
2011
Accepted:
24
March
2011
Context. Both remote-sensing measurements using the interplanetary scintillation (IPS) technique and in-situ measurements by the Ulysses spacecraft show a bimodal structure for the solar wind at solar minimum conditions. At present it still remains to address why the fast wind is fast and the slow wind is slow. While a robust empirical correlation exists between the coronal expansion rate fc of the flow tubes and the speeds v measured in situ, a more detailed data analysis suggests that v depends on more than just fc.
Aims. We examine whether the non-radial shape of field lines, which naturally accompanies any non-radial expansion, could be an additional geometrical factor.
Methods. We solved the transport equations incorporating the heating from turbulent Alfvén waves for an electron-proton solar wind along curved field lines given by an analytical magnetic field model, which is representative of a solar minimum corona.
Results. The field line shape is found to influence the solar wind parameters substantially, reducing the asymptotic speed by up to ~130 km s-1 or by ~28% in relative terms, compared with the case where the field line curvature is neglected. This effect was interpreted in the general framework of energy addition in the solar wind: compared to the straight case, the field line curvature enhances the effective energy deposition to the subsonic flow, which results in a higher proton flux and a lower terminal proton speed.
Conclusions. Our computations suggest that the field line curvature could be a geometrical factor which, in addition to the tube expansion, substantially influences the solar wind speed. Furthermore, although the field line curvature is unlikely to affect the polar fast solar wind at solar minima, it does help make the wind at low latitudes slow, which in turn helps better reproduce the Ulysses measurements.
Key words: waves / solar wind / stars: winds, outflows
© ESO, 2011
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.