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Solar Physics and the Solar-Stellar Connection at Dome C

Published online by Cambridge University Press:  13 November 2008

H. Zinnecker ,
N. Epchtein ,
H. Rauer ,
C. Denker  and
K.G. Strassmeier
C. Denker
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
K.G. Strassmeier
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
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Abstract

Solar magnetic fields evolve on many time-scales, e.g., the generation, migration, and dissipation of magnetic flux during the 22-year magnetic cycle of the Sun. Active regions develop and decay over periods of weeks. The build-up of magnetic shear in active regions can occur within less than a day. At the shortest time-scales, the magnetic field topology can change rapidly within a few minutes as the result of eruptive events such as flares, filament eruptions, and coronal mass ejections. The unique daytime seeing characteristics at Dome C, i.e., continuous periods of very good to excellent seeing during almost the entire Antarctic summer, allow us to address many of the top science cases related to the evolution of solar magnetic fields. We introduce the Advanced Solar Photometric Imager and Radiation Experiment and present the science cases for synoptic solar observations at Dome C. Furthermore, common science cases concerning the solar-stellar connection are discussed in the context of the proposed International Concordia Explorer Telescope.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 33: 2nd ARENA Conference: The Astrophysical Science Cases at Dome C , 2008 , pp. 97 - 104
Copyright
© EAS, EDP Sciences, 2008

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References

Andersen, D.R., et al., 2006, PASP, 118, 1574 CrossRef
Aristidi, E., et al., 2005, A&A, 444, 651
Cayrel de Strobel, G., 1996, A&AR, 7, 243
Coulter, R.L., & Kuhn, J.R., 1994, ASP Conf. Ser., 68, 37
Denker, C., et al., 2006, Proc. SPIE, 6267, 62670A CrossRef
Dupree, A.K., 2003, in The Future of Cool-Star Astrophysics, ed. A. Brown, G.M. Harper, & T.R. Ayres (University of Colorado), p. 1–13
Fröhlich, C., & Lean, J., 2004, ARA&A, 12, 273
Harvey, J.W., et al., 1996, Science, 533, 163
Hill, F., et al., 2004, ATST Site Survey Working Group Final Report (http://atst.nso.edu/site/reports/RPT-0021.pdf)
Keller, C.U., Harvey, J.W., & Giampapa, M.S., 2003, Proc. SPIE, 4853, 194 CrossRef
Kenyon, S.L., & Storey, J.W.V., 2006, PASP, 118, 489 CrossRef
Kosovichev, A.G., et al., 2007, Astron. Nachr., 328, 339 CrossRef
Kosugi, T., et al., 2007, Sol. Phys., 243, 3 CrossRef
Lawrence, J.S., et al., 2004, Nature, 431, 278 CrossRef
Lean, J., 1997, ARA&A, 35, 33 CrossRef
Nandy, D., & Martens, P.C.H., 2007, Adv. Space Res., 40, 891 CrossRef
Neidig, D., et al., 1998, ASP Conf. Ser., 140, 519
November, L.J., & Simon, G.W., 1988, ApJ, 333, 427 CrossRef
Rimmele, T.R., 2000, Proc. SPIE, 4007, 218 CrossRef
Roudier, T., et al., 1999, A&A, 349, 301
Sarazin, M., & Roddier, F., 1990, A&A, 227, 294
Strassmeier, K.G., 2005, Astron. Nachr., 326, 269 CrossRef
Strassmeier, K.G., et al., 2007, ASP Conf. Ser., 366, 332
Strassmeier, K.G., et al., 2008, EAS Publ. Ser. 33, 199
Tokovinin, A., 2004, PASP, 116, 941 CrossRef
Tomczyk, S., Lin, H., & Zurbuchen, T., 2007, NSF Proposal (http://www.cosmo.ucar.edu/publications/Prospectus.pdf)
van Noort, M., Rouppe van der Voort, L., & Löfdahl, M.G., 2005, Sol. Phys., 228, 191 CrossRef
Volkmer, R., et al., 2006, Proc. SPIE, 6267, 62670W CrossRef
Wagner, J., et al., 2006, Proc. SPIE, 6267, 626709 CrossRef
Yang, G., et al., 2004, ApJ, 617, 151 CrossRef