NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Rotational history of the sun: Spin-down of the interior by circulation currents and fluid instabilitiesA number of astronomical observations show that solar-type stars begin the main-sequence stage with surface rotation rates which are much greater than that of the sun. The subsequent decrease in the surface rotation rate is due to the braking torque exerted by magnetically-coupled mass loss (the solar wind). The direct braking action of the solar wind should be confined to the convective envelope so the rotation of the radiative interior remains an open question. After reviewing the relevant astronomical data, we describe how angular momentum could be transported out of the radiative interior by fluid instabilities and estimate the time scales for such transport. This picture is used to construct an evolutionary model of the sun, which predicts the present rotation of the radiative interior. The results of such a model are interpreted in terms of the measured oblateness of the solar surface.
Document ID
19810064420
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Endal, A. S.
(Louisiana State University Baton Rouge, LA, United States)
Sofia, S.
(NASA Goddard Space Flight Center Laboratory for Planetary Atmospheres, Greenbelt, MD, United States)
Date Acquired
August 11, 2013
Publication Date
January 1, 1980
Subject Category
Solar Physics
Meeting Information
Meeting: Conference on The ancient sun: Fossil record in the earth, moon and meteorites
Location: Boulder, CO
Start Date: October 16, 1979
End Date: October 19, 1979
Accession Number
81A48824
Funding Number(s)
CONTRACT_GRANT: NSF AST-78-23325
CONTRACT_GRANT: NSF AST-79-08489
Distribution Limits
Public
Copyright
Other

Available Downloads

There are no available downloads for this record.
No Preview Available