Evolution of sunspot properties during solar cycle 23

Watson, F., Fletcher, L. and Marshall, S. (2011) Evolution of sunspot properties during solar cycle 23. Astronomy and Astrophysics, 533, A14. (doi:10.1051/0004-6361/201116655)

Watson, F., Fletcher, L. and Marshall, S. (2011) Evolution of sunspot properties during solar cycle 23. Astronomy and Astrophysics, 533, A14. (doi:10.1051/0004-6361/201116655)

[img] Text
watsonetal11_arxiv.pdf
Restricted to Repository staff only

1MB

Publisher's URL: http://dx.doi.org/10.1051/0004-6361/201116655

Abstract

<b>Context.</b> The long term study of the Sun is necessary if we are to determine the evolution of sunspot properties and thereby inform modeling of the solar dynamo, particularly on scales of a solar cycle. <b>Aims.</b> We aim to determine a number of sunspot properties over cycle 23 using the uniform database provided by the SOHO Michelson Doppler Imager data. We focus in particular on their distribution on the solar disk, maximum magnetic field and umbral/penumbral areas. We investigate whether the secular decrease in sunspot maximum magnetic field reported in Kitt Peak data is present also in MDI data. <b>Methods</b>. We have used the Sunspot Tracking And Recognition Algorithm (STARA) to detect all sunspots present in the SOHO Michelson Doppler Imager continuum data giving us 30 084 separate detections. We record information on the sunspot locations, area and magnetic field properties as well as corresponding information for the umbral areas detected within the sunspots, and track them through their evolution. <b>Results</b>. We find that the total visible umbral area is 20−40% of the total visible sunspot area regardless of the stage of the solar cycle. We also find that the number of sunspots observed follows the Solar Influences Data Centre international sunspot number with some interesting deviations. Finally, we use the magnetic information in our catalogue to study the long term variation of magnetic field strength within sunspot umbrae and find that it increases and decreases along with the sunspot number. However, if we were to assume a secular decrease as was reported in the Kitt Peak data and take into account sunspots throughout the whole solar cycle we would find the maximum umbral magnetic fields to be decreasing by 23.6 ± 3.9 Gauss per year, which is far less than has previously been observed by other studies (although measurements are only available for solar cycle 23). If we only look at the declining phase of cycle 23 we find the decrease in sunspot magnetic fields to be 70 Gauss per year.

Item Type:Articles
Keywords:Sun: activity, Sun: evolution, Sun: photosphere, sunspots
Status:Published
Refereed:Yes
Glasgow Author(s) Enlighten ID:Watson, Mr Fraser and Fletcher, Professor Lyndsay
Authors: Watson, F., Fletcher, L., and Marshall, S.
College/School:College of Science and Engineering > School of Physics and Astronomy
Research Group:Astronomy and Astrophysics
Journal Name:Astronomy and Astrophysics
Publisher:EDP Sciences
ISSN:0004-6361
Published Online:18 August 2011

University Staff: Request a correction | Enlighten Editors: Update this record