POLAR investigation of the Sun—POLARIS

The POLAR Investigation of the Sun (POLARIS) mission uses a combination of a gravity assist and solar sail propulsion to place a spacecraft in a 0.48 AU circular orbit around the Sun with an inclination of 75° with respect to solar equator. This challenging orbit is made possible by the challenging development of solar sail propulsion. This first extended view of the high-latitude regions of the Sun will enable crucial observations not possible from the ecliptic viewpoint or from Solar Orbiter. While Solar Orbiter would give the first glimpse of the high latitude magnetic field and flows to probe the solar dynamo, it does not have sufficient viewing of the polar regions to achieve POLARIS’s primary objective: determining the relation between the magnetism and dynamics of the Sun’s polar regions and the solar cycle.

[1]  P. Riley,et al.  Abundance Variation at the Vicinity of an Active Region and the Coronal Origin of the Slow Solar Wind , 2006 .

[2]  G. G. Stokes "J." , 1890, The New Yale Book of Quotations.

[3]  T. Sanderson,et al.  Delay in solar energetic particle onsets at high heliographic latitudes , 2003 .

[4]  P. Liewer,et al.  Characteristics of active-region sources of solar wind near solar maximum , 2004 .

[5]  Claus Fröhlich,et al.  Solar radiative output and its variability: evidence and mechanisms , 2004 .

[6]  J. Geiss Processes Affecting Abundances in the Solar Wind , 1982 .

[7]  Colin R. McInnes,et al.  Solar Polar Orbiter: A Solar Sail Technology Reference Study , 2006 .

[8]  Juri Toomre,et al.  Evolving Submerged Meridional Circulation Cells within the Upper Convection Zone Revealed by Ring-Diagram Analysis , 2002 .

[9]  David Murphy,et al.  Scalable Solar Sail Subsystem Design Considerations , 2002 .

[10]  Edward J. Smith,et al.  Sources of the solar wind at solar activity maximum , 2002 .

[11]  Donald E. Billings,et al.  A Guide to the Solar Corona , 2013 .

[12]  Space Science Reviews , 1962, Nature.

[13]  A. Kosovichev,et al.  Torsional Oscillation, Meridional Flows, and Vorticity Inferred in the Upper Convection Zone of the Sun by Time-Distance Helioseismology , 2004 .

[14]  Jeffrey R. Hall,et al.  Determination of three‐dimensional structure of coronal streamers and relationship to the solar magnetic field , 2001 .

[15]  C. J. Wolfson,et al.  The Solar Oscillations Investigation - Michelson Doppler Imager , 1995 .

[16]  Mason,et al.  Solar wind outflow and the chromospheric magnetic network , 1999, Science.

[17]  David A. Gell,et al.  The High-Resolution Doppler Imager: status update 12 years after launch , 2003, SPIE Optics + Photonics.

[18]  Xianping Zhao,et al.  On formation of sigmoidal structure in active region AR 8100. , 2000 .

[19]  C. Russell,et al.  IMPACT: Science goals and firsts with STEREO , 2005 .

[20]  P. Lamy,et al.  Origin and Evolution of Coronal Streamer Structure During the 1996 Minimum Activity Phase , 1997 .

[21]  Ericka Stricklin-Parker,et al.  Ann , 2005 .

[22]  T. Duvall,et al.  Time-Distance Inversion Methods and Results – (Invited Review) , 2000 .

[23]  C. Schrijver,et al.  Photospheric and heliospheric magnetic fields , 2003 .

[24]  B. Fleck,et al.  Connecting Sun and Heliosphere (Solar Wind 11 / SOHO 16) , 2005 .

[25]  Steven Tomczyk,et al.  An instrument to observe low-degree solar oscillations , 1995 .

[26]  J. M. Herreros,et al.  Global Oscillations at Low Frequency from the SOHO mission (GOLF) , 1995 .