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dc.contributor.authorKane, R P-
dc.identifier.issn0975-105X (Online); 0367-8393 (Print)-
dc.description.abstractFor daily values in a strong 27-day sequence, lasting for more than 8 months, correlations of solar EUV with solar F10 radio emission were, sometimes, found to be lower than those with solar Mg II core-to-wing index, sometimes higher, and sometimes almost the same. Correlations of EUV with the UV Si III and Lyman-α were found to be mostly higher than those with F10 and Mg II. In contrast to the correlations for long-term changes (0.95 or more), the maximum correlations for short-term changes (daily values) were only -0.80, implying an explained variance of only -65%, leaving -35% unexplained. Hence, estimates of daily EUV using F10 and Mg II as proxies could have uncertainties of several tens of percent. For intermediate and long-term changes, EUV was very highly correlated with F10. Mg II and Lyman-α (and to some extent even with sunspots) during years of low and medium sunspot activity (1996-1999) of cycle 23. The Mg II had a slight superiority over F10, but both could be considered as good proxies for EUV. However, for the sunspot maximum years 2000-2002, the EUV evolution differed from the evolutions of F10 and Mg II, so that these would be unsatisfactotry proxies for EUV.en_US
dc.publisherNISCAIR-CSIR, Indiaen_US
dc.relation.ispartof96.60.Qc; 96.60.Tf; 94.20.Vven_US
dc.rights CC Attribution-Noncommercial-No Derivative Works 2.5 Indiaen_US
dc.sourceIJRSP Vol.33(4) [August 2004]en_US
dc.subjectSolar EUVen_US
dc.subjectSolar cycleen_US
dc.subjectSolar radio emissionen_US
dc.titleProxies for solar EUV in cycle 23en_US
Appears in Collections:IJRSP Vol.33(4) [August 2004]

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