Detail publikace

THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11

HABBAL, S. DRUCKMÜLLER, M. MORGAN, H. DING, A. JOHNSON, J. DRUCKMÜLLEROVÁ, H. DAW, A. ARNDT, M. DIETZEL, M. SAKEN, J.

Originální název

THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11

Typ

článek v časopise ve Web of Science, Jimp

Jazyk

angličtina

Originální abstrakt

We report on the first multi-wavelength coronal observations, taken simultaneously in white light, H alpha 656.3 nm, Fe ix 435.9 nm, Fe x 637.4 nm, Fe xi 789.2 nm, Fe xiii 1074.7 nm, Fe xiv 530.3 nm, and Ni xv 670.2 nm, during the total solar eclipse of 2010 July 11 from the atoll of Tatakoto in French Polynesia. The data enabled temperature differentiations as low as 0.2 x 106 K. The first-ever images of the corona in Fe ix and Ni xv showed that there was very little plasma below 5 x 105 K and above 2.5 x 106 K. The suite of multi-wavelength observations also showed that open field lines have an electron temperature near 1x106 K, while the hottest, 2x106 K, plasma resides in intricate loops forming the bulges of streamers, also known as cavities, as discovered in our previous eclipse observations. The eclipse images also revealed unusual coronal structures, in the form of ripples and streaks, produced by the passage of coronal mass ejections and eruptive prominences prior to totality, which could be identified with distinct temperatures for the first time. These trails were most prominent at 106 K. Simultaneous Fe x 17.4 nm observations from Proba2/SWAP provided the first opportunity to compare Fe x emission at 637.4 nm with its extreme-ultraviolet (EUV) counterpart. This comparison demonstrated the unique diagnostic capabilities of the coronal forbidden lines for exploring the evolution of the coronal magnetic field and the thermodynamics of the coronal plasma, in comparison with their EUV counterparts in the distance range of 1-3R. These diagnostics are currently missing from present space-borne and ground-based observatories.

Klíčová slova

eclipses - solar wind - Sun: corona

Autoři

HABBAL, S.; DRUCKMÜLLER, M.; MORGAN, H.; DING, A.; JOHNSON, J.; DRUCKMÜLLEROVÁ, H.; DAW, A.; ARNDT, M.; DIETZEL, M.; SAKEN, J.

Rok RIV

2011

Vydáno

20. 6. 2011

Nakladatel

Chicago Journals

Místo

Chicago, USA

ISSN

0004-637X

Periodikum

ASTROPHYSICAL JOURNAL

Ročník

734

Číslo

1

Stát

Spojené státy americké

Strany od

120

Strany do

137

Strany počet

18

BibTex

@article{BUT73126,
  author="Shadia Rifai {Habbal} and Miloslav {Druckmüller} and Huw {Morgan} and Adalbert {Ding} and Judd {Johnson} and Hana {Druckmüllerová} and Adrian {Daw} and Martina {Arndt} and Martin {Dietzel} and Jon {Saken}",
  title="THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11",
  journal="ASTROPHYSICAL JOURNAL",
  year="2011",
  volume="734",
  number="1",
  pages="120--137",
  issn="0004-637X"
}