1 Ocak 2018 Dergi makalesi Açık Erişim

Kilcik, A.; Yurchyshyn, V; Sahin, S.; Sarp, V; Obridko, V; Ozguc, A.; Rozelot, J. P.

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{
  "@context": "https://schema.org/", 
  "@id": 28649, 
  "@type": "ScholarlyArticle", 
  "creator": [
    {
      "@type": "Person", 
      "affiliation": "Akdeniz Univ, Fac Sci, Dept Space Sci & Technol, TR-07058 Antalya, Turkey", 
      "name": "Kilcik, A."
    }, 
    {
      "@type": "Person", 
      "name": "Yurchyshyn, V"
    }, 
    {
      "@type": "Person", 
      "affiliation": "Akdeniz Univ, Fac Sci, Dept Space Sci & Technol, TR-07058 Antalya, Turkey", 
      "name": "Sahin, S."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Akdeniz Univ, Fac Sci, Dept Space Sci & Technol, TR-07058 Antalya, Turkey", 
      "name": "Sarp, V"
    }, 
    {
      "@type": "Person", 
      "affiliation": "Russian Acad Sci, IZMIRAN, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Moscow 142190, Russia", 
      "name": "Obridko, V"
    }, 
    {
      "@type": "Person", 
      "name": "Ozguc, A."
    }, 
    {
      "@type": "Person", 
      "name": "Rozelot, J. P."
    }
  ], 
  "datePublished": "2018-01-01", 
  "description": "According to the modified Zurich classification, sunspot groups are classified into seven different classes (A, B, C, D, E, F and H) based on their morphology and evolution. In this classification, classes A and B, which are small groups, describe the beginning of sunspot evolution, while classes D, E and F describe the large and evolved groups. Class C describes the middle phase of sunspot evolution and the class H describes the end of sunspot evolution. Here, we compare the lifetime and temporal evolution of flaring and non-flaring active regions (ARs), and the flaring effect on ARs in these groups in detail for the last two solar cycles (1996 through 2016). Our main findings are as follows: (i) Flaring sunspot groups have longer lifetimes than non-flaring ones. (ii) Most of the class A, B and C flaring ARs rapidly evolve to higher classes, while this is not applicable for non-flaring ARs. More than 50 per cent of the flaring A, B and C groups changed morphologically, while the remaining D, E, F and H groups did not change remarkably after the flare activity. (iii) 75 per cent of all flaring sunspot groups are large and complex. (iv) There is a significant increase in the sunspot group area in classes A, B, C, D and H after flaring activity. In contrast, the sunspot group area of classes E and F decreased. The sunspot counts of classes D, E and F decreased as well, while classes A, B, C and H showed an increase.", 
  "headline": "The evolution of flaring and non-flaring active regions", 
  "identifier": 28649, 
  "image": "https://aperta.ulakbim.gov.tr/static/img/logo/aperta_logo_with_icon.svg", 
  "license": "http://www.opendefinition.org/licenses/cc-by", 
  "name": "The evolution of flaring and non-flaring active regions", 
  "url": "https://aperta.ulakbim.gov.tr/record/28649"
}