Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections

Li, Xiaolei; Wang, Yuming; Guo, Jingnan; Lyu, Shaoyu

doi:10.3847/2041-8213/ac5b72

Cited by 18 publications

(27 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The event we select is the second GOES X-class flare in solar cycle 25, hosted in NOAA active region 12887, occurring around 15:35 UT on 2021 October 28. This event has been reported by other papers, which focused on some observational features, such as observations of EUV waves and the corresponding CME (Devi et al 2022;Hou et al 2022), the CME three-part structure (Devi et al 2022), the eruption mechanism (Yamasaki et al 2022), the Sun-as-a-star spectroscopic characteristics (Xu et al 2022), the solar energetic particles (Li et al 2022), and the geomagnetic effects (Papaioannou et al 2022). It would be of great interest to check in what degree such a geoeffective solar eruption can be reproduced with a data-driven radiative MHD model.…”

Section: Event Overview and Numerical Setupsupporting

confidence: 65%

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Guo

Zhong

et al. 2023

ApJS

View full text Add to dashboard Cite

Solar filament eruptions, flares, and coronal mass ejections (CMEs) are manifestations of drastic releases of energy in the magnetic field, which are related to many eruptive phenomena, from the Earth’s magnetosphere to black hole accretion disks. With the availability of high-resolution magnetograms on the solar surface, observational data-based modeling is a promising way to quantitatively study the underlying physical mechanisms behind observations. By incorporating thermal conduction and radiation losses in the energy equation, we develop a new data-driven radiative magnetohydrodynamic model, which has the capability of capturing the thermodynamic evolution compared to our previous zero-β model. Our numerical results reproduce the major observational characteristics of the X1.0 flare on 2021 October 28 in NOAA active region 12887, including the morphology of the eruption, the kinematics of the flare ribbons, extreme ultraviolet (EUV) radiations, and the two components of the EUV waves predicted by the magnetic stretching model, i.e., a fast-mode shock wave and a slower apparent wave, due to successive stretching of the magnetic field lines. Moreover, some intriguing phenomena are revealed in the simulation. We find that flare ribbons separate initially and ultimately stop at the outer stationary quasi-separatrix layers (QSLs). Such outer QSLs correspond to the border of the filament channel and determine the final positions of flare ribbons, which can be used to predict the size and the lifetime of a flare before it occurs. In addition, the side views of the synthesized EUV and white-light images exhibit typical three-part structures of CMEs, where the bright leading front is roughly cospatial with the nonwave component of the EUV wave, reinforcing the use of the magnetic stretching model for the slow component of EUV waves.

show abstract

Section: Event Overview and Numerical Setupsupporting

confidence: 65%

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Guo

Zhong

et al. 2023

ApJS

View full text Add to dashboard Cite

show abstract

“…This event produced a strong CME which has been well studied in many papers (Hou et al 2022;Li et al 2022;Papaioannou et al 2022;Xu et al 2022). It is thus of new interest how this MFR grows into the CME, although the present simulation domain is not large enough to fully trace the MFR in a long range.…”

Section: Discussionmentioning

confidence: 90%

A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28

Yamasaki

Inoue

Bamba

et al. 2022

ApJ

View full text Add to dashboard Cite

The solar active region NOAA 12887 produced a strong X1.0 flare on 2021 October 28, which exhibits X-shaped flare ribbons and a circle-shaped erupting filament. To understand the eruption process with these characteristics, we conducted a data-constrained magnetohydrodynamics simulation using a nonlinear force-free field of the active region about an hour before the flare as the initial condition. Our simulation reproduces the filament eruption observed in the Hα images of GONG and the 304 Å images of SDO/AIA, and suggests that two mechanisms can possibly contribute to the magnetic eruption. One is the torus instability of the preexisting magnetic flux rope (MFR) and the other is upward pushing by magnetic loops newly formed below the MFR via continuous magnetic reconnection between two sheared magnetic arcades. The presence of this reconnection is evidenced by the SDO/AIA observations of the 1600 Å brightening in the footpoints of the sheared arcades at the flare onset. To clarify which process is more essential for the eruption, we performed an experimental simulation in which the reconnection between the sheared field lines is suppressed. In this case too, the MFR could erupt, but at a much reduced rising speed. We interpret this result as indicating that the eruption is not only driven by the torus instability, but additionally accelerated by newly formed and rising magnetic loops under continuous reconnection.

show abstract

“…As for the SEP characteristics, the peak proton flux with E >10 MeV turned out only ~30 pfu (1 pfu = 1 particle cm −2 s −1 sr −1 ) which is lower than that observed in most GLEs (Papaioannou et al 2022;Li et al 2022). The fact that the >10 MeV proton flux remained increased (albeit with a softer spectrum) for almost a week was due primarily to the delayed prolonged acceleration, associated with the post-eruption energy release (see below) and the CME-driven shock from the given flare, and, then, to a number of additional overlapping proton flares and CMEs.…”

Section: Overview Of the Eventmentioning

confidence: 67%

“…The estimated plane-of-sky speed of CME and its nose white-light shock were about 1240 and 1640 km 𝑠 −1 , respectively, i.e. quite high, but noticeably less than in most GLEs (see Li et al 2022;Papaioannou et al 2022). The intensive type II and III radio bursts with components from metric to kilometer wavelengths accompanied the flare and CME (Klein et al 2022).…”

Section: Overview Of the Eventmentioning

confidence: 91%

“…Besides the aforementioned paper by Papaioannou et al (2022), there are several other publications devoted to the analysis of the SEP-GLE73 event and associated solar activity phenomena: Battaglia, Collier, & Krucker (2022); Hou et al (2022); Li et al (2022); Klein et al (2022); Li et al (2022); Mishev et al (2022); Xu et al (2022). The solar manifestations of this event were observed with a number of spacecraft, in particular, with the Geostationary Operational Environmental Satellite (GOES; https://www.ngdc.noaa.gov/stp/satellite/goes/), the Solar and Heliospheric Observatory (SOHO; Domingo et al 1995), the Solar Dynamics Observatory (SDO; Pesnell, Thompson, & Chamberlin 2012), the Solar TErrestrial RElations Observatory (STEREO-A; Kaiser et al 2008), the Parker Solar Probe (PSP; Fox et al 2016), and the Solar Orbiter (SolO; Müller et al 2020).…”

Section: Overview Of the Eventmentioning

confidence: 99%

See 1 more Smart Citation

On some features of the solar proton event on 2021 October 28 – GLE73

Chertok

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In addition to several recent articles devoted to the rare event of ground-level enhancement of the solar relativistic proton flux observed on 2021 October 28 – GLE73, we study the 10–100 MeV solar energetic particle (SEP) component of this event. Based on the GOES satellite data for 26 GLEs recorded since 1986, we have formed a scatter plot displaying the ratio of the peak fluxes of the >10 MeV (J10) and >100 MeV (J100 ) protons and their energy spectra. Two extreme characteristics of the prompt component of the SEP-GLE73 event were revealed: (1) very small J10 and J100 proton fluxes and (2) a very hard energetic spectrum in the 10–100 MeV range. There are only two events with these characteristics similar to SEP–GLE73 namely, GLE40 (1989 July 25) and GLE46 (1989 November 15). A correspondence was demonstrated between the hard frequency spectrum of microwave radio bursts of initiating flares and the hard SEP energy spectrum of these two and other GLEs. These results suggest that the flare magnetic reconnection both in the impulsive and post-eruption phases plays an important role in the acceleration of the SEP–GLE protons.

show abstract

Solar Energetic Particles Produced during Two Fast Coronal Mass Ejections

Cited by 18 publications

References 38 publications

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

A Data-constrained Magnetohydrodynamic Simulation of the X1.0 Solar Flare of 2021 October 28

On some features of the solar proton event on 2021 October 28 – GLE73

Contact Info

Product

Resources

About