We have statistically analyzed a set of 115 low frequency (Deca-Hectometer wavelengths range) type II and type III bursts associated with major Solar Energetic Particle (SEP: E_p> 10 MeV) events and their solar causes such as solar flares and coronal mass ejections (CMEs) observed from 1997 to 2014. We classified them into two sets of events based on the duration of the associated solar flares:75 impulsive flares (duration < 60 min) and 40 gradual flares (duration > 60 min).On an average, the peak flux (integrated flux) of impulsive flares × 2.9 (0.32 J m⁻²) is stronger than that of gradual flares M6.8 (0.24 J m⁻²). We found that impulsive flare-associated CMEs are highly decelerated with larger initial acceleration and they achieved their peak speed at lower heights (− 27.66 m s⁻² and 14.23 R_o) than the gradual flare-associated CMEs (6.26 m s⁻² and 15.30 R_o), even though both sets of events have similar sky-plane speed (space speed) within LASCO field of view. The impulsive flare-associated SEP events (R_t = 989.23 min: 2.86 days) are short lived and they quickly reach their peak intensity (shorter rise time) when compared with gradual flares associated events (R_t= 1275.45 min: 3.34 days). We found a good correlation between the logarithmic peak intensity of all SEPs and properties of CMEs (space speed: cc = 0.52, SE_cc= 0.083), and solar flares (log integrated flux: cc = 0.44, SE_cc= 0.083). This particular result gives no clear cut distinction between flare-related and CME-related SEP events for this set of major SEP events. We derived the peak intensity, integrated intensity, duration and slope of these bursts from the radio dynamic spectra observed by Wind/WAVES. Most of the properties (peak intensity, integrated intensity and starting frequency) of DH type II bursts associated with impulsive and gradual flare events are found to be similar in magnitudes. Interestingly, we found that impulsive flare-associated DH type III bursts are longer, stronger and faster (31.30 min, 6.43 sfu and 22.49 MHz h⁻¹) than the gradual flare- associated DH type III bursts (25.08 min, 5.85 sfu and 17.84 MHz h⁻¹). In addition, we also found a significant correlation between the properties of SEPs and key parameters of DH type III bursts. This result shows a closer association of peak intensity of the SEPs with the properties of DH type III radio bursts than with the properties DH type II radio bursts, atleast for this set of 115 major SEP events.

我们统计分析了与主要太阳高能粒子（SEP： E _p > 10 MeV）事件相关的一组 115 个低频（十百米波长范围）II 型和 III 型爆发及其太阳耀斑和日冕质量等太阳原因1997 年至 2014 年观测到的抛射（CME）。我们根据相关太阳耀斑的持续时间将它们分为两组事件：75 次脉冲耀斑（持续时间 < 60 分钟）和 40 次渐进耀斑（持续时间 > 60 分钟）。平均而言，脉冲耀斑的峰值通量（积分通量）×2.9（0.32 J m ^-2）强于渐变耀斑M6.8（0.24 J m ^-2）。我们发现，与渐进耀斑相关的日冕物质抛射（CME）（6.26 m s ^{-2和 15.30} R _o）相比，与脉冲耀斑相关的日冕物质抛射（CME）高度减速，具有更大的初始加速度，并且它们在较低的高度（− 27.66 m s ^-2和 14.23  R o ）达到峰值速度。 _o），尽管两组事件在 LASCO 视野内具有相似的天面速度（空间速度）。与渐进耀斑相关事件（ R _t = 1275.45 分钟：3.34 天） 相比，脉冲耀斑相关 SEP 事件（R _t = 989.23 分钟：2.86 天）持续时间较短，并且很快达到峰值强度（上升时间较短）。我们发现所有 SEP 的对数峰值强度与 CME 的特性（空速：cc  = 0.52，SE _cc = 0.083）和太阳耀斑（对数积分通量：cc  = 0.44，SE _cc = 0.083）之间存在良好的相关性。对于这组主要 SEP 事件，这一特定结果没有明确区分耀斑相关和 CME 相关 SEP 事件。我们从 Wind/WAVES 观测到的无线电动态光谱中得出了这些爆发的峰值强度、积分强度、持续时间和斜率。与脉冲和渐进耀斑事件相关的 DH II 型爆发的大多数特性（峰值强度、积分强度和起始频率）被发现在强度上相似。有趣的是，我们发现与渐进耀斑相关的DH III型爆发（25.08分钟、5.85 sfu和17.84）相比，脉冲耀斑相关的DH III型爆发更长、更强、更快（31.30分钟、6.43 sfu和22.49 MHz h ⁻¹）。 MHz h ^-1 )。此外，我们还发现SEP的性质与DH III型爆发的关键参数之间存在显着相关性。该结果表明，SEP 的峰值强度与 DH III 型射电爆发的特性的关联性比与 DH II 型射电暴特性的关联性更紧密，至少对于这组 115 个主要 SEP 事件而言是如此。