The investigation of solar activity is a very important part of space physics because of the significant impact on Earth technological systems. The effective part of solar activity is solar storm which in turn consists of three parts namely The Coronal Mass Ejections (CMEs), Flares and The Solar Energetic Particles (SEPs). The output of X-ray and UV-variation are various with solar cycle and all of these are related to the transients released from large amount of energy from Sun [1] . SEPs are one population of near-Earth particles; they have intermediate energies from some 10 keV/nuclei to the GeV range and occur in events that last from some hour’s to a few days and increase above background by many orders of magnitude. Occasionally eruptions are directed toward the Earth change the conditions of near-Earth space in several ways, including a cut in the electricity power in high latitudes on the Earth and damaged of some satellites [2] . There are two types of SEP, “gradual SEP” and “impulsive SEP”; in this investigation the two types of events have been analyzed specially the high speed events for the peak of solar cycle (24) for years (2012-2015). All observations for this study were taken from Large Angle and Spectroscopic Coronagraph (LASCO), which provide the first ever CMEs database to cover a full solar cycle with a single instrument, thus opening investigations to the solar cycle dependence on CME properties [3] . By using the photometric scale observations of LASCO, so there will be able to find the speed of Coronal Mass Ejections (CMEs), angular width (AW) and the Central Position Angle (CPA), as for finding the intensity-time profile, the energy and the shape of the events which can be obtained from ERNE detectors system. LASCO and ERNE are scientific instruments boarded on SOHO [4] . The main objective of this study is to detect and analyze when and where SEPs take place by finding the location of CMEs and find the time of the events as well as find a statistical description to SEP for the peak of solar cycle (24) for years selected by taking high speed events CMEs with velocities > 1000 (km/s) and angular width > 200 (deg).

Research activity has been related to the observation of big solar eruptions. In big solar events, before the magnetic storm hits the Earth, SEPs bombard Earth earlier, and may be both (storm and particles) come from the eruption which is called CME. Observed eruptions are associated with different composition and energy spectra. So the investigation of their source is very important to learn SEPs [5] . SOHO which placed into the hole orbit close to lagrangian point L1 carries twelve scientific instruments, LASCO & ERNE are some of these devices that data were obtained by them for this study. ERNE provide an opportunity to analyze protons and helium nuclei intensity-time profile with high resolution and LASCO give information about acceleration, CPA, and AW, the speed of CME and their basic attributes which cataloged in a data base known as the SOHO/LASCO catalog Figure 1. The logarithmic intensity-time Profile of SEP associated to CME for the peak of solar cycle (24) for years (2012-2015) were provided by ERNE detectors [6] . From this profile the injection time, speed, width, acceleration, CPA and onset time were estimated. The Injection time (T_inj) representing the time of particles that Injected from the Sun and it gives the acceleration time for the particles [5] :

T_inj = (t₀-t_f) + 8.3 min (1)

Equation (1) gives the observer to set a real time at the detector.

The flight time can be realized by using beta equation, (this cannot be done without finding the ratio velocity of particles to the velocity of light which is called relativistic velocity coefficient (β) [7] .

where v = the speed of particles= s/t_f, c = the speed of light.

(t₀) onset time is observed by the detectors, (8.3 min) have been added to represent the time of light to reach the Earth from the Sun, and the flight time (T_f) given by equation (3):

where (s) is the fixed path length for the particles which equal the distance between the Sun and the detector (=1.2 AU) [8] , and β equal

P is the energy of proton = 938 Mev, E is the proton kinetic energy [9] . The injection time will be compared with the appearing time from LASCO [7] to ensure the accuracy of the events time and energy.

Figure 2 shows SOHO/ERNE detection for four important clear events especially the particular event on 7 March 2012, an SEPs event onset at 00:30 UT, 01:30 proton injection time at (00:11, 01:11) UT for proton energies (63.9 - 80.3) Mev, with CPA of Halo type and linear velocity of (2684, 1825) kms⁻¹. On 13 March 2012, an SEPs event onset at 17:30UT proton injection time at 16:53 UT for proton energies (20.3 - 28) Mev, with CPA of Halo type and linear velocity of 1884 kms⁻¹. On 28 March 2012, an SEPs event onset at 01:30UT proton injection time at 12:48 UT for proton energies (16.9 - 22.4) Mev, CPA of Halo and linear velocity of 1033 kms⁻¹. Five significant events observed from Figure 3, on 13 May 2013, SEPs event onset at 02:30, 15:30 UT proton injection time at 02:11, 15:11 UT for proton energies (63.9 - 80.3) Mev, CPA of Halo type and linear velocity of (1270, 1850) kms⁻¹. On 15 May 2013, SEPs event onset at 01:30 UT proton injection time at 01:11 UT for proton energies (63.9 - 80.3) Mev, CPA of Halo type and linear velocity of 1366 kms⁻¹. On 17 May 2013, SEPs event onset at 10:30 UT proton injection time at 10:11 UT for proton energies (50.8 - 67.4) Mev, CPA of Halo and linear velocity of 1345 kms⁻¹. On 22 May 2013, SEPs event onset at 13:30 UT proton injection time at 13:11 UT for proton energies (63.9 - 80.3) Mev, CPA of Halo and linear velocity of 1466 kms⁻¹. From Figure 4 on 12 December 2013, SOHO/ERNE detected a SEPs event onset at 03:30 UT proton injection time at 02:56 UT for proton energies (20.8 - 28) Mev, with CPA of 214^˚ and linear velocity of 1002 kms⁻¹.

From Figure 5 on 28 December 2013, SOHO/ERNE detected a SEPs event onset at 17:30 UT proton injection time at 17:11 UT for proton energies (63.9 - 80.3) Mev, with central position angle (CPA) of Halo, with a linear velocity of 1118 kms⁻¹.

Figure 6 shows three events on (1, 2, 10) September 2014, SOHO/ERNE detected a SEPs events onset at (22:30, 02:30 and 18:30) UT proton injection time at (22:11, 02:11 and 18:11) UT for proton energies (63.9 - 80.3) Mev, CPA of (Halo, 121^˚ and Halo) and linear velocity of (1404, 1141 and 1267) kms⁻¹.

From Figure 7 on (21-22) June 2015, SOHO/ERNE detected two SEPs events onset at (02:30 and 18:30) UT proton injection time at (02:11 and 18:11) UT for proton energies (63.9 - 80.3) Mev, with central position angle (CPA) of Halo and linear velocity of (1366 and 1209) kms⁻¹.

Table 1 summarizing the handled observations from LASCO and updating of previous investigations, also exhibit the first appearance, CPA, AW, speed, acceleration and the number of associated CME_s which is selected for this study ( the peak of solar cycle 24). Table 2 represents onset time and energy for the clear events by the intensity-time profiles obtained from ERNE for the same observations, the injection time, time of flight (T_f) and β calculation. While the first appearance time taken from LASCO in order to compare it with onset time for the

promotion of the calculations. From Table 2 we find that the onset time and appearance time are convergent. Figure 8 shows that 90% of the events was halo (360˚) central position angle (CPA), North West 1%, South West 4%, North East and South East 2%, and the average speed 1374 (km/s) for the selected observation of this study. Figure 9 shows a scatter plot (using SPSS software vir.19) between the measured acceleration, A (m/s²) and speed, v (km/s) that calculated in Table 1 for the handled observation (82 event) of the CMEs for which the acceleration estimate was possible. Despite the large scatter, acceleration has a probable correlation, where from Table 3 we find the parameter of the regression equation, B_° = 1347.029 and B₁= −0.913, since the principle equation of regression is Y= B_° ± B₁X that is mean (A= 1347.029 − 0.913v) or A= −0.913 (v-1475.388). And as shown in Figure 9 and Table 3 that the correlation coefficient is a negative value and its absolute value less than 0.5 (0.122), this shows inverse relationship between speed and acceleration in this region of solar cycle (24) i.e. the peak. So the CMEs (v < 1475.388 km/s) accelerate, and CMEs (v ~ 1475.388 km/s) have no realized acceleration and for CMEs (v > 1475.388 km/s) decelerate. Close to the Sun “A” is determined by the driving force and if A = 0 then v = 1475.388 km/s. From Figure 10 we note that the “Average” and “Median” almost

compatible and statistically this refers to accurate chose of the observations for the peak of solar cycle (24), and also from Figure 10 we note the existence of two peaks for the speed, the first peak in the year 2012 and the other in the year 2014, this corresponds that solar cycle (24) have double peaks [11] , as well as the behavior of the curves in Figure 10 and Figure 11 verified the approaches of Figure 9, that acceleration inversely proportional to the speed as mentioned before. From Figure 12 we note that 39% of total events are gradual and 29% are impulsive, the remaining is 32% are not clear events.

In this study the data analysis of the present work leads us to conclude the following:

1) The number of events for the peak of solar cycle (24) (2012-2015) which verifies the required conditions was 82 event, and this was from SOHO/LASCO CME Catalog [7] and ERNE.

2) The filtered events from 82 events as described in paragraph 2, were 16 events for the peak of solar cycle (24) which were verified by ERNE from the logarithmic intensity-time profile of these events.

3) It turns out that from these 82 events, 90% of the events were halo (360˚) central position angle (CPA), North West 1%, South West 4%, North East and South East 2%, as well as for associated SEP found that 39%

of gradual events and 29% of impulsive events while 32% were not clear events.

4) All results obtained in (Table 1 and Table 2) and (Figures 2-7) were hired for the purpose of statistical characteristics of SEP solar events for the peak of solar cycle (24), and we note that the onset time and appearance time almost identical and this shows the accuracy of analysis.

5) The results of injection time show that the bulk of the particle acceleration occurs during the impulsive phase of the events near the Sun.

6) The logarithmic intensity-time profile of gradual SEP shows events of temporal and spatial behavior depending on factors such as spacecraft position with respect to the CME.

7) From statistical analysis of speed and acceleration of 82 events for the whole peak of solar cycle (24) we found that the acceleration inversely proportional to speed and the relationship between them is not relevant, because the absolute value of the correlation coefficient between acceleration and speed is less than 0.5 (R = −0.122). So the CMEs (v < 1475.388 km/s) accelerate, and CMEs (v~1475.388 km/s) have no realized acceleration and for CMEs (v > 1475.388 km/s) decelerate.

8) We note that the speed increases in two region in the year 2012 and in the year 2014 and this is confirmed by the convergence of median and average, and this confirms that the peak of solar cycle (24) really is double peak [12] [13] . And to make sure of this fact, a simple test was held for the relationship between the solar events SEPs and the number of sun spot for the peak of solar cycle (24) (2012-2015) (sun spot number is an indicator of solar cycle) by considering the value of the correlation coefficient “R” through SPSS statistical program, so the result of R = 0.815, and according to statistical measurements for correlation coefficients, this result indicates to a relevant relation between solar events and solar cycle peak.

In fact, all these applications and approaches accounted for database work of the space agencies, in order to forecast the solar wind and warning from it, because some of solar wind affects Earth’s atmosphere and influence, satellites, power grids, communications, etc…and some other pass to other planets.

Wafaa Zaki,Atheer Zidane,Amjad Al-Sawad, (2016) Photometric and Statistical Analysis of Solar Energetic Particle (SEP) for the Peak of Solar Cycle 24. International Journal of Astronomy and Astrophysics,06,276-287. doi: 10.4236/ijaa.2016.63023