Clone of Solar Physics Research

Evolution of the sigmoid of this active region provides clear evidence that a flux rope formed before the CME occurred and not at its onset. Green & Kliem, Astrophys. J. Letters, 700, L83, 2009.

Lateral expansion of CMEs generates successive reconnections with the environment so increasing the impact zone of the CME. van Driel-Gesztelyi et al., Ann. Geophys., 26, 3077-3088, 2008

 Fieldline reconnection between the legs of magnetic arcades generates or augment flux ropes, highlighted by changes in sigmoid tomography. Tripathi et al., Astrophys. J. Letters, 698, L27-L32, 2009

 Twist stored in the form of helicity in filaments can be converted into writhe as these large structures erupt, resulting in their rotation. Green et al., Solar Physics, 246, 365-391, 2007

Simulations reveal that the acceleration of a CME will be determined by the fall in strength with height of any overlying magnetic field. Torok & Kliem, Astron. Nachr., 328, 743-746, 2007

Rotational direction of waves are consistent with helicity-sense of source active regions, implying magnetic link between wave and CME. Attrill et al., Astrophys. J. Letters, 656, L101-L104, 2007.

Plasma streams away from the solar surface at the edges of active regions and may contibrute a 1/4 of the solar wind's total material. Sakao et al., Science, 318, 1585, 2007

Reconnection at the edges of active regions will produce plamsa jets and chromospheric evaporation, which are both types of outflows. Baker et al., Astrophys. J., submitted, 2009

Outflows at the edges of active regions have low density and radience, which are opposite to similar temperature plasma in the active region. Del Zanna, Astron. & Astrophys., 481, L49-L52, 2008.

Reconnection at the edges of active regions will produce plamsa jets and chromospheric evaporation, which are both types of outflows. Baker et al., Astrophys. J., submitted, 2009

Expanding active regions can compress neighbouring field, generating forces in the latter that can accelerate plasma upwards as outflows. Murray et al., Solar Physics, submitted, 2009

Outflows may rise along funnels of open magnetic field and sink back to the solar surface along the closed loops of the active regions. Marsch, Hui, Sun et al., Astrophys. J., 685, 1262-1269, 2008

Eroneous reversals can be generated in photospheric magnetic data during flares as a result of non-thermal electron acceleration. Zhao, Wang, Matthews et al., Research in Astron. Astrophys., 9, 812-828, 2009

Moat flows are only present at locations around sunspots where the penumbral field is perpendicular to the umbra's border. Vargas Dominguez et al., Astrophys. J., 679, 900, 2008

Significant details of a magnetic field's twist are lost when it emerges through the solar surface, with only weak twist being distinguishable. Murray et al., Astron. & Astrophys., 479, 567-577, 2008

Certain dynamo models can generate magnetic helicity of one sign on large-scales, writhe, and the opposite sign on small scales, twist. Asgari-Targhi & Berger, GAFD, 103, 69-87, 2009

Reconnection between active regions and coronal holes interchanges positions of closed and open field, hence 'interchange' reconnection. Baker et al., Astron. Nachr., 328, 773, 2007

A series of reversals in the input and output fields during reconnection is termed 'oscillatory' and produces periodic heating and swaying jets. Murray et al., Astron. & Astrophys., 494, 329-337, 2009

A single active region can produce CMEs that have oppositely directed magnetic fields when measured near the Earth. Harra et al., Solar Physics, 244, 85-114, 2007

Even the smallest spotless active regions can generate coronal mass ejections (CMEs) that travel out across interplanetary space. Steed et al., Ann. Geophys., 26,3159, 2008.. 

The forces generated in flares can accelerate solar energetic particles along open fieldlines all the way from the Sun out to the Earth. Li et al., Astron. & Astrophys., 503, 1013, 2009