TY - CHAP
T1 - Ensemble and time averages
T2 - The missing diamagnetic effect
AU - Steinitz, R.
PY - 2002/1/1
Y1 - 2002/1/1
N2 - We address three features related to magnetic structures at the Solar suface: "Cool" sunspots, "Hot" corona and "Very High Speed" solar wind. We argue that the diamagnetic effect has been neglected in modelling the thermal and dynamic properties of these features. This omission is due to the difference between time averages and ensemble averages, for plasmas imbedded in diverging magnetic field structures. Gravity, combined with the correct time averages, yield speed filters; these provide cooling of spots, heating the corona and can accelerate the solar wind to high speeds. Thus, all three features can be understood in terms of one single mechanism, the diamagnetic effect.
AB - We address three features related to magnetic structures at the Solar suface: "Cool" sunspots, "Hot" corona and "Very High Speed" solar wind. We argue that the diamagnetic effect has been neglected in modelling the thermal and dynamic properties of these features. This omission is due to the difference between time averages and ensemble averages, for plasmas imbedded in diverging magnetic field structures. Gravity, combined with the correct time averages, yield speed filters; these provide cooling of spots, heating the corona and can accelerate the solar wind to high speeds. Thus, all three features can be understood in terms of one single mechanism, the diamagnetic effect.
UR - http://www.scopus.com/inward/record.url?scp=77957048408&partnerID=8YFLogxK
U2 - 10.1016/S0964-2749(02)80161-5
DO - 10.1016/S0964-2749(02)80161-5
M3 - Chapter
AN - SCOPUS:77957048408
T3 - COSPAR Colloquia Series
SP - 233
EP - 237
BT - COSPAR Colloquia Series
PB - Elsevier Masson SAS
ER -