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\@writefile{toc}{\contentsline {section}{Introduction}{1}{section*.1}}
\@writefile{toc}{\contentsline {section}{MHD Modeling Approach}{1}{section*.2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  Comparison of synoptic magnetograms from four solar observatories for CR 2060. The data have been converted to a radial field, smoothed (by diffusing and filtering the measurements), and, at the highest latitudes, filled, by extrapolating mid-latitude fields poleward. }}{2}{figure.1}}
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\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces  Coronal hole boundaries for a sequence of model solutions at different temperatures for CR 2051. The labels give the plasma temperature in units of $\times 10^6$K. Grey regions represent closed field lines while black indicates field lines that open into the heliosphere. }}{3}{figure.2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  SOHO/EIT observations at 195 \r A\nobreakspace  {}during CR 2051. Panels (a) through (d) differ only in the MHD solution used to produce the computed coronal hole boundaries (red curves). }}{4}{figure.3}}
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\@writefile{toc}{\contentsline {section}{An Application of the Model: Unipolar Streamers}{4}{section*.3}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces  (Left) Model solar wind speed at $30 R_{\odot }$, together with the location of STEREO A (green), B (red), and ACE (Earth, blue). The HCS is shown by the grey curve. The four panels show results from models driven by data from the following observatories: (a) SOLIS; (b) MDI; (c) GONG; and (d) WSO. (Right) Time series of solar wind speed for the 4 model solutions are compared with data from ACE and STEREO A/B. }}{5}{figure.4}}
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\@writefile{toc}{\contentsline {section}{Summary and Discussion}{5}{section*.4}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces  (Top) Selection of meridional slices of $pB$ with field lines superimposed. Field lines colored blue (red) open into the heliosphere and are inward (outward). Field lines colored green are closed.The heliographic latitude of ACE is indicated by the solid black line. (Middle) The photospheric magnetic field used to compute the MHD solution. The boundaries of coronal holes are indicated by the black curve and the trajectory of the ACE spacecraft (from right to left as time increases) is shown by the straight black line. Measurements by ACE are mapped back to their inferred source location via the lines branching off the trajectory, color-coded according to the measured {\it  in-situ} polarity. (Bottom) Solar wind speed measured by ACE, mapped back to $30 R_{\odot }$, and color-coded with the polarity of the field is shown, together with the mapped plasma density as a function of longitude. }}{6}{figure.5}}
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\bibstyle{aipproc}
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\bibcite{phillips09a}{{1}{2009}{{Phillips}}{{}}}
\bibcite{riley01a}{{2}{2001}{{Riley et~al.}}{{}}}
\bibcite{stevens11a}{{3}{2011}{{{Stevens} et~al.}}{{}}}
\bibcite{riley10a}{{4}{2010{}}{{{Riley} et~al.}}{{}}}
\bibcite{riley11a}{{5}{2011{}}{{{Riley} et~al.}}{{}}}
\bibcite{riley11b}{{6}{2011{}}{{{Riley} et~al.}}{{}}}
\bibcite{riley11c}{{7}{2011}{{{Riley} and {Lionello}}}{{}}}
\bibcite{riley10d}{{8}{2010{}}{{{Riley} et~al.}}{{}}}
\bibcite{riley11d}{{9}{2011{}}{{{Riley} et~al.}}{{}}}
\bibcite{mikic99a}{{10}{1999}{{Miki\'c et~al.}}{{}}}
\bibcite{lionello01a}{{11}{2001}{{Lionello et~al.}}{{}}}
\bibcite{riley07b}{{12}{2007}{{Riley}}{{}}}
\bibcite{wang09a}{{13}{2009}{{{Wang} et~al.}}{{}}}
\bibcite{cranmer10a}{{14}{2010}{{Cranmer}}{{}}}
\bibcite{fisk98a}{{15}{1998}{{{Fisk} et~al.}}{{}}}
\bibcite{antiochos11a}{{16}{2011}{{Antiochos et~al.}}{{}}}
\bibcite{riley11e}{{17}{2011}{{{Riley} and {Luhmann}}}{{}}}
\bibcite{neugebauer04a}{{18}{2004}{{{Neugebauer} et~al.}}{{}}}
