Publication detail

Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle

HABBAL, S. DRUCKMÜLLER, M. NATHALIA, A. DING, A. JOHNSON, J. ŠTARHA, P. HODEROVÁ, J. BOE, B. CONSTANTINIOU, S. ARNDT, M.

Original Title

Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle

Type

journal article in Web of Science

Language

English

Original Abstract

This letter capitalizes on a unique set of total solar eclipse observations acquired between 2006 and 2020 in white light, Fe xi 789.2 nm (T-fexi = 1.2 0.1 MK), and Fe xiv 530.3 nm (T-fexiv = 1.8 0.1 MK) emission complemented by in situ Fe charge state and proton speed measurements from Advanced Composition Explorer/SWEPAM-SWICS to identify the source regions of different solar wind streams. The eclipse observations reveal the ubiquity of open structures invariably associated with Fe xi emission from Fe10+ and hence a constant electron temperature, T-c = T-fexi, in the expanding corona. The in situ Fe charge states are found to cluster around Fe10+, independently of the 300-700 km s(-1) stream speeds, referred to as the continual solar wind. Thus, Fe10+ yields the fiducial link between the continual solar wind and its T-fexi sources at the Sun. While the spatial distribution of Fe xiv emission from Fe13+ associated with streamers changes throughout the solar cycle, the sporadic appearance of charge states >Fe11+ in situ exhibits no cycle dependence regardless of speed. These latter streams are conjectured to be released from hot coronal plasmas at temperatures >= T-fexiv within the bulge of streamers and from active regions, driven by the dynamic behavior of prominences magnetically linked to them. The discovery of continual streams of slow, intermediate, and fast solar wind characterized by the same T-fexi in the expanding corona places new constraints on the physical processes shaping the solar wind.

Keywords

Solar prominences; Solar cycle; Solar wind; Total eclipses; Solar coronal streamers; Solar magnetic fields; Solar coronal heating; Solar coronal mass ejections; Solar corona

Authors

HABBAL, S.; DRUCKMÜLLER, M.; NATHALIA, A.; DING, A.; JOHNSON, J.; ŠTARHA, P.; HODEROVÁ, J.; BOE, B.; CONSTANTINIOU, S.; ARNDT, M.

Released

12. 4. 2021

Publisher

IOP PUBLISHING LTD

Location

BRISTOL

ISBN

2041-8205

Periodical

Astrophysical Journal Letters

Year of study

911

Number

1

State

United States of America

Pages from

1

Pages to

14

Pages count

14

URL

https://iopscience.iop.org/article/10.3847/2041-8213/abe775/pdf

Full text in the Digital Library

http://hdl.handle.net/11012/200986

BibTex

@article{BUT171593,
  author="Shadia Rifai {Habbal} and Miloslav {Druckmüller} and Alzate {Nathalia} and Adalbert {Ding} and Judd {Johnson} and Pavel {Štarha} and Jana {Hoderová} and Benjamin {Boe} and Sage {Constantiniou} and Martina {Arndt}",
  title="Identifying the Coronal Source Regions of Solar Wind Streams from Total Solar Eclipse Observations and in situ Measurements Extending over a Solar Cycle",
  journal="Astrophysical Journal Letters",
  year="2021",
  volume="911",
  number="1",
  pages="1--14",
  doi="10.3847/2041-8213/abe775",
  issn="2041-8205",
  url="https://iopscience.iop.org/article/10.3847/2041-8213/abe775/pdf"
}