Initiation and Early Evolution of the Coronal Mass Ejection on 2009 May 13 From Extreme-Ultraviolet and White-Light Observations

Breakout Reconnection Observed by the TESIS EUV Telescope

“…During reconnection, plasma inflows from areas surrounding the current sheet increase the currentsheet density. Also, at high altitudes, scattering which depends on density contributes to the emission in the 171 Å line (Reva et al 2014). It is possible that the observed bright stripe is the scattered light in the dense current sheet.…”

“…TESIS included an EUV telescope, which built solar corona images in the Fe 171 Å line with 1.7 ′′ angular resolution and 1 • field of view. For the Fe 171 Å telescope, a special observational program was developed, in which the telescope built images of far corona (for more details, see Reva et al 2014). From April 8 to 10, TESIS worked in the far corona mode with a varying cadence of 10, 20, and 30 minutes.…”

“…Several events showed indirect evidence of the breakout model: quadrupolar magnetic field structure of the Bastille day flare (Aulanier et al 2000); 'EIT crinckles' (Sterling & Moore 2001); dimmings before the CME (Sterling & Moore 2004a); CME quadrupolar magnetic structure inferred from SXT images (Sterling & Moore 2004b); timing of brightenings during CME (Gary & Moore 2004); and prominence location relative to hotter plasma in the CME (Reva et al 2014). Manoharan & Kundu (2003); Aurass et al (2011Aurass et al ( , 2013 reported radio sources above null points of the CME quadrupolar structure before eruption, which the authors interpreted as evidence of breakout reconnection.…”

“…To confirm the breakout model, we need observations in the far corona. Although instruments that could observe far corona existed LASCO/C1 coronograph (Zhang et al 2001), Siberian solar radio telescope (Alissandrakis et al 2013), Mauna Loa Observatory (Bemporad et al 2007), TESIS EUV telescopes (Reva et al 2014), and SWAP EUV telescope (Seaton et al 2013) they were never used to test the breakout model.…”

KORTES Mission for Solar Activity Monitoring Onboard International Space Station

“…The effective focal length of all three telescopes equals to 1,740 mm giving a field of view (FoV) of 0.91 • to enable widefield observations of CME formation and flux-rope eruptions. The main advantage of the KORTES telescopes over other EUV telescopes and coronographs, e.g., LASCO/C2 and C3 (Brueckner et al, 1995) or SDO/AIA (Lemen et al, 2012), is that they may provide valuable observations in the so-called "blind zone"-the gap in solar altitudes between 1.2 and 2 solar radii (Reva et al, 2014(Reva et al, , 2017.…”