Radiative energy from a reconnection region around massive black hole

In the previous numerical study, we find the blob formation and ejection in the presence of magnetic reconnection in the environment of the hot flow of the accretion disc. Based on those encouraging results, in the present work, we calculate the energy and the spectrum of the emission in the different bands around sagittarius A* (Sgr A*). We assume the electrons in the magnetic reconnection region are non-thermal and emit synchrotron radiation. The electrons in the other region are thermal, which follows the thermal distribution, and the thermal electron emission mechanism is thermal synchrotron radiation. During the whole process of the magnetic evolution and reconnection, we find two peaks in the temporal light curve in the recently observed radio frequencies (230 and 43GHz) and near-infrared (NIR) wavelengths (3.8 and 2.2 mu m). Although the light curve of the NIR band is most prominent in a single peak. The first peak appears because of the blob in the plasma flow, which is formed due to the magnetic reconnection. The second peak appears due to the production of the non-thermal electrons with the evolution of the magnetic flux. Both peaks reach luminosity of more than 10(26) erg s(-1) for a single plasmoid/blob. For the NIR band, the highest luminosity can reach more than 10(28) erg s(-1). These luminosities can be high for the large simulation area and the stronger magnetic field with the multiple blobs. We infer that the observed flares are a group of magnetic reconnection phenomena, not a single one.

Automated summary

This study focuses on the formation and ejection of "blobs" due to magnetic reconnection in the hot flow environment of the accretion disc, and calculates the energy and emission spectrum in different bands near Sagittarius A*. The results show that the observed flares in various bands are a series of magnetic reconnection phenomena, rather than a single event.