THE VELOCITY DISTRIBUTION OF SOLAR PHOTOSPHERIC MAGNETIC BRIGHT POINTS

被引：51

作者：

Keys, P. H. ^{[1
]}

Mathioudakis, M. ^{[1
]}

Jess, D. B. ^{[1
]}

Shelyag, S. ^{[1
]}

Crockett, P. J. ^{[1
]}

Christian, D. J. ^{[2
]}

Keenan, F. P. ^{[1
]}

机构：

[1] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[2] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 740卷 / 02期

基金：

英国科学技术设施理事会; 美国国家科学基金会;

关键词：

Sun: activity; Sun: evolution; Sun: photosphere; G-BAND BRIGHT; FIELDS; MAGNETOCONVECTION; DYNAMICS; ELEMENTS; WAVES; FLOWS; CODE; SUN;

D O I：

10.1088/2041-8205/740/2/L40

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use high spatial resolution observations and numerical simulations to study the velocity distribution of solar photospheric magnetic bright points. The observations were obtained with the Rapid Oscillations in the Solar Atmosphere instrument at the Dunn Solar Telescope, while the numerical simulations were undertaken with the MURaM code for average magnetic fields of 200 G and 400 G. We implemented an automated bright point detection and tracking algorithm on the data set and studied the subsequent velocity characteristics of over 6000 structures, finding an average velocity of approximately 1 km s(-1), with maximum values of 7 km s(-1). Furthermore, merging magnetic bright points were found to have considerably higher velocities, and significantly longer lifetimes, than isolated structures. By implementing a new and novel technique, we were able to estimate the background magnetic flux of our observational data, which is consistent with a field strength of 400 G.

引用

页数：5

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