Charge States, Helium Abundance, and FIP Bias of the Interplanetary CMEs Classified by Flares and Hot Channels

Zhai, Huitong; Fu, Hui; Huang, Zhaoqin; Xia, Li

doi:10.3847/1538-4357/ac56e4

Cited by 3 publications

(41 citation statements)

References 62 publications

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“…The left (right) peak is less (higher) than 12. The minimum between the two peaks is about 12 (see Figure 1 in Zhai et al 2022). The results indicate that the Q Fe should be lower than 12 for the ICMEs not associated with flares on the Sun.…”

Section: Introductionmentioning

confidence: 82%

“…In addition, a positive correlation is also present between the helium abundance and flare intensities (Zhai et al 2022). Based on the observations of AIA/SDO and SECCHI on STEREO, Zhai et al (2022) traced 29 CMEs from the Sun all the way to the Earth. Hence, the connection between ICMEs detected in situ and activities on the Sun is established independent of any model and hypothesis.…”

Section: Introductionmentioning

confidence: 96%

“…The properties of the plasma inside ICMEs are also closely connected to the flaring process. Generally, the CMEs accompanied by flares are associated with higher charge states (Lepri & Zurbuchen 2004;Reinard 2008;Gopalswamy et al 2013) and higher helium abundance (Borrini et al 1982;Fu et al 2020;Zhai et al 2022). The average charge state of iron (Q Fe ) is positively correlated with flare intensities (Gopalswamy et al 2013;Zhai et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…Generally, the CMEs accompanied by flares are associated with higher charge states (Lepri & Zurbuchen 2004;Reinard 2008;Gopalswamy et al 2013) and higher helium abundance (Borrini et al 1982;Fu et al 2020;Zhai et al 2022). The average charge state of iron (Q Fe ) is positively correlated with flare intensities (Gopalswamy et al 2013;Zhai et al 2022). In addition, a positive correlation is also present between the helium abundance and flare intensities (Zhai et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…The average charge state of iron (Q Fe ) is positively correlated with flare intensities (Gopalswamy et al 2013;Zhai et al 2022). In addition, a positive correlation is also present between the helium abundance and flare intensities (Zhai et al 2022). Based on the observations of AIA/SDO and SECCHI on STEREO, Zhai et al (2022) traced 29 CMEs from the Sun all the way to the Earth.…”

Section: Introductionmentioning

confidence: 99%

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The Solar Cycle Dependence of In Situ Properties of Two Types of Interplanetary CMEs during 1999–2020

Shi

Huang

et al. 2022

ApJ

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Generally, in situ parameters of interplanetary coronal mass ejections (ICMEs) are analyzed as a whole, or ICMEs are classified by speed or whether they are with and without magnetic clouds. Zhai and colleagues found that ICMEs with and without flares can be extracted only by the average charge states of iron (Q Fe). In the present study, the ICMEs are categorized into two types, flare CMEs (FCs) and nonflare CMEs (NFCs) by the Q Fe. We find that the occurrence rates of FCs and NFCs are both decreased from solar maximum to minimum. The occurrence rates and proportions of FCs are both higher in solar cycle 23 than in solar cycle 24. In contrast, the occurrence rates of NFCs are almost the same during the two solar cycles. The durations of FCs are longer than those of NFCs. The fractions of FCs and NFCs that are associated with magnetic clouds (MCs) or magnetic field direction rotation evidence are 73% and 69%, respectively. The speed, Q Fe, O7+/O6+, helium abundance (A He), and first ionization potential bias are all higher for FCs than for NFCs. The above parameters inside NFCs and solar wind are almost the same. The solar cycle dependence of the parameters inside NFCs is more clear than that inside FCs. The statistical results demonstrate that the material sources of FCs are not completely the same as those of NFCs. Part of the material inside FCs should come from the lower atmosphere where the A He is higher. The statistical results indicate that all CMEs are associated with flux ropes on the Sun.

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Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Solar Cycle Dependence of In Situ Properties of Two Types of Interplanetary CMEs during 1999–2020

Shi

Huang

et al. 2022

ApJ

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The Properties of Small Magnetic Flux Ropes inside the Solar Wind Come from Coronal Holes, Active Regions, and Quiet Sun

Zhai

et al. 2023

ApJ

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The origination and generation mechanisms of small magnetic flux ropes (SMFRs), which are important structures in solar wind, are not clearly known. In the present study, 1993 SMFRs immersed in coronal holes, active regions, and quiet-Sun solar wind are analyzed and compared. We find that the properties of SMFRs immersed in three types of solar wind are significantly different. The SMFRs are further classified into hot-SMFRs, cold-SMFRs, and normal-SMFRs, according to whether the O7+/O6+ is 30% elevated or dropped inside SMFRs as compared with background solar wind. Our studies show that the parameters of normal-SMFRs are similar to background in all three types of solar wind. The properties of hot-SMFRs and cold-SMFRs seem to be lying in two extremes. Statistically, the hot-SMFRs (cold-SMFRs) are associated with longer (shorter) duration, lower (higher) speeds and proton temperatures, higher (lower) charge states, helium abundance, and first ionization potential bias as compared with normal-SMFRs and background solar wind. The anticorrelations between speed and O7+/O6+ inside hot-SMFRs (normal-SMFRs) are different from (similar to) those in background solar wind. Most hot-SMFRs and cold-SMFRs should come from the Sun. Hot-SMFRs may come from streamers associated with plasma blobs and/or small-scale activities on the Sun. Cold-SMFRs may be accompanied by small-scale eruptions with lower-temperature materials. Both hot-SMFRs and cold-SMFRs could also be formed by magnetic erosions of interplanetary coronal mass ejections that do not contain or do contain cold-filament materials. The characteristics of normal-SMFRs can be explained reasonably by the two originations, both from the Sun and generated in the heliosphere.

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The Contribution and FIP Bias of Three Types of Materials inside ICMEs Associated with Different Flare Intensities

Fu,

Shi,

Huang

et al. 2023

ApJ

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The relationship between coronal mass ejections (CMEs) and flares is an important issue in solar and stellar physics. The studies on the origination and generation mechanisms of interplanetary CME (ICME) materials are crucial for understanding the connection between CMEs and flares. The materials inside ICMEs can be classified into three types, coming from corona directly (corona materials), heated by magnetic reconnection in corona (heated corona materials), and generated by chromospheric evaporation (chromospheric evaporation materials). Here the contribution and first ionization potential (FIP) bias of three types of materials inside ICMEs associated with different flare intensities are analyzed and compared. We find that the speeds and scales of near-Earth ICMEs both increase with flare intensities. The proportions of heated corona materials are nearly constant with flare intensities. The contributions of corona materials (chromospheric evaporation materials) are significantly decreased (increased) with flare intensities. More than two-thirds of materials are chromospheric evaporation materials for ICMEs associated with strong flares. The FIP bias of corona materials and heated corona materials is almost the same. The FIP bias of chromospheric evaporation materials is significantly higher than that of corona materials and heated corona materials, and it is increased with flare intensities. The above characteristics of FIP bias can be explained reasonably by the origination and generation mechanisms of three types of ICME materials. The present study demonstrates that the origination and generation mechanisms of ICME materials are significantly influenced by flare intensities. The reasons for the elevation of FIP bias, if ICMEs are regarded as a whole, are that the FIP bias of chromospheric evaporation materials is much higher, and the chromospheric evaporation materials contributed significantly to the ICMEs that are associated with strong flares.

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Charge States, Helium Abundance, and FIP Bias of the Interplanetary CMEs Classified by Flares and Hot Channels

Cited by 3 publications

References 62 publications

The Solar Cycle Dependence of In Situ Properties of Two Types of Interplanetary CMEs during 1999–2020

The Solar Cycle Dependence of In Situ Properties of Two Types of Interplanetary CMEs during 1999–2020

The Properties of Small Magnetic Flux Ropes inside the Solar Wind Come from Coronal Holes, Active Regions, and Quiet Sun

The Contribution and FIP Bias of Three Types of Materials inside ICMEs Associated with Different Flare Intensities

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