arXiv:1706.02367v1 [physics.gen-ph] 2 Jun 2017 ∗ ae ns(o xml,MS n0.721 n 50.06;btt but 15.01.2016); and 02.07.2015 lines, on chromospheric and MLSO C2 the example, as such (for coronographs, ones dista spaceborne based some by asso at pictures typically outburst the are the in seen of flares kernel and a subs prominences surrounding pictures structures, of shown their have ejections from lines coronal as chromospheric The well the as in quality, structure t and outburst increased launching contrast considerably However, their [5] atmosphere outbursts, light. the scattered beyond of SMM) a amount (OSO-7, from rare considerable very only were the observed w coronographs were of problem ground-based flares by This and outbursts prominences the structure. of characteristic outbursts their the in uncertainty some more). even ejec t and of then km/s speed 2000 Earth, the to bot the (up usual, associated to greater As be substantially direction can are flares. the phenomena the in These and ejected filaments/prominences develop. wh is can processes, cloud aurorae physical in the and some the to into If base due coronal mag km/s the studied. the 400–900 from of ejected about cloud is velocity A tones a billion 3]. few [2, a weather of space mass the determine which system, -al [email protected] E-mail: pr rmteisffiinl la ehns faclrto fteo the of acceleration of mechanism clear insufficiently the from Apart p energetic the of one are (CME) ejections mass coronal The ewrs ooa asEetos atceAclrto;X-Ray Acceleration; Particle Ejections; Fields Mass Electric Coronal acceler the Keywords: of motion directed fields. The magnetic excessiv accelerate the acting. the field electric is by resulting radiation produced The hard be effect. to Compton the seems m to ejection outer, the The of considered. are envelope continuum coronal the and lines trbr srnmclIsiue(AS) oooo Moscow Lomonosov (GAISh), Institute Astronomical Sternberg Abstract. M tutr n atceAcceleration Particle and Structure CME .SRCUEADDNMC FCME OF DYNAMICS AND STRUCTURE 2. h ieecso h jciniaesrcue ntechrom the in structures ejection-image the of differences The nvriesi rs.1,Mso,199 Russia 119992 Moscow, 13, prosp. Universitetskii e.g. amrlnso yrgno ie fnurlo oie helium. ionized or neutral of lines or hydrogen of lines Balmer , .INTRODUCTION 1. grF Nikulin F. Igor c Fgr ) uhlosare loops Such 1). (Figure nce dhdalwqaiy because quality, low a had nd r iuiescattering diffusive ore h atce hl the while particles the tdprilsinduces particles ated 3SH,adteground- the and SOHO, C3 ntecrnlcontinuum. coronal the in uss antcand Magnetic Bursts; reeetosdue electrons free e ata ieecso the of differences tantial itdwt h loop–arc the with ciated ini h aeo flares of case the in tion c r tl insufficiently still are ich h at.Dtcinof Detection Earth. the enme fobservable of number he ihteotussof outbursts the with h tt University, State epaeaysaewith space terplanetary h oa coronographs the eoeai h Solar the in henomena ∗ suntcal when unnoticeable as eie lsawt a with plasma netized e r o iil in visible not are hey emgei storms magnetic he tuss hr is there utbursts, ospheric 2

FIG. 1: Outburst on 27 February 2000 with a well-developed envelope and dense kernel in the middle (SOHO LASCO C3).

These loops are sometimes diffuse and sometimes are composed of a few separated layers, but most often they possess a weakly filamentary structure. Such loops are commonly interpreted as the magnetic ones, i.e., connecting the opposite magnetic regions in the region of outburst. However, this is usually not confirmed by the detailed comparison with magnetograms. Moreover, the magnetic loops are not always located perpendicularly to the line of sight and, consequently, should usually represent the elongated eclipses (up to the stretching into a straight line). Since this is usually not observed, one should assume that the outburst is actually surrounded by a dynamic envelope, li