{"title":"Comparative analysis of the parameters of pulsars with braking indices \\(n>0\\) and \\(n<0\\)","authors":"C. C. Onuchukwu, E. Legahara","doi":"10.1007/s10509-024-04317-3","DOIUrl":null,"url":null,"abstract":"<div><p>We analyzed the timing parameters (the rotational frequency <span>\\(\\nu \\)</span>, the first <span>\\(\\left ( \\dot{\\nu } \\right )\\)</span> and second <span>\\(\\left ( \\ddot{\\nu } \\right )\\)</span> time-derivatives of frequency) and the derived parameters of a sample of pulsars for which <span>\\(\\ddot{\\nu } \\)</span> (470 pulsars) were recorded in the Australian Telescope National Facility (ATNF) pulsar catalog. We formed various subsamples, those with braking indices <span>\\(n<0\\)</span> and <span>\\(n>0\\)</span>, and glitching and non-glitching pulsars. Our statistical analyses of the timing and derived parameters indicated some level of differences and similarities among the parameters analyzed. Glitching pulsars appear to have a higher rotational frequency than non-glitching pulsars, and pulsars with <span>\\(n>0\\)</span> appear to rotate faster than those with <span>\\(n<0\\)</span>. Our results also suggest that glitching pulsars have lower values of <span>\\(\\left \\vert n \\right \\vert \\)</span> (where <span>\\(\\left \\vert n \\right \\vert \\)</span> is the absolute value of the braking index), and it is lower for the subsample with <span>\\(n>0\\)</span> than for the subsample with <span>\\(n<0\\)</span>. We believe that the results obtained could be useful in understanding the evolution of pulsar spin.</p></div>","PeriodicalId":8644,"journal":{"name":"Astrophysics and Space Science","volume":null,"pages":null},"PeriodicalIF":1.8000,"publicationDate":"2024-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astrophysics and Space Science","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s10509-024-04317-3","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0
Abstract
We analyzed the timing parameters (the rotational frequency \(\nu \), the first \(\left ( \dot{\nu } \right )\) and second \(\left ( \ddot{\nu } \right )\) time-derivatives of frequency) and the derived parameters of a sample of pulsars for which \(\ddot{\nu } \) (470 pulsars) were recorded in the Australian Telescope National Facility (ATNF) pulsar catalog. We formed various subsamples, those with braking indices \(n<0\) and \(n>0\), and glitching and non-glitching pulsars. Our statistical analyses of the timing and derived parameters indicated some level of differences and similarities among the parameters analyzed. Glitching pulsars appear to have a higher rotational frequency than non-glitching pulsars, and pulsars with \(n>0\) appear to rotate faster than those with \(n<0\). Our results also suggest that glitching pulsars have lower values of \(\left \vert n \right \vert \) (where \(\left \vert n \right \vert \) is the absolute value of the braking index), and it is lower for the subsample with \(n>0\) than for the subsample with \(n<0\). We believe that the results obtained could be useful in understanding the evolution of pulsar spin.
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