4 edition of Mechanisms of chromospheric and coronal heating found in the catalog.
Mechanisms of chromospheric and coronal heating
|Statement||P. Ulmschneider, E.R. Priest, R. Rosner (eds.).|
|Contributions||Ulmschneider, P. 1938-, Priest, E. R. 1943-, Rosner, Robert., Heidelberg Conference, Mechanisms of Chromospheric and Coronal Heating (1990)|
|LC Classifications||QB809 .M43 1991|
|The Physical Object|
|Pagination||xiv, 649 p. :|
|Number of Pages||649|
|ISBN 10||3540534369, 0387534369|
|LC Control Number||90025609|
1. The coronal heating problem. The so-called ‘coronal heating’ problem has existed for 75 years, since the solar corona was first demonstrated to contain plasma with temperatures of 1 million degrees kelvin and above, much higher than the photospheric surface temperature of approximately K [1,2].There have been many advances over this period, with great progress in Cited by: Chromospheric and Coronal Heating Mechanisms II. Space Science Reviews, Vol Issue , pp. Mani Chandra, Arnab Dhabal, Raziman T V Coronal Heating Problem.
Abstract: Inspired by recent observations suggesting that photospheric magnetic flux cancellation occurs much more frequently than previously thought, we analytically estimated the energy released from reconnection driven by photospheric flux cancellation, and proposed that it can act as a mechanism for chromospheric and coronal heating (Priest et al., ).Author: P. Syntelis, E.R. Priest. Chromospheric and coronal heating mechanisms: Author(eng) Stein, R. F.; Leibacher, J. Author Affiliation(eng) Lockheed Missiles and Space Co. Issue Date: Language: eng: Description: Dissipation mechanisms in the chromosphere were : J. Leibacher, R. F. Stein.
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One of the great problems of astrophysics is the unanswered question about the origin and mechanism of chromospheric and coronal heating.
Just how these outer stellar envelopes are heated is of fundamental importance, since all stars have hot chromospheric and coronal shells where the temperature rises to millions of degrees, comparable to the temperatures in the stars' : Paperback. One of the great problems of astrophysics is the unanswered question about the origin and mechanism of chromospheric and coronal heating.
Just how these outer stellar envelopes are heated is of fundamental importance, since all stars have hot chromospheric and coronal shells where the temperature rises to millions of degrees, comparable to the temperatures in the stars' cores.
One of the great problems of astrophysics is the unanswered question about the origin and mechanism of chromospheric and coronal heating. Just how these outer stellar envelopes are heated is of fundamental importance, since all stars have hot chromospheric and coronal shells where the temperature rises to millions of degrees, comparable to the temperatures in the stars' cores.
Here for. One of the paradigms about coronal heating has been the belief that the mean or summit temperature of a coronal loop is completely insensitive to the nature of the heating mechanisms. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86AAuthor: J.
Cook. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by: 4. Section 2 discusses the necessity of chromospheric and coronal heating and describes the elementary heating processes.
Section 3 outlines the hydrodynamic heating mechanisms and Section 4 the magnetic heating by: Abstract We review the mechanisms which have been proposed for the heating of stellar chromospheres and coronae. These consist of heating by acoustic waves, by slow and fast mhd waves, by body and surface Alfvén waves, by current or magnetic field dissipation, by microflare heating and by heating due to bulk flows and magnetic flux by: Mechanisms of Chromospheric and Coronal Heating (Invited review) Ulmschneider, P.; Musielak, Z.
Abstract. Publication: Current Theoretical Models and Future High Resolution Solar Observations: Preparing for ATST. Pub Date: Bibcode: ASPCU full text sources Cited by: 1. Request PDF | On Jan 1,P. Ulmschneider and others published Mechanisms of Chromospheric and Coronal Heating (Invited review) | Find, read and cite all the research you need on ResearchGate.
Except for F-stars, the chromospheric heating of rapidly rotating late-type stars is dominated by magnetic heating either through MHD wave dissipation (AC mechanisms) or through magnetic field dissipation (DC mechanisms).
The MHD wave and magnetic field energy comes from fluid motions in the stellar convection by: ISBN: OCLC Number: Notes: Proceedings of the Heidelberg Conference, Mechanisms of Chromospheric and Coronal Heating.
A Method to Determine the Heating Mechanisms of the Solar Corona of flux cancellation for chromospheric and coronal heating.
coronal heating mechanisms can. We review the mechanisms which are thought to provide steady heating of chromospheres and coronae. It appears now fairly well established that nonmagnetic chromospheric regions of latetype stars are heated by shock dissipation of acoustic waves which are generated in the stellar surface convection zones.
Theoretical models of coronal heating mechanisms include the two main groups of DC (§ ) and AC models (§ ), which involve as a primary energy source chromospheric footpoint motion or upward leaking Alfvén waves, which are dissipated in the corona by magnetic reconnection, current cascades, MHD turbulence, Alfvén resonance, resonant absorption, or phase mixing.
NASA/ADS. Chromospheric and coronal heating mechanisms. Ulmschneider, P. Abstract. The present work discusses the basic physical mechanisms which produce the heating of stellar chromospheres and coronae and concentrates on the physics of the heating processes.
Publication: NATO Advanced Science Institutes (ASI) Series C Author: P. Ulmschneider. Title: Book Review: Mechanisms of chromospheric and coronal heating / Springer, Authors: Cook, J. Journal: Space science reviews, vol. 64, no. 1/2, p. () Bibliographic Code: SSRv C.
Complete bibliographic record Other article options Print this article. As a result of the large body of data available from solar and stellar coronae, our understanding of the mechanisms responsible for the heating of coronal plasmas to temperatures of the order of ∼ 10 8 K has changed.
The solar corona is highly structured by magnetic fields and the acoustic shocks which, according to early theories, should have acted as the coronal energy source have not been Cited by: 1.
Observing the Roots of Solar Coronal Heating - in the Chromosphere Bart De Pontieu1,4, Scott W. McIntosh2, coronal mass supply mechanism that is driven from below, in the chromosphere. To connect the chromospheric and coronal dynamics we need to coalign the coronal spec.
There are a huge range of known energy release mechanisms on the Sun (see for example Erdélyi () and references therein), many of which have been implicated for coronal heating. At the. Thus coronal mass supply in transients is inextricably linked to direct chromospheric heating processes.
Using parametric models of a chromospheric heating function and of the pre-event chromosphere, an estimate is made of the extra power required to yield the emission measure enhancement of a large event evaporatively.Recent observations at high spatial resolution have shown that magnetic flux cancellation occurs on the solar surface much more frequently than previously thought, and so this led Priest et al to propose magnetic reconnection driven by photospheric flux cancellation as a mechanism for chromospheric and coronal heating.
In particular, they estimated analytically the amount of energy Cited by: 7.Mechanisms of Chromospheric and Coronal Heating: Proceedings of the International Conference, Heidelberg, 5 8 June by Peter Ulmschneider (Editor), E.R.