Show simple item record Li, Xing 2008-12-04T09:42:01Z 2008-12-04T09:42:01Z 2003-07-04
dc.identifier.citation Li , X 2003 , ' Transition region, coronal heating and the fast solar wind ' Astronomy and Astrophysics , vol 406 , no. 1 , pp. 345-356 . DOI: 10.1051/0004-6361:20030676 en
dc.identifier.issn 0004-6361
dc.identifier.other PURE: 89980
dc.identifier.other PURE UUID: 098f4c9c-0aec-4098-a930-001b6c20b1f9
dc.identifier.other dspace: 2160/1333
dc.identifier.other DSpace_20121128.csv: row: 1156
dc.identifier.other Scopus: 0038442154
dc.identifier.uri en
dc.identifier.uri en
dc.description Li, Xing, 'Transition region, coronal heating and the fast solar wind', Astronomy and Astrophysics (2003) 406 pp.345-356 RAE2008 en
dc.description.abstract It is assumed that magnetic flux tubes are strongly concentrated at the boundaries of supergranule convection cells. A power law spectrum of high frequency Alfvén waves with a spectral index -1 originating from the sun is assumed to supply all the energy needed to energize the plasma flowing in such magnetic flux tubes. At the high frequency end, the waves are eroded by ions due to ion cyclotron resonance. The magnetic flux concentration is essential since it allows a sufficiently strong energy flux to be carried by high frequency ion cyclotron waves and these waves can be readily released at the coronal base by cyclotron resonance. The main results are: 1. The waves are capable of creating a steep transition region, a hot corona and a fast solar wind if both the wave frequency is high enough and the magnetic flux concentration is sufficiently strong in the boundaries of the supergranule convection zone. 2. By primarily heating alpha particles only, it is possible to produce a steep transition region, a hot corona and a fast solar wind. Coulomb coupling plays a key role in transferring the thermal energy of alpha particles to protons and electrons at the corona base. The electron thermal conduction then does the remaining job to create a sharp transition region. 3. Plasma species (even ions) may already partially lose thermal equilibrium in the transition region, and minor ions may already be faster than protons at the very base of the corona. 4. The model predicts high temperature alpha particles (Tα ∼ 2 x 107 K) and low proton temperatures (Tp <106 K) between 2 and 4 solar radii, suggesting that hydrogen Lyman lines observed by UVCS above coronal holes may be primarily broadened by Alfvén waves in this range. en
dc.format.extent 12 en
dc.language.iso eng
dc.relation.ispartof Astronomy and Astrophysics en
dc.rights en
dc.subject Sun: corona en
dc.subject Sun: solar wind en
dc.subject Sun: transition region en
dc.title Transition region, coronal heating and the fast solar wind en
dc.type /dk/atira/pure/researchoutput/researchoutputtypes/contributiontojournal/article en
dc.contributor.institution Department of Physics en
dc.contributor.institution Mathematics and Physics en
dc.description.status Peer reviewed en

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