The size distribution of magnetic bright points derived from Hinode/SOT observations
Context. Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scal...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2009-04, Vol.498 (1), p.289-293 |
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| container_title | Astronomy and astrophysics (Berlin) |
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| creator | Utz, D. Hanslmeier, A. Möstl, C. Muller, R. Veronig, A. Muthsam, H. |
| description | Context. Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scale-magnetic-field energy. Aims. The size distribution of MBPs is derived for G-band images acquired by the Hinode/SOT instrument. Methods. For identification purposes, a new automated segmentation and identification algorithm was developed. Results. For a sampling of 0.108 arcsec/pixel, we derived a mean diameter of $(218 \pm 48)$ km for the MBPs. For the full resolved data set with a sampling of 0.054 arcsec/pixel, the size distribution shifted to a mean diameter of $(166 \pm 31)$ km. The determined diameters are consistent with earlier published values. The shift is most probably due to the different spatial sampling. Conclusions. We conclude that the smallest magnetic elements in the solar photosphere cannot yet be resolved by G-band observations. The influence of discretisation effects (sampling) has also not yet been investigated sufficiently. |
| doi_str_mv | 10.1051/0004-6361/200810867 |
| format | Article |
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Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scale-magnetic-field energy. Aims. The size distribution of MBPs is derived for G-band images acquired by the Hinode/SOT instrument. Methods. For identification purposes, a new automated segmentation and identification algorithm was developed. Results. For a sampling of 0.108 arcsec/pixel, we derived a mean diameter of $(218 \pm 48)$ km for the MBPs. For the full resolved data set with a sampling of 0.054 arcsec/pixel, the size distribution shifted to a mean diameter of $(166 \pm 31)$ km. The determined diameters are consistent with earlier published values. The shift is most probably due to the different spatial sampling. Conclusions. We conclude that the smallest magnetic elements in the solar photosphere cannot yet be resolved by G-band observations. The influence of discretisation effects (sampling) has also not yet been investigated sufficiently.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/200810867</identifier><identifier>CODEN: AAEJAF</identifier><language>eng</language><publisher>Les Ulis: EDP Sciences</publisher><subject>Astronomy ; Astrophysics ; Earth, ocean, space ; Exact sciences and technology ; High Energy Astrophysical Phenomena ; magnetic fields ; Sciences of the Universe ; Sun: photosphere ; techniques: image processing</subject><ispartof>Astronomy and astrophysics (Berlin), 2009-04, Vol.498 (1), p.289-293</ispartof><rights>2009 INIST-CNRS</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c396t-ef0c82fdec2be6fb42345555dca3292c5ac424109cdab8aec1ec221eeaa31a5f3</citedby><cites>FETCH-LOGICAL-c396t-ef0c82fdec2be6fb42345555dca3292c5ac424109cdab8aec1ec221eeaa31a5f3</cites><orcidid>0000-0003-2073-002X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,3714,27901,27902</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=21410140$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://hal.science/hal-00392206$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Utz, D.</creatorcontrib><creatorcontrib>Hanslmeier, A.</creatorcontrib><creatorcontrib>Möstl, C.</creatorcontrib><creatorcontrib>Muller, R.</creatorcontrib><creatorcontrib>Veronig, A.</creatorcontrib><creatorcontrib>Muthsam, H.</creatorcontrib><title>The size distribution of magnetic bright points derived from Hinode/SOT observations</title><title>Astronomy and astrophysics (Berlin)</title><description>Context. Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scale-magnetic-field energy. Aims. The size distribution of MBPs is derived for G-band images acquired by the Hinode/SOT instrument. Methods. For identification purposes, a new automated segmentation and identification algorithm was developed. Results. For a sampling of 0.108 arcsec/pixel, we derived a mean diameter of $(218 \pm 48)$ km for the MBPs. For the full resolved data set with a sampling of 0.054 arcsec/pixel, the size distribution shifted to a mean diameter of $(166 \pm 31)$ km. The determined diameters are consistent with earlier published values. The shift is most probably due to the different spatial sampling. Conclusions. We conclude that the smallest magnetic elements in the solar photosphere cannot yet be resolved by G-band observations. The influence of discretisation effects (sampling) has also not yet been investigated sufficiently.</description><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>High Energy Astrophysical Phenomena</subject><subject>magnetic fields</subject><subject>Sciences of the Universe</subject><subject>Sun: photosphere</subject><subject>techniques: image processing</subject><issn>0004-6361</issn><issn>1432-0746</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2009</creationdate><recordtype>article</recordtype><recordid>eNo9kEFPwyAYQInRxDn9BV64ePBQ9wFt1x6n0U1dssOqJl7IVwoburUL1EX99dLMlAsB3vtCHiGXDG4YJGwEAHGUipSNOEDGIEvHR2TAYsEjGMfpMRn0xCk58_4jHDnLxIAUxVpTb381raxvnS2_WtvUtDF0i6tat1bR0tnVuqW7xtatp5V2dq8ralyzpTNbN5UeLRcFbUqv3R4725-TE4Mbry_-9yF5ebgv7mbRfDF9vJvMIyXytI20AZVxU2nFS52aMuYiTsKqFAqec5WginnMIFcVlhlqxQLJmdaIgmFixJBcH-aucSN3zm7R_cgGrZxN5rK7AxA555DuWWDFgVWu8d5p0wsMZBdRdolkl0j2EYN1dbB26BVujMNaWd-rnIXvsRgCFx24EFF_9-_oPmWYMk5kBm9yfjtdvj89F_JV_AHaq4F8</recordid><startdate>20090401</startdate><enddate>20090401</enddate><creator>Utz, D.</creator><creator>Hanslmeier, A.</creator><creator>Möstl, C.</creator><creator>Muller, R.</creator><creator>Veronig, A.</creator><creator>Muthsam, H.</creator><general>EDP Sciences</general><scope>BSCLL</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><orcidid>https://orcid.org/0000-0003-2073-002X</orcidid></search><sort><creationdate>20090401</creationdate><title>The size distribution of magnetic bright points derived from Hinode/SOT observations</title><author>Utz, D. ; Hanslmeier, A. ; Möstl, C. ; Muller, R. ; Veronig, A. ; Muthsam, H.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c396t-ef0c82fdec2be6fb42345555dca3292c5ac424109cdab8aec1ec221eeaa31a5f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2009</creationdate><topic>Astronomy</topic><topic>Astrophysics</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>High Energy Astrophysical Phenomena</topic><topic>magnetic fields</topic><topic>Sciences of the Universe</topic><topic>Sun: photosphere</topic><topic>techniques: image processing</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Utz, D.</creatorcontrib><creatorcontrib>Hanslmeier, A.</creatorcontrib><creatorcontrib>Möstl, C.</creatorcontrib><creatorcontrib>Muller, R.</creatorcontrib><creatorcontrib>Veronig, A.</creatorcontrib><creatorcontrib>Muthsam, H.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Utz, D.</au><au>Hanslmeier, A.</au><au>Möstl, C.</au><au>Muller, R.</au><au>Veronig, A.</au><au>Muthsam, H.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The size distribution of magnetic bright points derived from Hinode/SOT observations</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2009-04-01</date><risdate>2009</risdate><volume>498</volume><issue>1</issue><spage>289</spage><epage>293</epage><pages>289-293</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><eissn>1432-0756</eissn><coden>AAEJAF</coden><abstract>Context. Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scale-magnetic-field energy. Aims. The size distribution of MBPs is derived for G-band images acquired by the Hinode/SOT instrument. Methods. For identification purposes, a new automated segmentation and identification algorithm was developed. Results. For a sampling of 0.108 arcsec/pixel, we derived a mean diameter of $(218 \pm 48)$ km for the MBPs. For the full resolved data set with a sampling of 0.054 arcsec/pixel, the size distribution shifted to a mean diameter of $(166 \pm 31)$ km. The determined diameters are consistent with earlier published values. The shift is most probably due to the different spatial sampling. Conclusions. We conclude that the smallest magnetic elements in the solar photosphere cannot yet be resolved by G-band observations. The influence of discretisation effects (sampling) has also not yet been investigated sufficiently.</abstract><cop>Les Ulis</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/200810867</doi><tpages>5</tpages><orcidid>https://orcid.org/0000-0003-2073-002X</orcidid><oa>free_for_read</oa></addata></record> |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; EZB-FREE-00999 freely available EZB journals |
| subjects | Astronomy Astrophysics Earth, ocean, space Exact sciences and technology High Energy Astrophysical Phenomena magnetic fields Sciences of the Universe Sun: photosphere techniques: image processing |
| title | The size distribution of magnetic bright points derived from Hinode/SOT observations |
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