Applications Of Solar Eruption Theory And Model To Studies In High-energy Astrophysics

Coronal mass ejection(CME) is a phenomenon of solar eruption, it causes theflux rope and magnetized plasma to be thrusted outward. In this process, hugemagnetic energy is rapidly released and converted to other forms of energy. It isbelieved that catastrophe and magnetic reconnection trigger the CME. Becausethe sun is closest to the earth and play an important role in human life, the solarphysics has further development.In the feld of high energy astrophysics, there are some physical phenomenahave the operation of a common physical mechanism with solar CME (e.g. mag-netar giant flares and episodic jets from black hole and accretion disk systems).Huge magnetic energy is released and plasmoid is ejected from the system in thisprocess, and the details are still unknown. Therefore, applications of the solarcme model to the phenomena in the high-energy astrophysics are very meaning-ful.Giant flares on soft gamma-ray repeaters that are thought to take place onmagnetars release enormous energy in a short time interval. Their power canbe explained by catastrophic instabilities occurring in the magnetic feld confg-uration and the subsequent magnetic reconnection. By analogy with the coronalmass ejection (CME) events on the Sun, we develop a theoretical model via ananalytic approach for magnetar giant flares. In this model, the rotation and/ordisplacement of the crust causes the feld to twist and deform, leading to fluxrope formation in the magnetosphere and energy accumulation in the relatedconfguration. When the energy and helicity stored in the confguration reacha threshold, the system loses its equilibrium, the flux rope is ejected outwardin a catastrophic way, and magnetic reconnection helps the catastrophe developto a plausible eruption. By taking SGR1806-20as an example, we calculatethe free magnetic energy released in such an eruptive process and fnd that it ismore than1047ergs, which is enough to power a giant flare. The released freemagnetic energy is converted into radiative energy, kinetic energy and gravita- tional energy of the flux rope. We calculated the light curves of the eruptiveprocesses for the giant flares of SGR1806-20, SGR0526-66and SGR1900+14,and compared them with the observational data. The calculated light curves arein good agreement with the observed light curves of giant flares.In many astrophysical black hole systems, episodic jets of plasma blobs havebeen observed, although the origin of the episodic ejection of blobs is unclear.Base on the model proposed by Yuan et al., we develop an magnetohydrodynam-ical model for episodic ejections of the plasma blob from black hole and accretiondisk systems, considering the relativistic efect. By taking Sgr A*and the stellarsize black hole for examples, we study the dynamics of the plasma blob. Ourmodel results show that the blobs can attain large Lorentz factor quickly andundergo expansion after thrusting outward. And we further study the collisionbetween two consecutive ejections in our model, and fnd the consecutive plasmablobs from the stellar size black hole can collide with each other and each ofthem has magnetic energy of more than1050erg in our calculation. In the thiscollision, about half the magnetic energy is released by magnetic reconnection,so multiple collisions among several such blobs can power a Gamma-ray burst.