Characteristics of DH type II bursts, CMEs and flares with respect to the acceleration of CMEs

Details Characteristics of DH type II bursts, CMEs and flares with respect to the acceleration of CMEs Characteristics of DH type II bursts, CMEs and flares with respect to the acceleration of CMEs

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012ap%26ss.337...47p&link_type=abstract

Astrophysics and Space Science, Volume 337, Issue 1, pp.47-64

Astronomy and Astrophysics

Astrophysics

Sun, Coronal Mass Ejections, Solar Flares, Type Ii Bursts

Scientific paper

A detailed investigation on DH-type-II radio bursts recorded in Deca-Hectometer (hereinafter DH-type-II) wavelength range and their associated CMEs observed during the year 1997-2008 is presented. The sample of 212 DH-type-II associated with CMEs are classified into three populations: (i) Group I (43 events): DH-type-II associated CMEs are accelerating in the LASCO field view ( a>15 m s-2); (ii) Group II (99 events): approximately constant velocity CMEs (-15< a<15 m s-2) and (iii) Group III (70 events): represents decelerating CMEs ( a<-15 m s-2). Our study consists of three steps: (i) statistical properties of DH-type-II bursts of Group I, II and III events; (ii) analysis of time lags between onsets of flares and CMEs associated with DH-type-II bursts and (iii) statistical properties of flares and CMEs of Group I, II and III events. We found statistically significant differences between the properties of DH-type-II bursts of Group I, II and III events. The significance ( P a ) is found using the one-way ANOVA-test to examine the differences between means of groups. For example, there is significant difference in the duration ( P a =5%), ending frequency ( P a =4%) and bandwidth ( P a =4%). The accelerating and decelerating CMEs have more kinetic energy than the constant speed CMEs. There is a significant difference between the nose height of CMEs at the end time of DH-type-IIs ( P a ≪1%). From the time delay analysis, we found: (i) there is no significant difference in the delay (flare start—DH-type-II start and flare peak—DH-type-II start); (ii) small differences in the time delay between the CME onset and DH-type-II start, delay between the flare start and CME onset times. However, there are high significant differences in: flare duration ( P a =1%), flare rise time ( P a =0.5%), flare decay time ( P a =5%) and CMEs speed ( P a ≪1%) of Group I, II and III events. The general LASCO CMEs have lower width and speeds when compared to the DH CMEs. It seems there is a strong relation between the kinetic energy of CMEs and DH-type-II properties.

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