Slow Solar Wind: Observable Characteristics for Constraining Modelling

Monday, 14 December 2015: 08:36
2011 (Moscone West)
Lucia Abbo1, Leon Ofman2, Spiro K Antiochos3, Viggo H Hansteen4, Louise Harra5, Yuan-Kuen Ko6, Giovanni Lapenta7, Bo Li8, Pete Riley9, Leonard Strachan6, Rudolf von Steiger10 and Y.-M. Wang11, (1)Astrophysical Observatory of Turin, Pino Torinese, Italy, (2)Catholic University of America, Washington, DC, United States, (3)NASA Goddard Space Flight Center, Greenbelt, MD, United States, (4)Institute for Theoretical Astrophysics, Oslo, Norway, (5)University College London, London, United Kingdom, (6)US Naval Research Laboratory, Washington, DC, United States, (7)Katholieke Universiteit Leuven, Leuven, Belgium, (8)Shandong University at Weihai, Weihai, China, (9)Predictive Science Inc., San Diego, CA, United States, (10)International Space Science Institute, Bern, Switzerland, (11)Naval Research Lab DC, Washington, DC, United States
The Slow Solar Wind (SSW) origin is an open issue in the post SOHO era and forms a major objective for planned
future missions such as the Solar Orbiter and Solar Probe Plus.
Results from spacecraft data, combined with theoretical modeling, have helped to investigate many
aspects of the SSW. Fundamental physical properties of the coronal plasma have been derived
from spectroscopic and imaging remote-sensing data and in-situ data, and these results have provided crucial insights for
a deeper understanding of the origin and acceleration of the SSW.
Advances models of the SSW in coronal streamers and other structures have been developed using 3D MHD
and multi-fluid equations.
Nevertheless, there are still debated questions such as:
What are the source regions of SSW? What are their contributions to the SSW?
Which is the role of the magnetic topology in corona for the origin, acceleration and energy deposition of SSW?
Which are the possible acceleration and heating mechanisms for the SSW?
The aim of this study is to present the insights on the SSW origin and formation
arisen during the discussions at the International Space Science Institute (ISSI) by the Team entitled ''Slow
solar wind sources and acceleration mechanisms in the corona'' held in Bern (Switzerland) in March
2014--2015. The attached figure will be presented to summarize the different hypotheses of the SSW formation.