A statistical study on the properties of CMEs and flares associated with DH-type II bursts in the 23rd solar cycle during the period 1997–2008 is carried out. A sample of 229 events from our recent work is used for the present study (Vasanth and Umapathy, 2013). The collected events are divided into two groups as (i) solar cycle rise phase events and (ii) solar cycle decay phase events. The properties of CMEs in the two groups were compared and the results are presented. It is noted that there is no difference in the properties of type II burst like start frequency and end frequency between the solar cycle rise phase events and decay phase events. The mean CME speed of solar cycle decay phase events (1373？km？s？1) is slightly higher than the solar cycle rise phase events (1058？km？s？1). The mean CME acceleration of solar cycle decay phase events (？15.18？m？s？2) is found to be higher than that of the solar cycle rise phase events (？1.32？m？s？2). There exists good correlation between (i) CME speed and width and (ii) CME speed and acceleration for solar cycle decay phase events ( , ) compared to solar cycle rise phase events ( , ). These results indicate that the type II bursts parameters do not depend upon the time of appearance in the solar cycle. 1. Introduction Coronal mass ejections (CMEs) are the large eruption of magnetized plasma from sun into heliosphere and are important cause for geomagnetic storms if they are directed towards earth. The shocks driven by the CMEs accelerate electrons and produce type II bursts in the corona and interplanetary medium (IP) [1]. Type II bursts are the longest known signatures of shock wave [2]. In the dynamic spectrum they are observed as slowly drifting (from high to low frequency) emission bands. The first identification of type II bursts was made by Payne-Scott et al. [3] and later Wild and McCready [2] classified them as type II bursts to differentiate them from fast drifting type III bursts. The first observation of type II bursts in the IP medium was made by IMP-6 [4] and Voyager [5] spacecraft missions. Many IP type II bursts are observed by ISEE-3 spacecraft in the frequency range of 2？MHz to 30？kHz [6, 7]. The data on DH-type II bursts are provided by radio and plasma wave (WAVES) experiment on board wind spacecraft launched in 1994 [8]. The wind spacecraft observes the type II/IV radio bursts in the frequency range between 14？MHz and 20？kHz by RAD1 and RAD2 due to ionospheric cut-off frequency [9–11]. The frequency range in the decameter hectometric (DH) wavelength domain corresponds to the heights of 2–10？
References
[1]
M. J. Reiner, “High-frequency Type II radio emissions associated with shocks driven by coronal mass ejections,” Journal of Geophysical Research A: Space Physics, vol. 104, no. 8, pp. 16979–16991, 1999.
[2]
J. P. Wild and L. L. McCready, “Observations of the spectrum of high intensity solar radiations at metrewavelengths,” Australian Journal of Scientific Research A, vol. 3, no. 4, pp. 541–557, 1950.
[3]
R. Payne-Scott, D. E. Yabsley, and J. G. Bolton, “Relative times of arrival of bursts of solar noise on different radio frequencies,” Nature, vol. 160, no. 4060, pp. 256–257, 1947.
[4]
H. H. Malitson, J. Fainberg, and R. G. Stone, “Observation of a Type II solar radio burst to 37 Rsun,” Astrophysical Journal, vol. 14, pp. 111–114, 1973.
[5]
A. Boischot, A. C. Riddle, J. B. Pearce, and J. W. Warwick, “Shock waves and Type II radiobursts in the interplanetary medium,” Solar Physics, vol. 65, no. 2, pp. 397–404, 1980.
[6]
H. V. Cane, N. R. Sheeley, and R. A. Howard, “Energetic interplanetary shocks, radio emission, and coronal mass ejections,” Journal of Geophysical Research, vol. 92, no. 9, pp. 9869–9874, 1987.
[7]
D. Lengyel-Frey and R. G. Stone, “Characteristics of interplanetary Type II radio emission and the relationship to shock and plasma properties,” Journal of Geophysical Research, vol. 94, no. 1, pp. 159–167, 1989.
[8]
J.-L. Bougeret, M. L. Kaiser, P. J. Kellogg et al., “WAVES: the radio and plasma wave investigation on the wind spacecraft,” Space Science Reviews, vol. 71, no. 1–4, pp. 231–263, 1995.
[9]
M. L. Kaiser, M. J. Reiner, N. Gopalswamy et al., “Type II radio emissions in the frequency range from 1–？MHz associated with the April 7, 1997 solar event,” Geophysical Research Letters, vol. 25, no. 14, pp. 2501–2504, 1998.
[10]
M. J. Reiner, M. L. Kaiser, J. Fainberg, J.-L. Bougeret, and R. G. Stone, “On the origin of radio emissions associated with the January 6–11, 1997, CME,” Geophysical Research Letters, vol. 25, no. 14, pp. 2493–2496, 1998.
[11]
V. Vasanth, S. Umapathy, B. Vr？nak, and M. Anna Lakshmi, “Characteristics of Type-II radio bursts associated with flares and CMEs,” Solar Physics, vol. 273, no. 1, pp. 143–162, 2011.
[12]
N. Gopalswamy, S. Yashiro, M. L. Kaiser, R. A. Howard, and J.-L. Bougeret, “Characteristics of coronal mass ejections associated with long-wavelength Type II radio bursts,” Journal of Geophysical Research A: Space Physics, vol. 106, no. 12, pp. 29219–29229, 2001.
[13]
B. Vr？nak and E. W. Cliver, “Origin of coronal shock waves: iIInvited review,” Solar Physics, vol. 253, no. 1-2, pp. 215–235, 2008.
[14]
J. Magdaleni？, B. Vr？nak, S. Pohjolainen, M. Temmer, H. Aurass, and N. J. Lehtinen, “A flare-generated shock during a coronal mass ejection on 24 December 1996,” Solar Physics, vol. 253, no. 1-2, pp. 305–317, 2008.
[15]
A. Nindos, C. E. Alissandrakis, A. Hillaris, and P. Preka-Papadema, “On the relationship of shock waves to flares and coronal mass ejections,” Astronomy and Astrophysics, vol. 531, article A31, 12 pages, 2011.
[16]
A. Lara, N. Gopalswamy, S. Nunes, G. Munoz, and S. Yashiro, “A statistical study of CMEs associated with metric Type II bursts,” Geophysical Research Letters, vol. 30, no. 12, pp. SEP 4-1–SEP 4-4, 2003.
[17]
N. Gopalswamy, A. Lara, R. P. Lepping, M. L. Kaiser, D. Berdichevsky, and O. C. St. Cyr, “Interplanetary acceleration of coronal mass ejections,” Geophysical Research Letters, vol. 27, no. 2, pp. 145–148, 2000.
[18]
V. Vasanth and S. Umapathy, “A statistical study on CMEs associated with DH-Type-II radio bursts based on their source location (limb and disk events),” Solar Physics, vol. 282, no. 1, pp. 239–247, 2013.
[19]
V. Vasanth and S. Umapathy, “A statistical study on DH CMEs and its geo-effectiveness,” ISRN Astronomy and Astrophysics, vol. 2013, Article ID 129426, 13 pages, 2013.
[20]
N. Gopalswamy, S. Yashiro, G. Michalek et al., “The SOHO/LASCO CME catalog,” Earth, Moon and Planets, vol. 104, no. 1–4, pp. 295–313, 2009.
[21]
S. Yashiro, N. Gopalswamy, G. Michalek et al., “A catalog of white light coronal mass ejections observed by the SOHO spacecraft,” Journal of Geophysical Research A: Space Physics, vol. 109, no. 7, article 105, 2004.
[22]
G. E. Brueckner, J.-P. Delaboudiniere, R. A. Howard et al., “Geomagnetic storms caused by coronal mass ejections (CMEs): March 1996 through June 1997,” Geophysical Research Letters, vol. 25, no. 15, pp. L3019–L3022, 1998.
[23]
N. Gopalswamy, E. Aguilar-Rodriguez, S. Yashiro, S. Nunes, M. L. Kaiser, and R. A. Howard, “Type II radio bursts and energetic solar eruptions,” Journal of Geophysical Research A: Space Physics, vol. 110, no. 12, article S07, 2005.
[24]
N. Gopalswamy, “Coronal mass ejections and Type II bursts,” in Solar Eruptions and Energetic Particles, N. Gopalswamy, R. Mewaldt, and J. Torsti, Eds., vol. 165 of Geophysical Monograph Series, p. 207, 2006.
[25]
Y. Leblanc, G. A. Dulk, and J.-L. Bougeret, “Tracing the electron density from the corona to 1 AU,” Solar Physics, vol. 183, no. 1, pp. 165–180, 1998.
[26]
N. Gopalswamy, W. T. Thompson, J. M. Davila et al., “Relation between Type II bursts and CMEs inferred from STEREO observations,” Solar Physics, vol. 259, no. 1-2, pp. 227–254, 2009.
[27]
B. Vr？nak, J. Magdaleni？, and H. Aurass, “Comparative analysis of Type II bursts and of thermal and non-thermal flare signatures,” Solar Physics, vol. 202, no. 2, pp. 319–335, 2001.
[28]
B. Vr？nak, “Processes and mechanisms governing the initiation and propagation of CMEs,” Annales Geophysicae, vol. 26, no. 10, pp. 3089–3101, 2008.
[29]
J. T. Gosling, E. Hildner, R. M. MacQueen, R. H. Munro, A. I. Poland, and C. L. Ross, “The speeds of coronal mass ejection events,” Solar Physics, vol. 48, no. 2, pp. 389–397, 1976.
[30]
Y.-J. Moon, G. S. Choe, H. Wang et al., “A statistical study of two classes of coronal mass ejections,” Astrophysical Journal Letters, vol. 581, no. 1, pp. 694–702, 2002.
[31]
B. Vr？nak, “Deceleration of coronal mass ejections,” Solar Physics, vol. 202, no. 1, pp. 173–189, 2001.
