Shock Wave Induced Solar Flares Associated With Coronal Mass Ejections (Cmes)
| dc.contributor.advisor | Kebede, Legesse W. (PhD) | |
| dc.contributor.author | Belay, Atakalti | |
| dc.date.accessioned | 2019-08-16T08:37:54Z | |
| dc.date.accessioned | 2023-11-09T11:25:50Z | |
| dc.date.available | 2019-08-16T08:37:54Z | |
| dc.date.available | 2023-11-09T11:25:50Z | |
| dc.date.issued | 2018-06-30 | |
| dc.description.abstract | In this work, we have advanced shock wave induced stellar flare model (SWIF model) which describes the nature of energetic events on star, mainly solar atmosphere. The SWIF model, theoretical model, works for energetic events both at weak magnetic field region as well as strong magnetic field region of stellar atmosphere. This advanced physical SWIF model has two parts. The first part of the SWIF model which is independent of pre-existed magnetic field; we named it shock wave induced flare on stellar, solar, quite region (SWIF-1SQR). The SWIF-1SQR model well describes Nano flares and micro flares as well as the impulsive flares theoretically. The second part of the SWIF model includes pre-existed force free magnetic field integrated with fast magnetic reconnection (FMR) theory. Thus, the second part of the SWIF model has been named as shock wave induced flare model on stellar, solar, active region (SWIF-2SAR model). The SWIF-2SAR model profoundly defines the impulsive flares and even small flares with high complexity nature of plasma dynamics. The SWIF model enables us to predict the suddenly releasing of flare energy, formation of coronal mass ejections (CMEs) as well as electromagnetic wave burst from small local region on stellar atmosphere, specifically on the sun. Generally, the SWIF model articulates how flares, CMEs and observable electromagnetic wave burst are created on weak and strong magnetic field region of stellar atmosphere. The minimum electron current limit, which is occurred at small region for formation of flares and CMEs, is approximated by 𝐽𝑒≈𝑒𝑛𝑒𝑐𝑠 that is the sonic electron current while the upper limit is 𝐽𝑒≈103 𝑒𝑛𝑒𝑐𝑠 at solar photosphere. Thus, the SWIF model predicts electron current limits which are responsible for solar flares and CMEs in the range of 𝐽𝑒≈105 𝐴 to 𝐽𝑒≈1012 𝐴 during flare formation. The corresponding electron induced magnetic field which provides flares and CMEs also anticipated as 𝐵≈104 𝐺 to 𝐵≈108 𝐺 in radius of 100 𝑚 collapsing spherical cavity. When this compacted magnetic field is well organized and exploded, a flare associated with CMEs and electromagnetic wave burst is looked. Thus, the SWIF model predicts stellar fares and CMEs that are transpired ubiquitous where plasma flows with velocity greater than background acoustic velocity is noteworthy. On basis of SWIF model advancing, the flare electron runaway current is determined by strength of velocity shock potential (VSP). Here, we investigate that the VSP triggers stellar (solar) explosive events and that can be described by SWIF model, physical model. | en_US |
| dc.identifier.uri | http://10.90.10.223:4000/handle/123456789/18793 | |
| dc.language.iso | en | en_US |
| dc.publisher | Addis Ababa University | en_US |
| dc.subject | Solar Atmosphere | en_US |
| dc.subject | Physical Change of Visible Star | en_US |
| dc.subject | Observational Evidence | en_US |
| dc.subject | Methodology | en_US |
| dc.title | Shock Wave Induced Solar Flares Associated With Coronal Mass Ejections (Cmes) | en_US |
| dc.type | Thesis | en_US |