The mechanism of wave dissipation in different layers of the sun, as well as the solar granules inter-Network Bright Points and interNetwork Bright Points of chromosphoric solar granules, have been explored in this article. This article's data come from the Interface Region Imaging Spectrograph (IRIS). IRIS is a small exploration mission by NASA. That obtains spectra in near-ultraviolet (NUV), far-ultraviolet 1 (FUV1), and far-ultraviolet 2 (FUV2), from 1332 to 2834 . Slit jaw images (SJIs) of IRIS, using various filters that can provide images centered on the Mg II h wing, Mg II k, Si IV 1403 , and C ii lines. To begin, Bright Points in the chromosphere are selected for this goal. These Points were first chosen using IRIS Slit Jaw Images (SJI) Si IV 1403 . The time slices of the Doppler velocity of the Mg II k spectrum are then drawn at a specified velocity (+/- 20 km/s) and were fed into the wavelet transform function to perform the time-frequency analysis to obtain the oscillation periods of the Doppler velocity. The wavelet transform used for this purpose is Morlet 5 wavelet. The velocity oscillation period data are utilized to determine the Bright Points of the Network and interNetwork solar granules at the chromosphere. The Doppler shift diagram for the Si IV 1394 spectral line is then displayed in time. This graph is a Doppler shift various time graph with attenuation that is caused by wave loss in the solar layers. According to the obtained data, the Network and interNetwork Bright Points, the chromospheric solar granules have an attenuation time 3 to 5 min. The oscillations of the solar granules Network Bright Points are damped more intensely than the solar granules inter-Network Bright Points, and hence their damping lifetime is shorter. Si IV 1394  Doppler velocity shift of Bright Points placed in the solar granules inter-Network is dampened by a lower slope and so has a longer damping life time. Sadeghi and Tavabi researched about the kinetic energy above the Bright Points of the Network and interNetwork regions of the solar granules in a part of a paper titled "A new approach to kinetic energy flux at the different frequencies above the IRIS Bright Points" in 2022. They claim that a substantial percentage of the energy of the Network Bright Points of solar granules is transferred to higher layers, namely the transition region corona, in the Network Bright Points of solar granules. These findings are congruent with the findings of the current study. The oscillations in these locations are dampened for a brief period of time, and the energy is transmitted to higher layers with little loss. Furthermore, it is stated in the cited paper that the majority of the energy at the interNetwork Bright Points of the solar granules does not transfer to higher layers of Sun. This suggests that the energy loss from Bright Points in the solar granules' interNetwork region is rather high in the chromospheric layer. The time period of the wave damping is longer than the length of the damping time in the oscillations, according to the current study on the mechanism of wave dissipation in different layers of the sun and the Network and interNetwork Bright Points of the chromosphere. It has also been demonstrated that the time period of the wave damping is greater than the length of the damping time in the oscillations of the Bright Points of the granules' Network region, which is the source of the most energy loss in this layer.

The solar corona has a temperature equivalent to one million degrees Kelvin. The very high temperature of this region indicates that this region is heated to this extent by a source other than the heat emitted from the photosphere. It is thought that the energy required to heat the solar corona is provided by the very turbulent flows of the convection layer located below the photosphere, which is proposed to explain how the two types of mechanisms are different. The first mechanism includes wave heating and describes the formation of sound waves, gravity waves and magnetic hydrodynamic waves due to the presence of turbulent and turbulent currents. After being produced, these waves go up and when they hit the solar corona, they disintegrate and release energy in the form of thermal energy. The second mechanism includes magnetic heating, in which magnetic energy is continuously created by the currents in the photosphere and is released towards magnetic regions and sunspots in the form of flares and huge solar flares. In this research, using the time series taken by the IRIS telescope, different regions of the solar disk in 4 filters C II, Si IV, Mg II h and k (1330, 1400, 2796 and 2832 Å) are investigated. The morphology and displacement of magnetic Bright Points can be described as convective turbulence caused by super-granular flows from the center to the edge. The purpose of this research is to find out the fluctuating morphology of the Bright Points in the border regions of the Network and inside the Network. The intensity-time graphs clearly show the coherence of the fluctuations, which is because of the common origin of these fluctuations, which are created with similar periods. Also, the wavelet analysis of intensity fluctuations showed that the frequency of fluctuations is from 2.5 to 12 minutes. Also, to investigate the wave propagation in these layers, the correlation between the chromosphere and the transition region was investigated. Due to the difference in the height of the chromosphere layer and the transition region, and the time delay obtained from the intensity fluctuations between the two mentioned layers, the wave speed was determined with an approximate value of 150 km  s-1. Examining the captured images shows that their source lies in the Bright Points of the chromosphere. Many jets reach a temperature of at least 105 K and form an important part of the transition region structure. They are likely an intermittent but continuous source of mass and energy for the solar wind.

A distinct difference is seen between different parts of the solar  chromosphere, including the Bright Points (BPs) at the boundary and within the Network, and the darker regions formed the interior of the granules. In the photosphere, apart from sunspots and holes, there are direct and concentrated magnetic fields in the form of small flux tubes with fields of 1 to 2 kG. Chromospheric Networks are highly dynamic regions with fine structures embedded in the magnetic flux. These structures are located inside the cell Network and there are also many small and dark cells around it. BPs can be thought of as trails of spicules through which mass and energy from the lower layers of the Sun are transported to the corona as the solar wind. Although in the last two decades, despite high-resolution observations and theoretical advances, effective steps have been taken to determine dynamics of BPs and various thermodynamic parameters such as temperature and density, but the mechanisms responsible for their formation are still unknown. These ambiguities are due to the difference in their appearance as a result of observation at different spectral lines and wavelengths. In terms of their dimensions, lifetimes and physical conditions, there is indirect evidence that there is a relationship between the identity of spicules and BPs of the chromospheric Network, which can be attributed to the position of the magnetic field around the Points. BPs form smaller or larger groups that, due to their specific morphology, carry plasma flux tubes to the magnetic corona. The flow behavior along BPs and spikes is a debatable issue. However, observations of the contents of the sticks show periodic up and down movements. In this research, using images of the solar disc extracted by the IRIS space telescope, we investigate the periodic behavior of fast Brightening on a small scale. By analyzing the movements of these Points using the wavelet method, one can understand their periodicity. Examining these Points in wavelengths of 1400, 1330, 2796 Å to the real identity and the effect of these Points on the reactions obtained by the sun. The Bright Points of the grid are arranged for the light grains visible in the filters and in the roughly cellular designs that form the boundaries of the grid. According to the graphs of wavelet analysis, the three-minute peaks are quite clear. The 3-minute and 5-minute chromospheric peaks seen in these analyzes show that the considered Bright Points are P modes, which means compression mode. In the three-minute oscillations, the origin is chromospheric, and in the five-minute oscillations, the origin is photosphere. Origin of the p modes is (5-minute fluctuations) compressive forces. Spectral images were used to obtain Doppler velocities and these velocities were calculated as -20  to 30 km-1. The results of this study suggested that these Bright Points are short-lived sources of plasma that originate from the chromosphere or the lower atmosphere of the Sun.

In this study, researchers investigated the properties of oscillated and non-oscillated Bright Points (BPs) in different regions of the Sun, including active regions (ARs) and coronal holes (CHs). The findings revealed both differences and similarities among these BPs across the various regions. Firstly, the study observed that interNetwork BPs in ARs exhibited higher damping times compared to Network BPs. Additionally, interNetwork BPs in ARs displayed wider ranges of maximum Doppler velocities in comparison to Network BPs. Although both forms of BPs had comparable damping times, interNetwork BPs demonstrated greater maximum Doppler velocities than Network BPs. Moreover, the study provided insights into the damping behavior of BPs in different regions. Specifically, it was noted that the majority of Network BPs in ARs exhibited overdamping, indicating that the damping effects were dominant. On the other hand, in CHs, interNetwork BPs displayed overdamping behavior, suggesting a similar dominance of damping effects. In contrast, oscillated Network BPs in CHs exhibited critical damping behavior, implying a balance between damping and driving forces. It is important to emphasize that the physical principles underlying BP damping may vary depending on the local plasma conditions and magnetic surroundings. Overall, this study highlights the diverse characteristics of BPs in different solar regions, shedding light on their damping times, maximum Doppler velocities, and damping behaviors. These findings contribute to our understanding of the intricate dynamics and plasma conditions occurring in different areas of the Sun, providing valuable insights into the complex nature of solar phenomena.

In this paper, a spectral approach to the origin and propagation of magnetoacoustic oscillations in the Network and interNetwork areas of solar granules is performed. The data used in this study are mostly from Interface Region Imaging Spectrometer (IRIS). Slit Jaw Images (SJIs) data of IRIS at wavelengths of 1400 angstroms related to Si IV and 2796 angstroms related to Mg II h / k and 2832 angstroms related to Mg II w s, are used to select Network and interNetwork areas. The data of the Mg II k spectrum with a wavelength of 2796 angstroms and a temperature of 10, 000 Kelvin have been used to construct the temporal profile of the intensity at the peaks of h3, k3, h2r, h2v, k2r and k2v, and the prospective profile of intensity temperature. One of the common methods for temporal and frequential characteristics analysis is the use of wavelet analysis. This method seems to be a practical method due to the variety and flexibility of wavelet types for different types of analysis. Wavelets and their convolution with waves lead to the extraction of time, frequency and power data. It should be noted that due to the uncertainty principle, resolution of time and frequency interact and its need to select optimum limit of the time and frequency resolution. One of the reasons for choosing Morlet Wavelet for the analysis of this study is the lack of a sharp edge, which reduces the ripple and improves the accuracy of detect the fluctuations properties. Another and one of the most important reasons for using the Morlet wavelet is that it does not change the temporal resolution of the wave. For these reasons, Morlett 5 was the most sensible and reliable choice for high-temporal and frequency-specific results for this study. Using wavelet analysis, the oscillation characteristics of the intensity are obtained in the Network areas and interNetwork areas. By Investigation of the intensity profiles in h and k peaks, it was found that the general behavior in them was the same and the only difference was in the intensities of these peaks and therefore their temperatures. In the case of intensity temperature profiles, the general behavior for intensity temperature profiles extracted from h and k peaks, also seems to be the same. By investigation of the wavelet analysis results, it appears that the oscillating behavior at the h and k peaks is almost similar. Using the results of wavelet analysis, in this study, the periods of oscillations in the intensities of Bright Points in the Network and interNetwork have been obtained. According to their values, it seems that the Bright Points of the interNetwork have a photospheric origin and the Bright Points of the Network have a chromospheric origin. Another result of the wavelet analysis of this study was the intensity of oscillations with a period of about 64 seconds. This high frequency differs from the solar researchers’ observations of photosphere and chromosphere oscillations, so it cannot be related to those oscillations. It seems that this is the first time that this type of high frequency oscillations has been reported. It seems that these high frequency oscillations can play an important role in heating the TR. For this reason, Accurate study of these high frequency oscillations is necessary to understand the causes and heating mechanisms of TR. These high frequency oscillations have been seen in almost all data and areas under study, so far there is no strong evidence of the origin and cause of these high frequency oscillations, and we hope that with more detailed and extensive studies we can better understand the properties and reason of these oscillations.

Our knowledge about the origin and transformation mechanisms of the Bright Points in the solar Network has a significant role in understanding the ejection of materials and the transfer of energy into the solar corona. Outside the active region of the Sun (AR), although it is called the Quiet Sun (QS), various types of small-scale Bright phenomena constantly occur within the boundary of the super granular cells above the magnetic Network. Knowing the Bright Points is an effective key in considering the solar spicules. In this research, we study the solar transition region Bright Points and examine their apparent velocities with the local correlation tracking Fourier (FLCT) method. The results illustrate that these Points differ in apparent velocity direction and Brightness. Their lifetime and average horizontal velocity were estimated at 100 s and 4 kms-1, respectively. Recently, a new group of solar spicules has been observed, those lifetimes are around 100 s, and show a typical horizontal velocity of 3-4 kms-1. According to the analysis of the two-dimensional, apparent velocity of the Bright Points on the rosettes of the Network, these Points can be the disk counterpart of the type II spicules. In addition, the analysis of the two-dimensional field of velocities shows rotations that can cause the excitation of Alfvenic pulses.

The Sun is a magnetically active star. It has a powerful magnetic field that shifts slightly from year to year until it reverses about every eleven years. The sun's magnetic field has many effects, the collection of which is called solar activity such as, sunspots, solar flares, and coronal mass ejections(CMEs). Currently, it is only possible to predict a magnetic storm 30 to 60 minutes before it occurs, which is a very short time. Solar flares and CMEs, massive eruptions of superheated plasma, are the two most energetic phenomenon which impulsively ejected and accelerated by releasing magnetic energy in the solar corona. Heliosphere, space weather, and the Earth are affected from transporting coronal plasma. Following the occurrence of these phenomenon in the Sun, the solar wind blows with greater speed and intensity and sends energetic charged particles into the space of the solar system. When these particles reach the Earth, their radiating electromagnetic waves interact with magnetic field of the Earth. Then various effects are observed, as shock waves and massive geomagnetic storms that disrupt satellites and power grids. Today, using the advancements of ground and space technology, the solar surface can be easily observed. Therefore, observation and prediction of solar storm will be possible more than in the past. In this paper, we review papers intended to collect comprehensive information about what has already been researched about fast solar jets and CMEs made by ground and space instruments over the last decades.