2017
DOI: 10.1007/s11207-017-1170-8
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Quiet-time 0.04 – 2 MeV / nucleon $0.04\,\mbox{--}\,2\mbox{ MeV}/\mbox{nucleon}$ Ions at 1 AU in Solar Cycles 23 and 24

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Cited by 7 publications
(20 citation statements)
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“…They are variously associated with CIRs (Chotoo et al 2000), ISEPs (Hovestadt et al 1984b,a;Desai et al 2006b), and GSEPs (Desai & Mason 2001;Mason et al 1999), depending on the phase of solar activity. In particular, prior observations suggest that CIRs are the dominant source of ST ions during solar minima (Desai et al 2006c;Dayeh et al 2009Dayeh et al , 2017Zel'dovich et al 2011Zel'dovich et al , 2018Zel'dovich et al , 2021 and both ISEP and GSEP events dominate ST sources during solar maxima (Dayeh et al 2017(Dayeh et al , 2009Desai et al 2006c). To quantify the similarity of suprathermal abundances to the known populations in Table 2, we have generated plots of quiet time X/O normalized to them Quiet Time (X/O) : Known (X/O) as a function of M/Q, averaging over each solar cycle extremum and all years from Figure 3.…”
Section: Abundances As a Function Of M/qmentioning
confidence: 98%
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“…They are variously associated with CIRs (Chotoo et al 2000), ISEPs (Hovestadt et al 1984b,a;Desai et al 2006b), and GSEPs (Desai & Mason 2001;Mason et al 1999), depending on the phase of solar activity. In particular, prior observations suggest that CIRs are the dominant source of ST ions during solar minima (Desai et al 2006c;Dayeh et al 2009Dayeh et al , 2017Zel'dovich et al 2011Zel'dovich et al , 2018Zel'dovich et al , 2021 and both ISEP and GSEP events dominate ST sources during solar maxima (Dayeh et al 2017(Dayeh et al , 2009Desai et al 2006c). To quantify the similarity of suprathermal abundances to the known populations in Table 2, we have generated plots of quiet time X/O normalized to them Quiet Time (X/O) : Known (X/O) as a function of M/Q, averaging over each solar cycle extremum and all years from Figure 3.…”
Section: Abundances As a Function Of M/qmentioning
confidence: 98%
“…ST ions are likely associated with CIRs in solar minima (Desai et al 2006c;Dayeh et al 2009Dayeh et al , 2017Zel'dovich et al 2011Zel'dovich et al , 2018Zel'dovich et al , 2021. CIRs are formed when coronating fast solar wind streams from coronal holes overtake slow wind streams.…”
Section: Abundances During Solar Cycle Extrema M/qmentioning
confidence: 99%
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