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Shohei Nishimoto
National Defense Academy of Japan
Corresponding Author
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X-rays and extreme ultraviolet (EUV) emissions from solar flares rapidly change the physical composition of the Earth’s thermosphere and ionosphere, thereby causing space weather phenomena such as communication failures. To predict the effects of flare emissions on the Earth’s upper atmosphere, numerous empirical and physical models have been developed. We verify the extent of reproducing the flare emission spectra using a one-dimensional hydrodynamic calculation and the CHIANTI atomic database. To verify the proposed model, we use the observed EUV spectra obtained by the extreme ultraviolet variability (EVE) on board the Solar Dynamics Observatory (SDO). We examined the “EUV flare time-integrated irradiance” and “EUV flare line rise time” of the EUV emissions for 21 events by comparing the calculation results of the proposed model and observed EUV spectral data. The proposed model succeeded in reproducing the EUV flare time-integrated irradiance of the Fe VIII 131 Å , Fe XVIII 94 Å, and Fe XX 133 Å, as well as the 55 to 355 Å and 55 to 135 Å bands. For the EUV flare line rise time, there was acceptable correlation between the proposed model estimations and observations for all Fe flare emission lines. These results demonstrate that the proposed model can reproduce the EUV flare emission spectra from the emitting plasma with relatively high formation temperature. This indicates that the physics-based model is effective for the accurate reproduction of EUV spectral flux.
Keywords
Solar flare, X-ray emission, EUV emission, Space weather
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This is a list of supplementary files associated with this preprint. Click to download.
- table1.xls
Table 1. Comparative parameters for the M9.9-class flare on January 1, 2014.
- table2.xls
Table 2. Flare event list for this study.
- graphicabst.png
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CURRENT STATUS: Published
View the published article at Earth, Planets and Space.
Version (no preprint)
Posted 26 Feb, 2021
Editorial decision: Minor Revision
On 26 Feb, 2021
Editor assigned
On 19 Feb, 2021
Submission checks complete
On 19 Feb, 2021
Editor invited
On 19 Feb, 2021
This version was not preprinted
Version 2
Posted 07 Dec, 2020
No community comments so far
Editorial decision: Minor Revision
On 31 Jan, 2021
Review #1 received
Received 07 Jan, 2021
Reviewer #1 agreed
On 03 Jan, 2021
Reviewers invited
Invitations sent on 30 Nov, 2020
Editor assigned
On 24 Nov, 2020
Submission checks complete
On 24 Nov, 2020
Editor invited
On 24 Nov, 2020
No comments provided
Editorial decision: Minor Revision
On 21 Oct, 2020
Review #1 received
Received 12 Oct, 2020
Reviewer #1 agreed
On 16 Sep, 2020
Reviewers invited
Invitations sent on 12 Aug, 2020
Editor assigned
On 08 Aug, 2020
Submission checks complete
On 07 Aug, 2020
Editor invited
On 07 Aug, 2020
First submitted
On 05 Aug, 2020
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Comments: 0
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A new preprint design is coming!
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See the published version of this preprint at Earth, Planets and Space.
This is a preprint, a preliminary version of a manuscript that has not completed peer review at a journal. Research Square does not conduct peer review prior to posting preprints. The posting of a preprint on this server should not be interpreted as an endorsement of its validity or suitability for dissemination as established information or for guiding clinical practice.
Learn more about In Review
Full paper
Shohei Nishimoto
National Defense Academy of Japan
Corresponding Author
Badges
Prescreen
This manuscript passed our Prescreen assessment
Complete author information
Appropriate declaration statements
Potential risks to human health
Prescreen
Peer Review Timeline
CURRENT STATUS: Published
View the published article at Earth, Planets and Space.
Version (no preprint)
Posted 26 Feb, 2021
Editorial decision: Minor Revision
On 26 Feb, 2021
Editor assigned
On 19 Feb, 2021
Submission checks complete
On 19 Feb, 2021
Editor invited
On 19 Feb, 2021
This version was not preprinted
Version 2
Posted 07 Dec, 2020
No community comments so far
Editorial decision: Minor Revision
On 31 Jan, 2021
Review #1 received
Received 07 Jan, 2021
Reviewer #1 agreed
On 03 Jan, 2021
Reviewers invited
Invitations sent on 30 Nov, 2020
Editor assigned
On 24 Nov, 2020
Submission checks complete
On 24 Nov, 2020
Editor invited
On 24 Nov, 2020
No comments provided
Editorial decision: Minor Revision
On 21 Oct, 2020
Review #1 received
Received 12 Oct, 2020
Reviewer #1 agreed
On 16 Sep, 2020
Reviewers invited
Invitations sent on 12 Aug, 2020
Editor assigned
On 08 Aug, 2020
Submission checks complete
On 07 Aug, 2020
Editor invited
On 07 Aug, 2020
First submitted
On 05 Aug, 2020
Metrics
Comments: 0
PDF Downloads: ...
HTML Views: ...
License:
This work is licensed under a CC BY 4.0 License. Read Full License
View the published article at Earth, Planets and Space.
X-rays and extreme ultraviolet (EUV) emissions from solar flares rapidly change the physical composition of the Earth’s thermosphere and ionosphere, thereby causing space weather phenomena such as communication failures. To predict the effects of flare emissions on the Earth’s upper atmosphere, numerous empirical and physical models have been developed. We verify the extent of reproducing the flare emission spectra using a one-dimensional hydrodynamic calculation and the CHIANTI atomic database. To verify the proposed model, we use the observed EUV spectra obtained by the extreme ultraviolet variability (EVE) on board the Solar Dynamics Observatory (SDO). We examined the “EUV flare time-integrated irradiance” and “EUV flare line rise time” of the EUV emissions for 21 events by comparing the calculation results of the proposed model and observed EUV spectral data. The proposed model succeeded in reproducing the EUV flare time-integrated irradiance of the Fe VIII 131 Å , Fe XVIII 94 Å, and Fe XX 133 Å, as well as the 55 to 355 Å and 55 to 135 Å bands. For the EUV flare line rise time, there was acceptable correlation between the proposed model estimations and observations for all Fe flare emission lines. These results demonstrate that the proposed model can reproduce the EUV flare emission spectra from the emitting plasma with relatively high formation temperature. This indicates that the physics-based model is effective for the accurate reproduction of EUV spectral flux.
Figure 1
Figure 2
Figure 3
Figure 4
Figure 5
Figure 6
Figure 7
Figure 8
Figure 9
Figure 10
Figure 11
Figure 12
This is a list of supplementary files associated with this preprint. Click to download.
- table1.xls
Table 1. Comparative parameters for the M9.9-class flare on January 1, 2014.
- table2.xls
Table 2. Flare event list for this study.
- graphicabst.png
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