The velocity pattern of weak solar magnetic fields
Abstract
We have measured the proper motion of magnetic elements on the quiet Sun by means of local correlation tracking. The existence of a pattern in the intranetwork (IN) flow is confirmed. This velocity field is consistent with the direct Doppler measurement of the horizontal component of the supergranular velocity field. The IN elements generally move toward the network boundaries. By tracking test points we confirm that the magnetic elements converge in areas corresponding to the magnetic network. But because the IN elements are of random polarity, they cannot contribute to the growth or maintenance of the magnetic network. By calculating the cross correlation between the magnetogram and Dopplergram, we confirm that the supergranule boundaries and the magnetic network are roughly correlated.
Additional Information
© 1988 Kluwer Academic Publishers. Provided by the NASA Astrophysics Data System. Received 23 October 1987. We are indebted to Dr S. F. Martin for many helpful comments, discussion and suggestions. We wish to thank the Big Bear staff for the support in observation, Dr B. Popp for his computer programs and J. Nenow for processing films. Also we are grateful for the assistance from Kitt Peak Observatory, especially Drs J. Harvey and K. Harvey for their valuable suggestions and F. Recely for his help in observation. This work is supported by NSF under grant ATM-8513577 and NASA under grant NGL 05 002 034.Attached Files
Published - 1988SoPh__115__205W.pdf
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Additional details
- Eprint ID
- 103630
- Resolver ID
- CaltechAUTHORS:20200602-075231064
- NSF
- ATM-8513577
- NASA
- NGL 05 002 034
- Created
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2020-06-02Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field