Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations
Spectropolarimetry using IR wavelength of 1075 nm has been proved to be a powerful tool for directly mapping solar coronal magnetic fields including transverse component directions and line-of-sight component intensities. Solar tomography, or stereoscopy based on EUV observations, can supply 3-D...
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| Format: | Article |
| Language: | English |
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Copernicus Publications
2009-07-01
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| Series: | Annales Geophysicae |
| Online Access: | https://www.ann-geophys.net/27/2771/2009/angeo-27-2771-2009.pdf |
| _version_ | 1818014431449186304 |
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| author | Y. Liu Y. Liu |
| author_facet | Y. Liu Y. Liu |
| author_sort | Y. Liu |
| collection | DOAJ |
| description | Spectropolarimetry using IR wavelength of 1075 nm has been proved
to be a powerful tool for directly mapping solar coronal magnetic
fields including transverse component directions and line-of-sight
component intensities. Solar tomography, or stereoscopy based on EUV
observations, can supply 3-D information for some magnetic field
lines in bright EUV loops. In a previous paper \citep{liu08} the
locations of the IR emission sources in the 3-D coordinate system
were inferred from the comparison between the polarization data and
the potential-field-source-surface (PFSS) model, for one of five
west limb regions in the corona (Lin et al., 2004). The paper shows that
the region with the loop system in the active region over the
photospheric area with strong magnetic field intensity is the region
with a dominant contribution to the observed Stokes signals. So, the
inversion of the measured Stokes parameters could be done assuming
that most of the signals come from a relatively thin layer over the
area with a large photospheric magnetic field strength. Here, the
five limb coronal regions are studied together in order to study the
spatial correlation between the bright EUV loop features and the
inferred IR emission sources. It is found that, for the coronal
regions above the stronger photospheric magnetic fields, the
locations of the IR emission sources are closer to or more
consistent with the bright EUV loop locations than those above
weaker photospheric fields. This result suggests that the structures
of the coronal magnetic fields observed at IR and EUV wavelengths
may be different when weak magnetic fields present there. |
| first_indexed | 2024-04-14T06:44:30Z |
| format | Article |
| id | doaj.art-1a82a6fdb39a4bb5929ff39fcb75890c |
| institution | Directory Open Access Journal |
| issn | 0992-7689 1432-0576 |
| language | English |
| last_indexed | 2024-04-14T06:44:30Z |
| publishDate | 2009-07-01 |
| publisher | Copernicus Publications |
| record_format | Article |
| series | Annales Geophysicae |
| spelling | doaj.art-1a82a6fdb39a4bb5929ff39fcb75890c2022-12-22T02:07:12ZengCopernicus PublicationsAnnales Geophysicae0992-76891432-05762009-07-01272771277710.5194/angeo-27-2771-2009Coronal magnetic fields inferred from IR wavelength and comparison with EUV observationsY. Liu0Y. Liu1Yunnan Astronomical Observatory, National Astronomical Observatories, Kunming 650011, ChinaInstitute for Astronomy, University of Hawaii, 34 Ohia Ku Street, Pukalani, HI 96768, USASpectropolarimetry using IR wavelength of 1075 nm has been proved to be a powerful tool for directly mapping solar coronal magnetic fields including transverse component directions and line-of-sight component intensities. Solar tomography, or stereoscopy based on EUV observations, can supply 3-D information for some magnetic field lines in bright EUV loops. In a previous paper \citep{liu08} the locations of the IR emission sources in the 3-D coordinate system were inferred from the comparison between the polarization data and the potential-field-source-surface (PFSS) model, for one of five west limb regions in the corona (Lin et al., 2004). The paper shows that the region with the loop system in the active region over the photospheric area with strong magnetic field intensity is the region with a dominant contribution to the observed Stokes signals. So, the inversion of the measured Stokes parameters could be done assuming that most of the signals come from a relatively thin layer over the area with a large photospheric magnetic field strength. Here, the five limb coronal regions are studied together in order to study the spatial correlation between the bright EUV loop features and the inferred IR emission sources. It is found that, for the coronal regions above the stronger photospheric magnetic fields, the locations of the IR emission sources are closer to or more consistent with the bright EUV loop locations than those above weaker photospheric fields. This result suggests that the structures of the coronal magnetic fields observed at IR and EUV wavelengths may be different when weak magnetic fields present there.https://www.ann-geophys.net/27/2771/2009/angeo-27-2771-2009.pdf |
| spellingShingle | Y. Liu Y. Liu Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations Annales Geophysicae |
| title | Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations |
| title_full | Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations |
| title_fullStr | Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations |
| title_full_unstemmed | Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations |
| title_short | Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations |
| title_sort | coronal magnetic fields inferred from ir wavelength and comparison with euv observations |
| url | https://www.ann-geophys.net/27/2771/2009/angeo-27-2771-2009.pdf |
| work_keys_str_mv | AT yliu coronalmagneticfieldsinferredfromirwavelengthandcomparisonwitheuvobservations AT yliu coronalmagneticfieldsinferredfromirwavelengthandcomparisonwitheuvobservations |