A three-dimensional magnetohydrodynamic model of the global solar corona is described. The model uses observed photospheric magnetic fields as a boundary condition. A version of the model with a polytropic energy equation is used to interpret solar observations, including eclipse images of the corona, Ulysses spacecraft measurements of the interplanetary magnetic field, and coronal hole boundaries from Kitt Peak He 10 830 Å maps and extreme ultraviolet images from the Solar Heliospheric Observatory. Observed magnetic fields are used as a boundary condition to model the evolution of the solar corona during the period February 1997–March 1998. A model with an improved energy equation and Alfvén waves that is better able to model the solar wind is also presented.
REFERENCES
1.
2.
3.
L.
Acton
, S.
Tsuneta
, Y.
Ogawara
, R.
Bentley
, M.
Bruner
, R.
Canfield
, L.
Culhane
, G.
Doschek
, E.
Hiei
, and T.
Hirayama
, Science
258
, 618
(1992
).4.
D. J.
McComas
, S. J.
Bame
, B. L.
Barraclough
, W. C.
Feldman
, H. O.
Funsten
, J. T.
Gosling
, P.
Riley
, R.
Skoug
, A.
Balogh
, R.
Forsyth
, B. E.
Goldstein
, and M.
Neugebauer
, Geophys. Res. Lett.
25
, 1
(1998
).5.
B. W.
Lites
, B. C.
Low
, V.
Martı́nez Pillet
, P.
Seagraves
, A.
Skumanich
, Z. A.
Frank
, R. A.
Shine
, and S.
Tsuneta
, Astrophys. J.
446
, 877
(1995
).6.
E. N. Parker, Interplanetary Dynamical Processes (Wiley, New York, 1963).
7.
E. R. Priest, Solar Magnetohydrodynamics (Reidel, Dordrecht, 1982).
8.
E. N. Parker, Cosmical Magnetic Fields (Clarendon, Oxford, 1979).
9.
E. N. Parker, Spontaneous Current Sheets in Magnetic Fields (Oxford, New York, 1994).
10.
11.
12.
The numerical techniques used are similar to those described for a cylindrical code by
R.
Lionello
, Z.
Mikić
, and D. D.
Schnack
, J. Comput. Phys.
140
, 172
(1998
).13.
Z.
Mikić
and J. A.
Linker
, Solar Wind Eight: Proceedings of the Eight International Solar Wind Conference
, edited by D.
Winterhalter
, J. T.
Gosling
, S. R.
Habbal
, W. S.
Kurth
, and M.
Neugebauer
(Conf. Proc.
Vol. 382, American Institute of Physics
, Woodbury, NY
, 1996
), p. 104
.14.
J. A. Linker, Z. Mikić, and D. D. Schnack, Solar Drivers of Interplanetary and Terrestrial Disturbances, edited by K. S. Balasubramaniam, S. L. Keil, and R. N. Smartt (Astronomical Society of the Pacific, 1996), Conf. Series Vol. 95, p. 208.
15.
J. A. Linker, Z. Mikić, D. A. Biesecker, R. J. Forsyth, S. E. Gibson, A. J. Lazarus, A. Lecinski, P. Riley, A. Szabo, and B. J. Thompson, “Magnetohydrodynamic modeling of the solar corona during Whole Sun Month,” J. Geophys. Res. (in press).
16.
J. A. Linker, Z. Mikić, and D. D. Schnack, Proceedings of the Third SOHO Workshop—Solar Dynamic Phenomena and Solar Wind Consequences, Estes Park, CO (European Space Agency, Paris, 1994), SP-373, p. 249.
17.
18.
Z. Mikić and J. A. Linker, Coronal Mass Ejections, edited by N. Crooker, J. Joselyn, and J. Feynman (American Geophysical Union, Washington DC, 1997), Geophys. Monograph 99, p. 57.
19.
J. A. Linker and Z. Mikić, Coronal Mass Ejections, edited by N. Crooker, J. Joselyn, and J. Feynman (American Geophysical Union, Washington DC, 1997), Geophys. Monograph 99, p. 269.
20.
A. V.
Usmanov
, Solar Wind Eight: Proceedings of the Eight International Solar Wind Conference
, edited by D.
Winterhalter
, J. T.
Gosling
, S. R.
Habbal
, W. S.
Kurth
, and M.
Neugebauer
(Conf. Proc.
Vol. 382, American Institute of Physics
, Woodbury, NY
, 1996
), p. 141
.21.
A. V. Usmanov, B. P. Besser, J. M. Fritzer, and M. L. Goldstein, “Two-dimensional MHD simulation of the solar corona with WKB Alfvén waves,” J. Geophys. Res. (submitted).
22.
Y. V. Pisanko, “A composite MHD model of an expanding corona and its application to the Whole Sun Month campaign,” J. Geophys. Res. (submitted).
23.
24.
25.
F. Endler, Ph.D. thesis, Gottingen University, 1971.
26.
R. S.
Steinolfson
, S. T.
Suess
, and S. T.
Wu
, Astrophys. J.
255
, 730
(1982
).27.
H.
Washimi
, Y.
Yoshino
, and T.
Ogino
, Geophys. Res. Lett.
14
, 487
(1987
).28.
J. A.
Linker
, G.
Van Hoven
, and D. D.
Schnack
, Geophys. Res. Lett.
17
, 2281
(1990
).29.
A. H.
Wang
, S. T.
Wu
, S. T.
Suess
, and G.
Poletto
, Sol. Phys.
147
, 55
(1993
).30.
D. E. Billings, A Guide to the Solar Corona (Academic, New York, 1966).
31.
K. H.
Schatten
, J. M.
Wilcox
, and N.
Ness
, Sol. Phys.
6
, 442
(1969
).32.
33.
34.
J. T.
Hoeksema
, J. M.
Wilcox
, and P. H.
Scherrer
, J. Geophys. Res.
88
, 9910
(1983
).35.
36.
37.
38.
39.
E. J.
Smith
, M.
Neugebauer
, A.
Balogh
, S. J.
Bame
, G.
Erdos
, R. J.
Forsyth
, B. E.
Goldstein
, J. L.
Philips
, and B.
Tsurutani
, Geophys. Res. Lett.
20
, 2327
(1993
).40.
E. J.
Smith
, R. G.
Marsden
, and D. E.
Page
, Science
268
, 1005
(1995
).41.
A.
Balogh
, E. J.
Smith
, B. T.
Tsurutani
, D. J.
Southwood
, R. J.
Forsyth
, and T. S.
Horbury
, Science
268
, 1007
(1995
).42.
M.
Neugebauer
, R. J.
Forsyth
, A. B.
Galvin
, K. L.
Harvey
, J. T.
Hoeksema
, A. J.
Lazarus
, R. P.
Lepping
, J. A.
Linker
, Z.
Mikić
, J. T.
Steinberg
, R.
von Steiger
, Y.-M.
Wang
, and R.
Wimmer-Schweingruber
, J. Geophys. Res.
103
, 14587
(1998
).43.
S. E. Gibson, D. A. Biesecker, M. Guhathakurta, J. T. Hoeksema, A. J. Lazarus, J. A. Linker, Z. Mikić, Y. Pisanko, J. T. Steinberg, B. J. Thompson, and X. P. Zhao, “The three-dimensional coronal magnetic field during Whole Sun Month,” to appear in Astophys. J.
44.
A. R. Breen, Z. Mikić, J. A. Linker, A. J. Lazarus, B. J. Thompson, P. J. Moran, C. A. Varley, P. J. S. Williams, D. A. Biesecker, and A. Lecinski, “Interplanetary scintillation measurements of the solar wind during Whole Sun Month: Linking coronal and in situ observations,” J. Geophys. Res. (in press).
45.
A. Posner, V. Bothmer, B. J. Thompson, H. Kunow, B. Heber, R. Muller-Mellin, A. J. Lazarus, A. Szabo, Z. Mikić, and J. A. Linker, “In-ecliptic CIR-associated energetic particle events and polar coronal hole structures: SOHO/COSTEP observations for the Whole Sun Month campaign,” J. Geophys. Res. (in press).
46.
M. H.
Acuna
, K. W.
Ogilvie
, D. N.
Baker
, S. A.
Curtis
, D. H.
Fairfield
, and W. H.
Mish
, Space Sci. Rev.
71
, 5
(1995
).47.
Z. Mikić and A. N. McClymont, Solar Active Region Evolution: Comparing Models with Observations, edited by K. S. Balasubramaniam and G. W. Simon (Astronomical Society of the Pacific, 1994), Conf. Ser. Vol. 68, p. 225.
48.
This simulation took 65 h of CPU time on a single processor of the Cray-T90 supercomputer. A real-time solution would take about 10 times longer. It may be possible to perform a real-time simulation once our code is ported to a massively parallel computer.
49.
50.
S. R.
Habbal
, R.
Esser
, M.
Guhathakurta
, and R. R.
Fisher
, Geophys. Res. Lett.
22
, 1465
(1995
).51.
R.
Rosner
, W. H.
Tucker
, and G. S.
Vaiana
, Astrophys. J.
220
, 643
(1978
).52.
53.
This content is only available via PDF.
© 1999 American Institute of Physics.
1999
American Institute of Physics
You do not currently have access to this content.
