|
|
Articles
Solar wind streams originate from low-density, magnetically open
regions of the sun's corona, known as coronal holes. The locations,
areal sizes, rotation, and solar-cycle evolution of these regions can
be reproduced and understood by applying simple extrapolation models to
measurements of the photospheric magnetic field. The surprisingly rigid
rotation displayed by many coronal holes suggests that field-line
reconnection occurs continually in the corona, despite the high
electrical conductivity of the coronal plasma. The magnetic field
strengths and field-line divergence rates in coronal holes can be
related empirically to the bulk speed and the mass and energy flux
densities of the solar wind plasma. Such relations may help to
illuminate the physical processes responsible for heating the corona
and driving the solar wind.
THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
|
Science. ISSN 0036-8075 (print), 1095-9203 (online)
Magazine | News | Signaling | Careers | Multimedia | Collections | Help | Site Map | RSS
Subscribe | Feedback | Privacy / Legal | About Us | Advertise With Us | Contact Us
© 1996 American Association for the Advancement of Science. All Rights Reserved.
AAAS is a partner of HINARI, AGORA, PatientInform, CrossRef, and COUNTER.
You have reached the bottom of the page. Back to top