Relationship of decametric-hectometric type II radio burst, coronal mass ejections and solar flare observed during 1997–2014

Accepted Manuscript

Relationship of Decametric-Hectometric Type II radio burst, coronal mass ejections and solar flare observed during 1997-2014 Nishant Mittal , V.K. Verma PII: DOI: Reference:

S1384-1076(16)30044-6 10.1016/j.newast.2016.07.001 NEASPA 1002

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New Astronomy

Received date: Revised date: Accepted date:

24 December 2015 20 May 2016 4 July 2016

Please cite this article as: Nishant Mittal , V.K. Verma , Relationship of Decametric-Hectometric Type II radio burst, coronal mass ejections and solar flare observed during 1997-2014, New Astronomy (2016), doi: 10.1016/j.newast.2016.07.001

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ACCEPTED MANUSCRIPT Highlights The starting frequency of 85% DH type-II bursts lies in the range of 1- 14 MHz. DH type II radio bursts (1-16 MHz) originate between 2.2-4.5 RS. 48% DH Type II associated CMEs are located between ±40° of solar central disc. Mean linear/initial speed of DH Type II associated CMEs are 1157/ 1200 km/s. Most of type II bursts are associated with strong SXR (X, M) class of solar flares.

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Relationship of Decametric-Hectometric Type II radio burst, coronal mass ejections and solar flare observed during 1997-2014 Nishant Mittal1 and V. K. Verma2 1. Dept. of Physics, H.R. Institute of Technology, Ghaziabad - 201003, India 2. Uttrakhand Space Application Centre, Dehradun-248006, India

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Abstract: In the present study we have investigated 426 DH Type II radio burst and associated CMEs events observed during the time period of 1997-2014. The starting frequency of most of associated DH type-II bursts (85%) lies in the range of 1- 14 MHz (364 out of 426) with mean value of starting frequency is ~11MHz. The study of starting frequency (1-16 MHz) of DH type II bursts and heliocentric distance in solar radii indicate that DH type II radio bursts originate from 2.2-4.5 (RS) heliocentric distance in solar radii. We also found that the ~ 48% DH Type II radio bursts associated

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CMEs are located between ±40° of solar central disc and we also found that duration of DH type II radio bursts located at solar disc center are more than the duration of DH type II radio bursts located at solar limb. It is found that mean value for linear and initial speed of DH Type II associated CMEs are 1157 km/s and 1200 km/s, respectively. The CMEs speed are not correlated with duration of DH Type II radio bursts indicate that the durations of DH Type II radio bursts does not depend on speed of CMEs. The study also show that 426 DH type II radio bursts associated CMEs/flares occurred when there is coronal holes(CH) in nearby area and

the mean distance between DH type II burst associated

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CMEs/ flares and boundary of coronal hole (CH) is 26°. The study also shows that there is no relation between drift velocity of DH type II radio bursts and speed of CMEs. The study also indicate that about 45% flares those associated DH Type II radio bursts have duration about 60 minutes and long duration DH Type II radio bursts are associated with

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X-class flares. We found that the chances of DH type II radio bursts are more if the importance of SXR flares class increases. We have also discussed that the results obtained in the present investigation in view of latest heliophysics

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interpretations.

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Key words: Sun; Solar flares; Coronal mass ejections; DH Type II radio bursts 1. Introduction

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Solar radio bursts were amongst the first phenomena identified as targets for radio astronomy. Study on typeII radio bursts have been carried out by solar astronomers more than half century (Kundu, 1965; Reiner, 2000). The properties of type-II burst wavelength (1-16 MHz) associated with Coronal mass ejections (CMEs) were studied by several authors (Gopalswamy et al., 1999, Sharma et al, 2008, 2015, Suresh and Sangramanju, 2015, Mittal et al., 2016). The CMEs associated with DH-type-II radio bursts are called DHCMEs. The shocks driven by CMEs accelerated electrons; produce type-II bursts. CMEs associated with Type radio II bursts are more energetic on the average and there is a hierarchical relationship between CME kinetic energy and the wavelength range of Type II radio bursts (Gopalswamy et al., 2005; Lara et al., 2003; Gopalswamy, 2006). The average speeds of CMEs associated with Type II bursts confined to metric 

Corresponding author: Dr. Nishant Mittal (Ph: +919456662599) Email: [email protected]

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ACCEPTED MANUSCRIPT wavelengths is 610 km/s, only about 30% higher than the average speed (~470 km/s) of all CMEs. On the other hand Type II bursts with emission in the metric to kilometric wavelengths (the so-called m-km Type II bursts) are associated with CMEs of higher average speed: 1490 km/s, which is ~3 times the average speed of all CMEs. CMEs associated with decameter-hectometric (DH) Type II bursts have intermediate speed 1115 km/s. Interestingly, the average speed (1524 km/s) of CMEs associated with large solar energetic particle (SEP) events is very similar to that of CMEs with m-km Type II bursts. This is consistent with the idea that CME-driven shocks accelerate both ions and electrons. Statistical studies have confirmed this close

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association (see e.g. Gopalswamy, 2003; Cliver et al., 2004). Thus, Type II bursts, especially those occurring at longer wavelengths, have become good indicators of SEP events. There are some observations that contradict the above picture. It was recognized long ago that some fast CMEs observed during 1979–1982 were not associated with metric Type II bursts (Sheeley et al., 1984). These CMEs had speeds up to 1600 km/s with a median value of ~455 km/s. When CMEs move faster than the characteristic speed of the ambient medium (say, the Alfv´en speed), they drive fast-mode MHD shocks, which in turn accelerate electrons to

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produce the Type II bursts. In this scheme, the radio-quietness (i.e. the lack of Type II bursts in the metric and DH wavelengths) can be explained as being due to either the fast CMEs not attaining super-Alfv´enic speeds, or the CME-driven shocks are unable to excite Type II emission (Sheeley et al., 1984). Gopalswamy (1998) study a set of m-type-II radio bursts without interplanetary (IP) counterparts and IP shocks without m-type-II radio bursts and conclude that the shocks inferred from m-type-

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II radio bursts and the IP shocks are of different origin. It is now well-known that space weather is significantly controlled by coronal mass ejections (CMEs) which can affect our Earth environment in many

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ways (Gopalswamy, 2006; Iyer et al., 2006). The starting frequency of a type II burst is of particular interest because it is indicative of the height of shock formation ahead of the CME. By studying a large number of type II bursts associated with EUV waves or white-light CMEs, Gopalswamy et al. (2013) were able to

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determine the heights of shock formation. They found that the starting frequency (f) of a type II is smaller when the shock forms at a greater heliocentric distance according to the empirical relation, f = 308.17r-3.78 –

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0.14, where f is in MHz and r is the heliocentric distance in solar radii. Gopalswamy et al (2015) found that for the 2000 September 12 event, f = 24 MHz, so the shock formation height was r = 1.97 Rs, corresponding

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to the outer corona which is consistent with the estimate of ~1.92 Rs made from the flare acceleration method (Mäkelä et al. 2015). According to Gopalswamy et al (2015) the frequency range 2–14 MHz corresponds to plasma frequencies in the 3–10 RS heliocentric range and hence provides radio observations filling the gap between metric and kilometric observations. Shelke and Pande (1985) suggested that in many cases type II radio bursts are produced after shock waves gets connected with open magnetic fields of coronal holes. Earlier, Verma and Pande (1989) and Verma (1992, 1998, 2002) suggested that the CME events are perhaps have been produced by some mechanism, in which the mass ejected by some solar flares or active prominences, gets connected with the open magnetic lines of CHs (coronal holes: source of high speed solar winds) and moves

along them to

appear as CMEs. The recent papers of Liu, et al. (2006), Liu (2007), Jiang, et al. (2007) and Asai et al. (2008, 2009) carried out studied CMEs and found that CHs close to the active region involved in the coronal mass ejections. 3

ACCEPTED MANUSCRIPT In the present paper we propose to investigate relationship between DH Type II radio burst and associated CMEs including other solar phenomena observed during the interval period of 1997 to 2014. No studies have ever dealt with such a large sample of 426 DH Type II radio burst associated CME events, to understand the properties of Type II radio burst associated CMEs. In section 1 of the paper we try give an introduction about various facts of Type II radio burst associated CMEs related research work. In section 2 of paper we mentioned about observational data and analysis. In section 3 we have discussed the results obtained in the present investigation. A brief summary and conclusions are delivered in last section 4.

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2. Observational Data, Analysis and Results

In present study we have considered 426 DH Type II bursts associated CMEs those are available online at the CDAW Data Center (http://cdaw.gsfc.nasa.gov/CME_list/radio/waves type2.html). The detailed information for CMEs and solar flares observed LASCO (Brueckner et al., 1995) and other instruments are taken from CDAW catalogue (http://cdaw.gsfc.nasa.gov/CME_list). The DH-type-II bursts are recorded

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in the frequency range between 16MHz to 20 kHz using RAD-2 (16–1MHz) and RAD-1 (1MHz–20 kHz) instruments by the Radio and Plasma Wave (WAVES) experiment on board the Wind spacecraft (Bougeret et al., 1995). The Type II burst starting frequency indicates the height at which shocks are being formed from the eruption (Gopalswamy et al., 2005). Total 482 events are observed during period 1997-2014, but 56 events does not have clear frequency and time duration, therefore after excluding 56 events we are left with 426

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DH Type II radio bursts.

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2.1. DH Type II radio bursts associated CMEs and solar flares The probability density distributions and cumulative distribution function of starting and ending frequency of DH Type II radio burst events are presented in Figures 1 and 2. Figure 1 shows the

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starting frequency of DH type-II bursts varies from 16 to 1MHz, where 16MHz is the upper cutoff frequency of the WAVES instrument. The starting frequency of events at 16MHz implies that they cover the whole

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range of the WAVES instrument and some of them may be a continuation of metric type-II bursts. We calculated the mean value of DH type II radio bursts starting frequency of 426 events is 11 MHz as shown in

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Figure 1. From distribution we can conclude that 34% DH type-II bursts have starting frequencies below or equal to 10MHz and remaining 66% events has frequency greater than 10MHz. The type-II burst ending frequency indicates the energy of CMEs (Gopalswamy et al., 2005, 2006); that is, when the kinetic energy of the associated CMEs are more than the shock can travel to larger distance in the interplanetary medium. Figure 2 shows that 84% events have ending frequency within the range of 20KHz to 5MHz and the remaining 16% DH type-II bursts have frequency greater than 5MHz. The mean value of DH type II bursts ending frequency is 2.23 MHz as shown in Figure 2. According to Gopalswamy et al (2015) the frequency range 2–14 MHz corresponds to plasma frequencies in the 3–10 RS heliocentric range and hence provides radio observations filling the gap between metric and kilometric observations. Gopalswamy et al. (2013) were able to determine the heights of shock formation. They found that the starting frequency (f) of a type II is smaller when the shock forms at a greater 4

ACCEPTED MANUSCRIPT heliocentric distance according to the empirical relation, f = 308.17r -3.78 – 0.14, where f is in MHz and r is the heliocentric distance in solar radii. We have used above relation to calculated the heliocentric distance in solar radii for all 426 events. The starting frequency of DH type II radio bursts versus heliocentric distance in solar radii is shown in Figure 3. Out of 426 DH Type II radio burst associated SXR flares considered for study, the locations of 77 DH Type II radio burst associated SXR flares are not known. The spatial location of 349 DH Type II radio burst

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associated SXR flares on solar disc are shown in Figure 4.

In Figure 4 we have plotted solar disk locations of Type II radio burst associated CMEs related solar flares on x axis as an east (-90⁰ to 0⁰) to west (0⁰ to 90⁰) longitude in degree and on y axis as a south (-90⁰ to 0⁰) – north (0⁰ to 90⁰) latitude in degree. The location of Type II radio burst associated CMEs related solar flares in Figure 4 are shown by filled circle and the relative sizes of filled circle represent the duration of DH Type II radio burst. The smaller sizes of filled circles represent small duration DH Type II radio burst while bigger

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sizes of filled circles represent large duration of DH Type II radio bursts. It is clear from Figure 4 that the source locations of ~97% DH Type II radio burst associated CMEs related solar flares occur within ±30⁰ solar latitude while solar longitude: east-west longitude shows that the ~48% DH Type II radio burst associated CMEs related solar flares sources are mostly concentrated within ±40⁰ solar longitude. From figure 4 it is clear that those DH Type II bursts are associated with flares have long duration in ±30⁰

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longitudinal range at solar disc. From figure 4 it is also clear that the flares associated with short duration DH Type II bursts are distributed throughout the solar disc. The SXR class of DH Type II radio burst associated

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CMEs related solar flares are investigated and found that the SXR class of 80 DH Type II radio burst associated SXR solar flares are not known and these 80 events are excluded from study. The SXR class of 346

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type II radio burst associated solar flares are known. In Table 1 we have shown the relation between duration of Type II radio burst and Type II radio burst related CMEs associated classes of SXR solar flares. It is clear from Table 1 that 24% of DH Type II associated CMEs are related with X-class flares, 49% of DH Type II

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associated CMEs are related with M-class flares, 25% of DH Type II associated CMEs are related with Cclass flares and 2% of DH Type II associated CMEs are related with A and B SXR class flares. We have also

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studied the relation between duration of DH Type II radio burst and classes of SXR flares associated with type II radio burst are shown in Table 1. From Table 1 it is clear about 45% flares those associated DH Type II bursts have duration about 60 minutes. In Table 2 we show mean and median duration of DH Type II bursts relative to intensity of flares. From Table 2 it is also clear that durations of

SXR flares increases as

importance of SXR flares .i.e the mean and median durations of X class of SXR flares are greater than M class of SXR flares. In Figure 5 (lower panel) we have shown a probability density distribution and cumulative distribution function plot between linear speed of CMEs versus fraction of CMEs with mean and median speed of CMEs and In Figure 5 (upper panel) we have shown a probability density distribution and cumulative distribution function plot between initial speed of CMEs versus fraction of CMEs with mean and median speed of CMEs. As clear from Figure 5, there is not much difference in the mean value of DH Type II 5

ACCEPTED MANUSCRIPT associated CMEs for two different speeds, such as linear and initial speed. The mean value of linear speed is 1157 km/s while mean initial speed is 1200 km/s. Median linear speed is 1099 km/s and median initial speed is 1122 km/s. The mean and median initial speed is slightly greater than mean linear speed.

We also studied the relation between various speeds of CMEs versus duration of DH Type II radio burst as shown in Figure 6. In upper panel of Figure 6 we have shown a plot between linear speed and initial speed of CMEs versus duration of DH Type II radio burst. In lower panel of Figure 6 we have shown a plot between

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initial speed of CMEs versus duration of DH Type II radio burst. In upper panel of Figures 6 show weak correlations between speeds of CMEs versus duration of DH Type II radio burst. The correlation between duration of DH Type II bursts and linear speed of CMEs and initial speeds of CME are 0.27 and 0.25, respectively which clearly indicate that the duration of DH type radio bursts does not depend on speed of CMEs.

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The relation between acceleration of CMEs associated with DH Type II radio burst and duration of DH Type II radio burst is studied to know their relationship. In Figure 7 we have plotted a relation between duration of DH Type II radio burst versus accelerations of DH CMEs with correlation coefficient R= -0.01. The poor correlations clearly indicate that the duration of burst does not depend on accelerations of CMEs.

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The probability density distribution and cumulative distribution function of apparent width of Type II radio bursts associated CMEs are presented in Figure 8. The angular width is the angular extent between the two

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edge position angles of the CME in the sky plane. The width of the CMEs varies between few degree to 360 degree. The average width of DH- CMEs is 271 degree, while the average width of CMEs is 580 as shown by Mittal et al., (2009, and 2010). From figure 8 it is clear that 57% (244) events have width larger than 300

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degree. Out of 244 events 242 are full HCMEs. 15% events have width less than 120 degree and remaining

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28% have width between 1200- 3000.

Figure 9 shows probability density distribution and cumulative distribution function of acceleration of events

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with their numbers. 57% of DH CMEs are decelerated, 15% are moving with zero or little acceleration and remaining 28% are accelerated. It is clear from figure that DH type II bursts associated CMEs are bias towards deceleration and peak occurs at -10 m/s2. The mean value of DH type II associated CMEs acceleration is -7.79 m/s2, when we restricted the CMEs acceleration range between ±110 m/s2. Figure 10 shows the relation between drift velocity of Type II radio burst and speed of CMEs. It is clear from figure that there is very low correlation between drift velocity and linear and initial speed of CMEs. The correlation coefficient between drift velocity of DH Type II radio bursts between linear speed of CMEs is -0.24 while the correlation coefficient between drift velocity of DH Type II radio bursts between initial speed of CMEs is -0.22 which indicate that drift velocity of DH type II radio bursts has no relation with linear or initial speed of CMEs.

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ACCEPTED MANUSCRIPT Figure 11 upper panel shows a scatter plot of linear speed of DH type II bursts associated CMEs with versus acceleration of CMEs with values of correlation coefficient as R= -0.24 while Figure 11 lower panel shows a scatter plot of initial speed of DH type II bursts associated CMEs with versus acceleration of CMEs with values of correlation coefficient as R= -0.51. Upper panel of figure 11 indicates that there is no correlation between linear speed of DH-CMEs and acceleration; while lower panel of figure 11 indicates that initial speed of DH-CMEs has good correlation with acceleration.

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2.2 Role of CHs in origin of CMEs and related DH Type II radio bursts We know that the CMEs are usually associated with solar flares like active phenomena which are mainly responsible for CMEs occurrences. As mentioned earlier Verma & Pande (1989), Verma (1992), Verma (1998), and Verma (2002) reported the role of coronal holes and solar flares/ eruptive solar phenomena in the origin of CMEs by investigating temporal and spatial relationship between

CMEs associated solar flare

location's and boundary of CHs. Verma (2002) analyzed 196 CMEs observed by LASCO/ SOHO during year

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2000 using CHs daily map and CHs synoptic chart data observed by Kit Peak National Observatory (KPNO), USA and solar flares observed by various ground observatories and found that CMEs are associated Hα flares and coronal holes. In the present investigation to determine the distance between the CMEs associated solar flares or solar active phenomena locations and CHs locations, we used Heliophysics Event Registry search

http://www.lmsal.com/isolsearch.

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program, available at Lockheed Martin Solar Astrophysics Laboratory, USA at following link:

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From the analysis of 426 DH type II associated CMEs, solar flares and CHs we have found that in all cases of DH type radio bursts II associated CMEs were produced when CMEs associated solar flares and CHs boundary are very closed as shown Figure 12. Figure 12 shows probability density distribution and

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cumulative distribution function plot. Recently Mittal and Verma (2016) used this methodology to understand the relation between geomagnetic storms and CHs. In Table 3 we have shown the relationship of distance

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between duration of DH Type II radio burst associated solar SXR flares and boundary of CHs. From Table 2 It is clear that the duration of DH Type II radio burst and distance between boundary of CHs and location of

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Type II radio burst associated solar flares has no relation. In Figure 12 we have plotted x-axis as a distance between DH Type II radio bursts associated solar flares locations and coronal holes boundary and y-axis as a number of DH Type II radio bursts associated CMEs. In Figure 12 shows that mean and median distance between the DH type II radio bursts associated solar flares and boundary of CHs are 26⁰ and 20⁰, respectively.

2.3 Relation between Type II Radio Bursts and other Solar Phenomena

We try to understand the relation between type II bursts and other solar phenomena by studying correlation matrix as shown in Table 4. In column C1we have shown Duration of type II radio bursts, In column C2 we have shown Drift velocity of type II bursts, C3 we have shown the Linear Speed of CMEs associated with type II radio bursts, in column C4 we have shown an Initial Speed of CMEs associated with type II radio 7

ACCEPTED MANUSCRIPT bursts, in column C5 we have shown an acceleration of CMEs associated with type II radio bursts, in column C6 we have the flare Energy of various SXR flares derived from their class, in column C7 we have shown the distance between coronal hole and flare and in column C8 we have shown an angular width of CMEs associated with type II radio bursts. We know that values of correlation varies between 1 to -1. The values of correlation and strength of the linear relationship may be described as 1 as perfect relationship, 0.8-1.0 as very strong, 0.60-0.80 as strong relationship, 0.40-0.60 as moderate relationship, 0.20-0.40 as weak relationship and 0.00-0.20 as none or extremely weak relationship. The various correlation values given in Table 4 clearly

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show that there are moderate to weak relation between duration of type II bursts and other solar phenomena.

3. Results, Discussions and Conclusions

In the present study we have investigated 426 type II radio burst and associated CMEs events observed during the time period of 1997-2014. The main results of an investigation carried out in previous section to understand the DH Type II radio bursts associated CMEs are as under:

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1. The starting frequency of most of associated DH type-II bursts (85%) lies in the range of 1- 14 MHz (364 out of 426) with mean starting frequency is ~11MHz; as shown in Figure 1. The mean value of starting frequency of DH type II bursts 11 MHz indicate that in most cases type DH type II radio bursts starts around 11 MHz

2. The ending frequencies lie in the range 20 KHz to 8MHz for 95% of events, i.e. 406 events out of 426

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events. Average ending frequency is about 2.23MHz; as shown in Figure 2.

3. The study of starting frequency of DH type II bursts and heliocentric distance in solar radii suggest that DH

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type II radio bursts of frequencies 1-16 MHz originate between 2.2-4.5 heliocentric distance in solar radii. 4. From Table 2 it is clear about 45% flares those associated DH Type II bursts have duration about 60 minutes. Table 2 it is also clear that mean and median duration DH Type II radio bursts increases with the

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importance of class of SXR flares.

5. From Figure 4 it is clear that the 48% DH Type II associated CMEs are located between ±40° of solar

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central disc and also found that duration of DH type II radio bursts at central disc are larger in compare to limb DH Type II radio bursts.

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6. Figure 5 show distribution of speed of DH Type II associated CMEs for linear speed and initial speed with mean values of linear speed of CMEs and initial speed of CMEs associated with DH Type II radio bursts are 1157 km/s and 1200 km/s, respectively. 7. Figure 6 shows scatter plot of linear and initial speed of CMEs versus duration of DH Type II bursts. The values for correlation coefficients of linear and initial speed of CMEs versus duration of DH Type II bursts are 0.27 and 0.25, respectively which are very low and indicate no relation between speed of CMEs and duration of DH type II radio bursts. 8. Figure 7 shows scatter plot of acceleration of CMEs and duration of DH type II radio bursts with value of correlation coefficients as r= -0.01 which is very low indicating no relation between acceleration of CMEs and durations of DH type II radio bursts.

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ACCEPTED MANUSCRIPT 9. Figure 8 shows histogram plot between angular width of CMEs and number of DH type II radio bursts and shows that mean apparent angular width of DH type II bursts associated CMEs is 2710. 10. Figure 9 shows histogram plot between acceleration of CMEs associated with DH type II radio bursts with number of DH type II radio bursts. Figure 9 also indicate that 57% of DH type II radio bursts associated CMEs are decelerated, 15% of DH type II radio bursts associated CMEs are moving with zero or little acceleration and remaining 28% of DH type II radio bursts associated CMEs are accelerated. It is clear from Figure 9 that DH type II bursts associated CMEs are bias towards deceleration and peak occurs at -10 m/s2.

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The mean value of DH type II associated CMEs acceleration is -7.79 m/s2, when we restricted the CMEs acceleration range between ±110 m/s2.

11. Figure 10 shows a scatter plot of drift velocity of DH Type II radio bursts with linear and initial speed of CMEs. The correlation coefficient between drift velocity of DH Type II radio bursts between linear speed of CMEs is -0.24 while the correlation coefficient between drift velocity of DH Type II radio bursts between initial speed of CMEs is -0.22 which indicate that drift velocity of DH type II radio bursts has no relation

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with linear or initial speed of CMEs.

12. Figure 11 upper panel shows a scatter plot of linear speed of DH type II bursts associated CMEs with versus acceleration of CMEs with values of correlation coefficient as R= -0.24 while

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panel of

Figure 11 shows a scatter plot of initial speed of DH type II bursts associated CMEs with versus acceleration of CMEs with values of correlation coefficient as R= -0.51. there is no correlation between

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linear speed of DH-CMEs and acceleration; while initial speed of DH-CMEs has good correlation with acceleration.

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13. The Figure 12 is histogram between distance between location of DH type II associated CMEs related solar flares and boundary of CHs in degree versus number of DH type II radio bursts. We have found that in all cases of DH type radio bursts II associated CMEs were produced when CMEs associated solar flares and

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CHs boundary are very closed as shown Figure 12. 14. In Table 3 we have shown the relationship of distance between duration of DH Type II radio burst

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associated solar SXR flares and boundary of CHs. From Table 3 It is also clear that the duration of DH Type II radio burst and distance between boundary of CHs and location of Type II radio burst associated solar flares

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has no relation. The mean and median distance between the DH type II radio bursts associated solar flares and boundary of CHs are 26⁰ and 20⁰, respectively. 15. We found that 24% of DH Type II associated CMEs are related with X-class flares, 49% of DH Type II associated CMEs are related with M-class flares, 25% of DH Type II associated CMEs are related with Cclass flares and 2% of DH Type II associated CMEs are related with A and B - SXR class flares.

Komitov, et al, (2010) analysed SXR flares data observed by GOES satellite during period of 1980 -2009 and found that during 1980-2009 a total of 44267 SXR flares were observed by GOES satellite and Out of these 87.22% belong to C class of SXR flares, 11.86% belong to M class of SXR flares and 0.91% belong to X Class of SXR flares. This indicate that chances of DH type II radio bursts are more if the importance of SXR flares class increases. An investigation also tell us that all large flares does not produce 9

ACCEPTED MANUSCRIPT Type II radio burst clearly tell us that solar flares and CMEs may be necessary condition but sufficient condition for occurrence of DH Type II radio burst events are still unknown. This indicate role CHs may be very important in production of DH type II radio bursts as earlier suggested by Shelke and Pande(1985). We have also studied the relation between duration of DH Type II radio burst and classes of SXR flares associated with type II radio burst and we found that 45% flares those associated DH Type II bursts have duration about 60 minutes. In Table 2 we show mean and median duration of DH Type II bursts relative to intensity of flares. From Table 2 it is also clear that durations of SXR flares increases as importance of SXR flares .i.e the mean

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and median durations of X class of SXR flares are greater than M class of SXR flares. In investigation we also find 48% solar flares associated DH CMEs are located between ±40° of solar disc. We noted that the duration of Type II DH radio burst (Duration in min) does not depend on the speeds and accelerations of CMEs associated with Type radio burst. It is also noted that the duration of Type II radio burst (Duration in min) appeared to be depend on the class of SXR solar flares indicating that large solar flares may produce strong Type radio burst.

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Type II radio bursts in the metric and longer wavelengths are of primary interest because they are indicative of shock-accelerated particles. According to Gopalswamy et al (2015) the frequency range 2–14 MHz corresponds to plasma frequencies in the 3–10 Rs heliocentric range and hence provides radio observations filling the gap between metric and kilometric observations. The starting frequency of a type II burst is of particular interest because it is indicative of the height of shock formation ahead of the CME. By

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studying a large number of type II bursts associated with EUV waves or white-light CMEs, Gopalswamy et al. (2013) were able to determine the heights of shock formation. They found that the starting frequency (f) of a

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type II is smaller when the shock forms at a greater heliocentric distance according to the empirical relation, f = 308.17r-3.78 – 0.14, where f is in MHz and r is the heliocentric distance in solar radii. For the 2000 September 12 event, f = 24 MHz, so the shock formation height was r = 1.97 Rs, corresponding to the outer

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corona. This is consistent with the estimate of ~1.92 Rs made from the flare acceleration method (Mäkelä et al. 2015). Following , Gopalswamy et al. (2013) empirical relation = 308.17r-3.78 – 0.14, where f is in MHz

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and r is the heliocentric distance in solar radii we have estimated the heliocentric distance in solar radii for all 426 events as shown in Figure 3. The heliocentric distance in solar radii for mean frequency and median

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frequency also estimated as shown in Figure 3. As discussed in section 2.2 we have found locations of DH type II related CMEs associated

flare (FL) and CH and the distance between flare and CHs are 10-90⁰ with mean distance value as 26° and median distance value as 20°. As clear from Figure 12 that about 49% DH type II related CMEs associated flare (FL) and CH and the distance between flare and CHs are 10°. Shelke & Pande (1985) suggested that in many cases type II radio bursts are produced after shock waves gets connected with open magnetic fields of coronal holes. Earlier, Verma and Pande (1989) and Verma (1992, 1998, 2002) suggested that the CME events are perhaps have been produced by some mechanism, in which the mass ejected by some solar flares or active prominences, gets connected with the open magnetic lines of CHs (coronal holes: source of high speed solar winds) and moves along them to appear as CMEs. In the view of above we conclude that in the production of DH type II radio bursts, the role CMEs/solar flares and CH appear to be very important. The 10

ACCEPTED MANUSCRIPT theoretical interpretation for production of DH type II radio bursts based on CMEs/solar flares and CH is not available and thus it should be developed to understand DH type II radio bursts phenomena.

4. Brief Summary and Conclusions In the present study we have investigated 426 DH Type II radio burst and associated CMEs events observed during the time period of 1997-2014. The starting frequency of most of associated DH type-II bursts (85%) lies in the range of 1- 14 MHz (364 out of 426) with mean value of starting frequency is ~11MHz. The

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study of starting frequency (1-16 MHz) of DH type II bursts and heliocentric distance in solar radii indicate that DH type II radio bursts originate from 2.2-4.5 (RS) heliocentric distance in solar radii. We also found that the 48% DH Type II radio bursts associated CMEs are located between ±40° of solar central disc and we also found that duration of DH type II radio bursts located at solar disc center are more than the duration of DH type II radio bursts located at solar limb. It is found that mean value linear and initial speed of DH Type II associated CMEs are 1157 km/s and 1200 km/s, respectively. The CMEs speed are not correlated with

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duration of DH Type II radio bursts indicate that the durations of DH Type II radio bursts does not depend on speed of CMEs. The study also show that 426 DH type II radio bursts associated CMEs/flares occurred when there is coronal holes(CH) in nearby area and the mean distance between DH type II burst associated CMEs/ flares and boundary of coronal hole (CH) is 26°. The study also shows that there is no relation between drift velocity of DH type II radio bursts and speed of CMEs. The study also indicate that about 45%

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flares those associated DH Type II radio bursts have duration about 60 minutes and long duration DH Type II radio bursts are associated with X-class flares. This study also indicate that chances of DH type II radio

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bursts are more if the importance of SXR flares class increases. The investigation also shows that mean value of apparent angular width of DH type II bursts associated CMEs is 2710 and mean value of acceleration of DH type II radio bursts associated CMEs is -7.79 m/s2. The various correlation values given in Table 4 clearly

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show that there are moderate to weak relation between duration of type II bursts and other solar phenomena.

Acknowledgements: We are thankful to N. Gopalswamy and his team for providing CMEs related to data to users

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through CDAW. This CME catalogue is generated and maintained by the Centre for Solar Physics and Space Weather. The Catholic University of America in cooperation with the Naval Research Laboratory and NASA. SOHO is a project of international cooperation between ESA and NASA. We are also thankful to creator of WIND/WAVES catalogue of radio burst whose data are used in the present study. We are thankful to anonymous referee for excellent comments

which improves the contents of the paper.

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ACCEPTED MANUSCRIPT Sheeley, N. R., Jr.; Howard, R. A.; Michels, D. J.; Robinson, R. D.; Koomen, M. J. Associations between coronal mass ejections and metric type II bursts, ApJ, 279, 839

and

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Verma, V. K., 2002, Coronal mass ejections: Relationship with solar flares and coronal holes, COSPAR Colloquia Series, Elsevier Science Ltd, 13, 319

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Figure Caption:

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Mean = 11 MHz

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Figure 1: Histogram shows probability density and cumulative distribution as fraction of DH type II radio burst events versus starting frequency (MHz)

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Mean = 2.23 MHz

Figure 2: Histogram shows probability density and cumulative distribution as fraction of DH type II radio burst events versus ending frequency (MHz)

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No. of Events = 426

4.5

3.5 3 2.5

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Distance in Solar radii

Mean Frequency = 10.98 MHz 4

2 1.5 1

Median Frequency = 14 MHz

0 0

1

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3

4

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7

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9

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Starting Frequency (MHz)

Figure 3: Shows plot of starting frequency of DH type II radio bursts versus heliocentric distance in solar

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radii with heliocentric distance in solar radii of mean and median frequency.

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90 80 70 60

12.5 hrs

50

65.25 hrs

30 20 10 0

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Latitude (Degree)

40

-10 -20 -30 -40

0.41 hrs

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-90 -80 -70 -60 -50 -40 -30 -20 -10

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Longitude (Degree)

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Figure 4: Figure shows latitudinal and longitudinal distribution of 426 DH Type II associated SXR flares locations on solar disc with their durations.

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Mean = 1200 km/sec Median = 1122 km/sec

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Initial Speed

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Mean = 1157 km/sec Median = 1099 km/sec

Linear Speed

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Linear Speed

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Initial Speed

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Figure 5: Upper figure show the probability density and cumulative distribution of initial speed of DH Type II associated CMEs versus fraction of DH Type II associated CMEs with mean and median CMEs speed for 420 events. Lower figure show the distribution of linear speed of DH Type II associated CMEs versus fraction of DH Type II associated CMEs with mean and median CMEs speed for 426 events.

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4500

t = 0.252VCME + 23.67

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R = 0.27

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Linear Speed

2500 2000 1500 1000 500 0 500

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Duration (min.)

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Speed (km/sec) 4500

t = 0.219VCME + 52.32

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Speed (km/sec)

Figure 6: Upper figure shows the scatter plot of linear speed of CMEs associated with DH Type II radio bursts versus duration of DH type II radio bursts with values of correlation coefficient while lower figure shows the scatter plot of initial speed of CMEs associated with DH Type II radio bursts versus duration of DH type II radio bursts with values of correlation coefficient.

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250 200

a= -0.005t - 9.202

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R = -0.01

50 0 -50 -100 -150 -200 -250 500

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Acceleration (m/s2)

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Duration (min.)

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Figure 7: Scatter plot shows the relation between DH Type II bursts duration and acceleration of CMEs.

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Figure 8: Histogram shows probability density and cumulative distribution of the widths of CMEs associated with DH Type II bursts for 426 events.

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Figure 9: Histogram shows probability density and cumulative distribution values acceleration of CMEs associated with DH type II radio bursts for all events.

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4000

Events = 426 Linear CME Speed

3000 2500 2000

VCME = -1.024Vd + 1266.

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R = -0.24

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CME Speed (km/sec)

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VCME = -1.027Vd + 1312

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Figure 10: Upper figure show a scatter plot of Drift velocity of DH type II bursts versus linear CMEs speed with values of correlation coefficient. Lower figure show a scatter plot of Drift velocity of DH type II bursts versus initial CMEs speed with values of correlation coefficient.

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90

y = -0.019x + 11.63

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R = -0.24

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Acceleration (m/s2)

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Figure 11: Upper figure show a scatter plot of linear speed of DH type II radio bursts associated CMEs versus acceleration of CMEs with values of correlation coefficient. Lower figure show a scatter plot of initial speed of DH type II radio bursts associated CMEs versus acceleration of CMEs with values of correlation coefficient. 24

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Figure 12: Figure shows the probability density and cumulative distribution for distance between flare location and coronal hole for all CMEs associated DH Type II radio bursts with mean value as 26°.

Table Caption: Table 1: Durations (min) of DH Type II radio bursts and associated of SXR flares Duration (min)

Number of SXR flares associated with DH type II radio bursts B- Class C- Class M- Class X- Class 25

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0 55 8 5 2 0 1 3 0 0 0 13

1 80 22 11 3 7 3 5 4 3 4 29

1 18 10 7 5 3 1 5 4 1 6 22

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0 4 1 0 0 0 0 0 0 0 0 0

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0 60 120 180 240 300 360 420 480 540 600 >600

Table 2: Durations (min) of DH Type II radio burst associated various classes of SXR flares Flares associated with type II radio burst Duration (min)

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C- Class

M- Class

X- Class

172

83

313

501

75

265

0

5

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Mean Duration

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No. of Events

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Median Duration

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CH Distance

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Table 3: Distance between boundary of CHs and location of DH Type II radio burst associated flares

A- Class 0 0 0 0 0 0 0 0 0

Flares associated DH type II Radio Bursts B- Class C- Class M- Class 1 28 83 1 17 30 1 8 20 0 9 10 1 7 1 0 5 7 1 5 11 0 3 5 0 1 4

X- Class 48 13 4 5 5 3 1 2 0

Table 4: Spearman correlation matrix for different solar parameters C1

C2

C3

C4

C5 26

C6

C7

C8

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C2

0.93681 0.49015 7 0.46177 3 0.06026 0.28839

C3 C4 C5 C6 C7 C8

0.02220 1 0.43972 6

0.93681 1 0.42708 0.40204 0.03703 2 0.24671 0.01693 0.40194

0.49015 7 0.42708 1

0.46177 3 0.40204 0.94612

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1

0.16369 0.42486 8 0.11292 0.39158 6

0.42343 0.43748 0.10223 0.39528 3

C1 = Duration of type II radio bursts

0.21636 0.06963 0.11592

0.28839 0.24671 0.42486 8 0.43748 0.21636 1 0.14183 0.29041 6

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C2 = Drift velocity

0.06026 0.03703 2 0.16369 0.42343 1

C3 = Linear Speed of CMEs associated with type II radio bursts C4 = Initial Speed of CMEs associated with type II radio bursts

C5 = Acceleration of CMEs associated with type II radio bursts C6 = Flare Energy derived from their class C7 = Distance between Coronal Hole and flare

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C8 = Angular width of CMEs associated with type II radio bursts

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0.02220 1 0.01693 0.11292 0.10223 0.06963 0.14183 1

0.43972 6 0.40194 0.39158 6 0.39528 3 0.11592 0.29041 6 0.03278 2 1

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C1

0.03278 2