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Power spectra of solar network and non-network fields

Lee, Jeongwoo and Chae, J.-C. and Yun, H. S. and Zirin, H. (1997) Power spectra of solar network and non-network fields. Solar Physics, 171 (2). pp. 269-282. ISSN 0038-0938. https://resolver.caltech.edu/CaltechAUTHORS:20201021-171001229

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Abstract

We report new properties of solar magnetic fields in a quiet region as found from their magnetic power spectra. The power spectra of network and intranetwork fields (non-network fields) are separately calculated from a Big Bear magnetogram obtained with moderately high spatial resolution of 1.5 arc sec and a high sensitivity reaching 2 Mx cm⁻². The effect of seeing on the power spectrum has been corrected using Fried's (1966) Modulation Transfer Function with the seeing parameter determined in our previous analysis of the magnetogram. As a result, it is found that the two-dimensional power spectra of network and non-network fields appear in a form: Γ(k₀ ≲ k ≲ k₁) ∼ k⁻¹ and Γ(k ≳ k₁) ∼ k^(3.5). Here k₀ ≈ 0.47 Mm⁻¹ for network fields and k₀ ≈ 0.69 Mm⁻¹ for non-network fields, the latter of which corresponds to the size of mesogranulation; k₁ ≈ 3.0 Mm⁻¹ for both, which is about the size of a large granule. The network field spectrum below k₀ appears nearly flat, whereas that of non-network fields instead decreases towards lower wave numbers as Γ(k) ∼ k^(1.3). The turnover behavior of magnetic field spectra around k₁ coincides with that found for the velocity power spectrum, which may justify the kinetic approach taken in previous theoretical studies of the solar magnetic power spectra.


Item Type:Article
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https://doi.org/10.1023/a:1004904406126DOIArticle
https://rdcu.be/b8WkNPublisherFree ReadCube access
Additional Information:© 1997 Kluwer Academic Publishers. Received 13 August, 1996; in final form 8 November, 1996. We thank Dr Jingxiu Wang for suggesting the topic of this paper and the referee for attentive corrections. One of us (JL) has been supported by the 1995 KOSEF Post-Doc. program and HSY by the Basic Science Research Institute Program, Ministry of Education 1996 (BSRI-96–5408). The work at Big Bear Solar Observatory was supported by NASA under Grant NAGW-1972.
Funders:
Funding AgencyGrant Number
Korea Science and Engineering Foundation (KOSEF)UNSPECIFIED
Ministry of Education (Korea)BSRI-96-5408
NASANAGW-1972
Subject Keywords:Power Spectrum, Modulation Transfer Function, Lower Wave, Kinetic Approach, Solar Magnetic Field
Issue or Number:2
Record Number:CaltechAUTHORS:20201021-171001229
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20201021-171001229
Official Citation:Lee, J., Chae, J., Yun, H.S. et al. POWER SPECTRA OF SOLAR NETWORK AND NON-NETWORK FIELDS. Solar Physics 171, 269–282 (1997). https://doi.org/10.1023/A:1004904406126
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:106201
Collection:CaltechAUTHORS
Deposited By: Rebecca Minjarez
Deposited On:23 Oct 2020 15:09
Last Modified:23 Oct 2020 15:09

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