View in EDS

Three‐Dimensional Structure of the Corona During WHPI Campaign Rotations CR‐2219 and CR‐2223.

Saved in:
Bibliographic Details
Title: Three‐Dimensional Structure of the Corona During WHPI Campaign Rotations CR‐2219 and CR‐2223.
Authors: Lloveras, D. G.1 (AUTHOR) dlloveras@iafe.uba.ar, Vásquez, A. M.1,2 (AUTHOR), Nuevo, F. A.1,3 (AUTHOR), Frazin, R. A.4 (AUTHOR), Manchester, W.4 (AUTHOR), Sachdeva, N.4 (AUTHOR), Van der Holst, B.4 (AUTHOR), Lamy, P.5 (AUTHOR), Gilardy, H.5 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Jun2022, Vol. 127 Issue 6, p1-20. 20p.
Subject Terms: Electron density, Theory of wave motion, Plasma Alfven waves, Solar corona, Solar cycle, Terminal velocity, Planetary rotation, Rotational motion
Abstract: Differential emission measure tomography (DEMT) and white light (WL) tomography were applied to study the three‐dimensional (3D) structure of the global solar corona for two Whole Heliosphere and Planetary Interactions campaign periods, Carrington rotations 2219 and 2223. With DEMT, Solar Dynamics Observatory/Atmospheric Imaging Assembly images were used to reconstruct the 3D coronal electron density and temperature in the range of heliocentric distance 1.02–1.25 R⊙. With WL tomography, Solar and Heliospheric Observatory/Large Angle and Spectrometric COronagraph‐C2 images were used to reconstruct the 3D electron density in the range of heliocentric distance 2.5–6.0 R⊙. The two periods were also simulated with the 3D‐magneto‐hydrodynamic Alfvén Wave Solar Model (AWSoM), and its results compared in detail with the reconstructions. The DEMT analysis reveals a 20% less dense and 20% hotter corona than for rotations corresponding to the solar cycle 23/24 deep minimum. The electron density and temperature of the AWSoM model agree with DEMT results within 10% and 20%, respectively, while its electron density overestimates results of WL tomography up to 75%. The slow (fast) component of the terminal wind speed of the model is found to be associated with field lines characterized by larger (smaller) values of the tomographic density and temperature at the coronal base. DEMT reconstructions reveal the coronal plasma to be ubiquitously characterized by temperature variability of up to ≈45% over spatial scales of order ∼104 km. Taking into account this level of fine‐structure by global models may be consequential for their predictions on wave propagation in the corona. Key Points: Tomographic analysis of Whole Heliosphere and Planetary Interactions rotations indicate a corona 20% less dense and 20% hotter compared to rotations of the SC 23/24 solar minimumThe model density and temperature agree with extreme ultraviolet tomography results within 20% and overestimates up to 75% the density from white light tomographyThe wind model slow/fast component is associated with field lines characterized by larger/lower tomographic electron density and temperature [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: GreenFILE
FullText Text:
  Availability: 0
Header DbId: 8gh
DbLabel: GreenFILE
An: 157689971
AccessLevel: 6
PubType: Academic Journal
PubTypeId: academicJournal
PreciseRelevancyScore: 0
IllustrationInfo
Items – Name: Title
  Label: Title
  Group: Ti
  Data: Three‐Dimensional Structure of the Corona During WHPI Campaign Rotations CR‐2219 and CR‐2223.
– Name: Author
  Label: Authors
  Group: Au
  Data: <searchLink fieldCode="AR" term="%22Lloveras%2C+D%2E+G%2E%22">Lloveras, D. G.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> dlloveras@iafe.uba.ar</i><br /><searchLink fieldCode="AR" term="%22Vásquez%2C+A%2E+M%2E%22">Vásquez, A. M.</searchLink><relatesTo>1,2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Nuevo%2C+F%2E+A%2E%22">Nuevo, F. A.</searchLink><relatesTo>1,3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Frazin%2C+R%2E+A%2E%22">Frazin, R. A.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Manchester%2C+W%2E%22">Manchester, W.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Sachdeva%2C+N%2E%22">Sachdeva, N.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Van+der+Holst%2C+B%2E%22">Van der Holst, B.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Lamy%2C+P%2E%22">Lamy, P.</searchLink><relatesTo>5</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Gilardy%2C+H%2E%22">Gilardy, H.</searchLink><relatesTo>5</relatesTo> (AUTHOR)
– Name: TitleSource
  Label: Source
  Group: Src
  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Space+Physics%22">Journal of Geophysical Research. Space Physics</searchLink>. Jun2022, Vol. 127 Issue 6, p1-20. 20p.
– Name: Subject
  Label: Subject Terms
  Group: Su
  Data: <searchLink fieldCode="DE" term="%22Electron+density%22">Electron density</searchLink><br /><searchLink fieldCode="DE" term="%22Theory+of+wave+motion%22">Theory of wave motion</searchLink><br /><searchLink fieldCode="DE" term="%22Plasma+Alfven+waves%22">Plasma Alfven waves</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+corona%22">Solar corona</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+cycle%22">Solar cycle</searchLink><br /><searchLink fieldCode="DE" term="%22Terminal+velocity%22">Terminal velocity</searchLink><br /><searchLink fieldCode="DE" term="%22Planetary+rotation%22">Planetary rotation</searchLink><br /><searchLink fieldCode="DE" term="%22Rotational+motion%22">Rotational motion</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: Differential emission measure tomography (DEMT) and white light (WL) tomography were applied to study the three‐dimensional (3D) structure of the global solar corona for two Whole Heliosphere and Planetary Interactions campaign periods, Carrington rotations 2219 and 2223. With DEMT, Solar Dynamics Observatory/Atmospheric Imaging Assembly images were used to reconstruct the 3D coronal electron density and temperature in the range of heliocentric distance 1.02–1.25 R⊙. With WL tomography, Solar and Heliospheric Observatory/Large Angle and Spectrometric COronagraph‐C2 images were used to reconstruct the 3D electron density in the range of heliocentric distance 2.5–6.0 R⊙. The two periods were also simulated with the 3D‐magneto‐hydrodynamic Alfvén Wave Solar Model (AWSoM), and its results compared in detail with the reconstructions. The DEMT analysis reveals a 20% less dense and 20% hotter corona than for rotations corresponding to the solar cycle 23/24 deep minimum. The electron density and temperature of the AWSoM model agree with DEMT results within 10% and 20%, respectively, while its electron density overestimates results of WL tomography up to 75%. The slow (fast) component of the terminal wind speed of the model is found to be associated with field lines characterized by larger (smaller) values of the tomographic density and temperature at the coronal base. DEMT reconstructions reveal the coronal plasma to be ubiquitously characterized by temperature variability of up to ≈45% over spatial scales of order ∼104 km. Taking into account this level of fine‐structure by global models may be consequential for their predictions on wave propagation in the corona. Key Points: Tomographic analysis of Whole Heliosphere and Planetary Interactions rotations indicate a corona 20% less dense and 20% hotter compared to rotations of the SC 23/24 solar minimumThe model density and temperature agree with extreme ultraviolet tomography results within 20% and overestimates up to 75% the density from white light tomographyThe wind model slow/fast component is associated with field lines characterized by larger/lower tomographic electron density and temperature [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
PLink https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=8gh&AN=157689971
RecordInfo BibRecord:
  BibEntity:
    Identifiers:
      – Type: doi
        Value: 10.1029/2022JA030406
    Languages:
      – Code: eng
        Text: English
    PhysicalDescription:
      Pagination:
        PageCount: 20
        StartPage: 1
    Subjects:
      – SubjectFull: Electron density
        Type: general
      – SubjectFull: Theory of wave motion
        Type: general
      – SubjectFull: Plasma Alfven waves
        Type: general
      – SubjectFull: Solar corona
        Type: general
      – SubjectFull: Solar cycle
        Type: general
      – SubjectFull: Terminal velocity
        Type: general
      – SubjectFull: Planetary rotation
        Type: general
      – SubjectFull: Rotational motion
        Type: general
    Titles:
      – TitleFull: Three‐Dimensional Structure of the Corona During WHPI Campaign Rotations CR‐2219 and CR‐2223.
        Type: main
  BibRelationships:
    HasContributorRelationships:
      – PersonEntity:
          Name:
            NameFull: Lloveras, D. G.
      – PersonEntity:
          Name:
            NameFull: Vásquez, A. M.
      – PersonEntity:
          Name:
            NameFull: Nuevo, F. A.
      – PersonEntity:
          Name:
            NameFull: Frazin, R. A.
      – PersonEntity:
          Name:
            NameFull: Manchester, W.
      – PersonEntity:
          Name:
            NameFull: Sachdeva, N.
      – PersonEntity:
          Name:
            NameFull: Van der Holst, B.
      – PersonEntity:
          Name:
            NameFull: Lamy, P.
      – PersonEntity:
          Name:
            NameFull: Gilardy, H.
    IsPartOfRelationships:
      – BibEntity:
          Dates:
            – D: 01
              M: 06
              Text: Jun2022
              Type: published
              Y: 2022
          Identifiers:
            – Type: issn-print
              Value: 21699380
          Numbering:
            – Type: volume
              Value: 127
            – Type: issue
              Value: 6
          Titles:
            – TitleFull: Journal of Geophysical Research. Space Physics
              Type: main
ResultId 1