Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-23T14:29:04.283Z Has data issue: false hasContentIssue false
  • English
  • Français

Small-scale flux emergence events observed by Sunrise/IMaX

Published online by Cambridge University Press:  08 June 2011

S. L. Guglielmino ,
V. Martínez Pillet ,
J. C. del Toro Iniesta ,
L. R. Bellot Rubio ,
F. Zuccarello  and
S. K. Solanki
S. L. Guglielmino
Affiliation:
IAC Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, E-38200, Spain email: [email protected] ULL Departamento de Astrofísica, Univ. de La Laguna, La Laguna, Tenerife, E-38205, Spain
V. Martínez Pillet
Affiliation:
IAC Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, E-38200, Spain email: [email protected]
J. C. del Toro Iniesta
Affiliation:
IAA Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, Granada, E-18080, Spain
L. R. Bellot Rubio
Affiliation:
IAA Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, Granada, E-18080, Spain
F. Zuccarello
Affiliation:
Dipartimento di Fisica e Astronomia - Sezione Astrofisica, Via S. Sofia 78, 95123 Catania, Italy
S. K. Solanki
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany School of Space Research, Kyung Hee University, Yongin, Gyeonggi 446-701, Republic of Korea
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Thanks to the unprecedented combination of high spatial resolution (0″.2) and high temporal cadence (33 s) spectropolarimetric measurements, the IMaX magnetograph aboard the Sunrise balloon-borne telescope is revealing new insights about the plasma dynamics of the all-pervasive small-scale flux concentrations in the quiet Sun. We present the result of a case study concerning the appearance of a bipole, with a size of about 4″ and a flux content of 5 × 1017 Mx, with strong signal of horizontal fields during the emergence. We analyze the data set using the SIR inversion code and obtain indications about the three-dimensional shape of the bipole and its evolution with time.

Keywords

Sun: photosphereSun: magnetic fieldsSun: activityTechniques: high angular resolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 140 - 142
Copyright
Copyright © International Astronomical Union 2011

References

Barthol, P., et al. . 2010, Solar Phys., in pressGoogle Scholar
Danilovic, S., et al. . 2010, Astrophys. Jour. Lett., 723, L149CrossRefGoogle Scholar
Hagenaar, H. J., 2001, Astrophys. Jour., 555, 448CrossRefGoogle Scholar
Martnez Pillet, V., et al. . 2010, Solar Phys., in pressGoogle Scholar
Ruiz Cobo, B. & del Toro Iniesta, J.C. 1992, Astrophys. Jour., 398, 375CrossRefGoogle Scholar
Solanki, S. K., et al. . 2010, Astrophys. Jour. Lett., 723, L127CrossRefGoogle Scholar