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Filaments disappearance in relation to coronal mass ejections during the solar cycle 23
Accepted Manuscript Filaments Disappearance in Relation to Coronal Mass Ejections during the Solar Cycle 23 R. Mawad, Mosalam Shaltout, M. Yousef, S. Yousef, M. Ewaida PII: DOI: Reference:
S0273-1177(14)00692-9 http://dx.doi.org/10.1016/j.asr.2014.11.002 JASR 12016
To appear in:
Advances in Space Research
Received Date: Revised Date: Accepted Date:
25 November 2013 4 October 2014 4 November 2014
Please cite this article as: Mawad, R., Shaltout, M., Yousef, M., Yousef, S., Ewaida, M., Filaments Disappearance in Relation to Coronal Mass Ejections during the Solar Cycle 23, Advances in Space Research (2014), doi: http:// dx.doi.org/10.1016/j.asr.2014.11.002
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Filaments Disappearance in Relation to Coronal Mass Ejections during the Solar Cycle 23 R. Mawad1,3 , Mosalam Shaltout2, M. Yousef3, S. Yousef4 and M. Ewaida5 1. Astronomy & Meteorology Department, Faculty of Science, Al-Azhar University, Egypt 2. National Research Institute of Astronomy and Geophysics, Helwan, Egypt 3. Space Weather Monitoring Center, Physics Dept., Helwan University, Egypt 4. Astronomy Department, Cairo University, Faculty of Science, Egypt 5. Physics Department, Faculty of Science, Menofia University, Egypt (Correspondence to: [email protected]) ABSTRACT: We have studied the relationship between filament disappearances with CMEs during solar period 1996-2010. We used the observed disappearing filaments in Hα data from Meudon given in NOAA, and coronal mass ejections data (CMEs) from SOHO/LASCO. We obtained 278 CME events (14%) contemporary filament disappearances and CME ejections (from a total of 2018 filament disappearance events and 15,874 CME events during 19962010). We found that the number of associated CME-Filament Disappearance events increased with the increase of the solar activity and significantly decreased with quiet sun. The longer filament disappearances have activity and ability to contemporary association with CMEs more than shorter filament disappearances. The filament disappearance powers the associated CMEs. CMEs which are associated with filament disappearance are ejected with higher speeds, massive, more energetic, and smaller angular width compared to non-associated CME events. In addition, the associated filament disappearance CMEs have two types depending on their duration; short-lived (<9 hours), and long-lived (>9 hours). Keywords: Filament, Filament Disappearance, Coronal Mass Ejection, CME. 1 Introduction: Filaments and prominences refer to the same physical structures on the Sun, either projected onto the disk or extended above the solar limb. The majority of the previous statistical studies regarded the connection between filament (or prominence) eruptions and CMEs have focused on prominences because they could easily be detected, observed, and measured against the dark sky background. Many studies show that the disappearances of prominences/filaments are often associated with Coronal Mass Ejections (CMEs) (Webb and Hundhausen, 1987). The Catalogue of Solar Filament Disappearances 1964-1980 (Wright, 1991) offered the most useful data set to investigate whether quiescent filaments (disparition brusques, DBs), However, although the connection between DBs and CMEs is clearly demonstrated in individual cases (e.g. Schmieder et al., 2000), conflicting overall conclusions are obtained for the correspondence between these two phenomena: from a nearly one-to-one (Gilbert et al., 2000) to a poor correlation (Yang and Wang, 2000). During the lifetime of prominences/filaments, incidents may occur that lead to the sudden disappearance of the prominence, a phenomenon also called “disparition brusque” (DB). This sometimes violent event results from instability of the prominence structure, and takes place on a very short time-scale (from a few minutes to several hours). In some cases, it is followed by a reappearance of the prominence at the same location. Many studies show that the disappearances of prominences / filaments are often associated with Coronal Mass Ejections (Pojoga and Huang, 2003). Yang and Wang, (2001) compared the data of filament and prominence disappearances which are observed from Big Bear Solar Observatory Hα full disk images observed between January 1997 and June 1999 (431 filament and prominence disappearance events), and CME data from LASCO aboard Solar and Heliospheric Observatory (SOHO), they found that most of filament disappearances seem to have no corresponding CME events. Even for the limb events, only 10 to 30% (very low) filament disappearances are associated with CMEs.
Yang and Wang (2001) found that there are three possible reasons: (1) They did not make a distinct between the thermal filament disappearance and the filament eruptions. Even for filament eruptions, only the dynamic filament eruptions might cause CMEs (Mouradian et. al, 1995). (2) It is possible that some filament disappearances on the disk might be associated with very weak halo CMEs which are difficult to be detected. (3) They recently noticed that some erupting filaments come back to the sun, if they have no continuous acceleration and their speeds are lower than the escaping speed of the gravity of the sun. Different types of prominence activity that are often referred to as disappearances, and these types may have a different relationship with CMEs. Detailed studies of individual events (Pettit, Edison 1943, Mouradian and SoruEscaut 1989, Tonooka et al. 2000) clearly indicate that there are different scenarios that lead to the same result: the disappearance of the prominence or filament. In many cases, the actual eruption of the prominence takes place, while in other situations the prominence vanishes with no portion of it appearing to escape from the Sun. Few studies that investigate the DB-CME correspondence take into account the specific type of disappearance (often for a limited number of well-observed events), many other broader studies do not consider such differentiation (Yang and Wang, 2000) and (Pojoga et. al., 2003). Moreover, CMEs, associated with the prominences, are not difficult to detect. Many classifications of prominence have been proposed in the past. Gilbert et al. (2000) developed definitions of active prominences (APs) and eruptive prominences (EPs) and studied the relationship between APs, EPs, and CMEs for 54 events. They found that 94% of the EPs had an association with CMEs compared to only 46% for APs. Gopalswamy et al. (2003) defined a prominence as a radial or a transverse event. They showed that the radial events have a strong correlation to the CMEs, 83% of the radial events were associated with CMEs compared to 24% for transverse events (Ju Jing, et. al., 2004). Filaments are thin condensed sheets of chromospheric material located in the low corona. They are suspended above neutral lines between two opposite magnetic polarities. Their temperature and density are two orders of magnitudes smaller and greater than that of the ambient corona respectively. When observed in Hα, they appear as dark ribbons against the chromosphere. When they appear on the limb, they are bright features and are called prominence. Some filaments and prominences end their existence by eruption (Yang and Wang, 2001). (ojoga and Huang (2003) classified the filament disappearances to three classes: eruptive, quasi-eruptive and vanishing filaments. They Studied the Sudden disappearances of prominences/filaments as identified from the Prairie View Solar Observatory Hα images and Meudon Observatory spectroheliograms for the period January 1, 2000 to March 31, 2000. The Hα events were compared with CME data from LASCO C2 and C3 coronagraphs aboard SOHO. Their study shows that the eruptive events are strongly associated with CMEs while the other types are not. The disappearance of filament event of September 26, 1997 was detected by LASCO C2 and EIT. By the end of the next day, this filament disappearance resulted in a halo CME. From northwest on 2003 February 18, with a LASCO and EIT combined image, a filament with more substantial thickness and length was seen in the northern hemisphere and slightly to the west on February 17 in the BBSO Hα image. The disappearance of this filament the next day accompanied the limb CME at 02:42 (Feynman and Ruzmaikin, 2006). LASCO coronagraph images can only detect apparent speeds and widths of the CMEs since the images are twodimensional projections of the white light emission on the plane of the sky (POS). The three dimensional structure and actual speed of CMEs remain unknown due to the projection ambiguity (Xie et al., 2004). some authors prefer to studying the `solar mass ejection' (SME), rather than `coronal mass ejection' (CME), because the origin and
2
evolution of transient events in the solar atmosphere is not yet known from current white-light coronagraph observations and in situ solar wind measurements (Bothmer and Schwenn, 1998). The Catalogue of Solar Filament Disappearances 1964-1980 (Wright, 1991) offered us the most useful data set to investigate whether Quiescent filaments (disparition brusques, DBs) and MCs can be associated and related their magnetic structures (Bothmer, 1993; Rust, 1994). The solar latitude of the filaments was ~30-60°. Nine of MCs cases identified in Helios and near Earth solar wind data to be uniquely associated with quiescent filament disappearances (DBs) at mid to high solar latitudes outside active regions. In eight of the nine cases was found agreement between the magnetic flux tube structure of the MC and that of the associated filament as inferred from the orientation of the filament axis and its magnetic polarity, on the assumption of left-handed (right-handed) magnetic helicity dominance of filaments in the northern (southern) solar hemisphere (Bothmer and Schwenn, 1998). Normal velocity CMEs are categorized as being associated with either a flare or a disappearing filament whereas extreme velocity CMEs are typically associated with both a flare and a filament eruption. Normal velocity CMEs associated with filament disappearances typically show constant acceleration in the corona, whereas those associated with flares usually show a constant speed or decreasing speed (Sheeley et al. 1999; Andrews & Howard 2001; Moon et al. 2002). Extremely fast CMEs (v > 1500 km/sec) are as likely to show constant acceleration as constant or decreasing speed (Feynman & Ruzmaikin 2004). Constantin, et. al. (2007) studied a complex filament composed by a main body (a huge polar filament), and a tail (a small filament situated between active regions) was observed between 6 and 14 January 2001. They have analyzed its dynamics. The tail suffered a thermal sudden disappearance and reappeared after two days. A decaying active region plays the role of attractor for the complex filament. A spectacular CME, produced after a helical up-awarded movement of plasma, movement observed in the coronal loops of the main body of the filament during three days before the CME onset. They have analyzed also the CME shape and movement using SOHO data. We will develop our study of the association between filament disappearances and CMEs to be differing from previous studies by the following items:
Studying the association between filament disappearances and CMEs during a time interval (from 1996 to 2010).
Measuring the location of CME is very important for better accuracy than the previous studies. Temporal and spatial conditions are used to select the filament Disappearance-CME associated events.
Assuming the simultaneous association of filament disappearances with CMEs when CMEs are ejected during the disappearing times of filaments.
2
Working Method: For selecting the filament Disappearance-CME associated events, we used the following conditions:-
2.1 The Temporal Condition: We put the criteria that the CME time must be within filament disappearance time: Fstart < CMEt < Fend Where CMEt is the CME ejection
(1)
time, Fstart is the filament disappearance start time, and Fend is the filament
disappearance end time (Musalam Shaltout and Mawad, R., 2006). 2.2 Spatial Condition: LASCO coronagraph images can only detect apparent speeds and widths of the CMEs since the images are twodimensional projections of the white light emission on the plane of the sky (POS). The three dimensional structure and actual speed of CMEs remain unknown due to the projection ambiguity (Xie et al., 2004). The Filament has solar latitude and central meridian (longitude), it is positioned in 3 dimensional coordinates (i.e. we have different
3
position coordinates). The selections of the CMEs which are ejected due to filament disappearance must have the same filament locations. It is our task now to make sure that both CMEs and the associated filaments have the same location. This can be done by two ways: [1] In the meanwhile, (Gopalswamy et al., 2001) reported that 11 out of 34 metric type II bursts from source longitudes <60º were not associated with LASCO CMEs, indicating approximately a third of CMEs originating from the disk center were invisible to LASCO. In addition, from the longitudinal variation of CME association with EIT waves (Biesecker et al., 2002; Cliver et al., 2005) estimated 40% of the CMEs from source longitudes <60º are invisible to LASCO. Different visibilities have been reported in various studies, since the visibility would be different between energetic and average CMEs (S. Yashiro et al., 2005). Only 15% of disk C-class flares had associated CMEs. The limb flares had more CMEs (30%) since CMEs are most visible when they originate from the limb. The CME association rates for M-class flares are 43% for disk events and 51% for limb events. This association rate is similar to that of Andrews (2003), who reported 55% for M-class flares. The CME association rates for the flares between X1 and X3 levels are 91% for disk events and 82% for limb events (Yashiro et al., 2005). The CME association rates are 15% (12–18%) and 30% (24–36%) for the disk and limb events, respectively. The ratio indicates that 50% of disk CMEs were invisible with the assumption that all limb CMEs are visible (Yashiro et al., 2005). From Yashiro research we can neglect any filament that has longitude lesser than 60º, it is one method for solving our problem. [2] (B. Vrsňak et al., 2005), used the condition | (ΨCME – ΨF) | < Φ/4 (i.e. the location of the flare or filament is between middle quarter of the CME width). The second method is more accurate than the first method, but this method is more redirected (Mosalam Shaltout and Mawad, R., 2009), we have tested this method but it gives us very little Filament-CME associated list, and we cannot correlate it, we assuming the condition: | (ΨCME – ΨF) | < Φ/2
(2)
(i.e. the location of the filament is bounded by half of CME width). Now, we have to convert the longitude and latitude of the disappearing filament to position angle, it is the current problem. This can be done by converting the spherical coordinate (latitude and longitude) of filament to plane coordinate (position angle) in order to match the CME plane images. We use the spherical triangle of the heliocentric celestial coordinates. The F point is the Filament location on the solar sphere. The solar sphere is parallel to celestial sphere, N is the north pole of the ecliptic and north of the sun, P point is the north pole of the earth, β is the celestial latitude, λ is the ecliptic longitude, Ψ CME is the position angle which we need to calculate. Now we want to convert the sphere of the sun to plan disk, to simulate it such as viewing the disk of the sun. The FPN angle must be 90°, from the spherical triangle NPF we can use the cos-cos formula to determine the ΨCME, then: Cos ΨF Cos (90°-λ) = Sin ΨF Cot (90° –β) – Sin(90° -λ) Cot 90° Cos ΨF sin λ = sin ΨF Tan β
4
Then: ΨF=Tan-1[ sin λ / tan β]
(3)
From this formula we can calculate the position angle of the disappearing filament from its latitude and longitude as shown in disk or flat plane (2-dimensions) (Mosalam Shaltout and Mawad, R., 2009). Then the spatial condition is: | (ΨCME – Ψ F ) | < Φ/2 , In the case of a filament consisting of several sections then: | (ΨCME – Ψ F1 ) | < Φ/2 , | (ΨCME – Ψ F2 ) | < Φ/2 , | (ΨCME – Ψ F3 ) | < Φ/2 , ΨF1 < ΨCME < ΨF2 , ΨF2 < ΨCME < ΨF3 , or ΨF1 < ΨCME < ΨF3 ,
(4)
Where ΨF1 , ΨF2 and Ψ F3 are the position angles of three locations of the filament disappearances, and Φ is the angular width of CME. 3 Data Sources: We selected the sudden filament disappearance from Meudon as given by National Geophysical Data Center (NOAA) available on URL: ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SOLAR_FILAMENTS/ While the CMEs data are obtained from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) mission existing on URL: http://cdaw.gsfc.nasa.gov/CME_list/. The initial CME sample consists of 15,874 events are observed by SOHO/LASCO, and 1993 filament disappearance events are observed from NOAA, during the period 1996-2010. The filament data have the field: time, locations, importance, radial extent, blue and shift. While the CME data have the fields: time, position angle, angular width, linear speed, initial speed, final speed, speed at 20Rsun, acceleration, mass, and kinetic energy. We have selected the disappearing filaments (DSF) from all data list (8854 filaments). The results are compiled in table 3. 4
Results and Discussions
4.1 Listing the CME-Filament Disappearance According to the above conditions (1) and (2), we obtained 278 events (14%) simultaneous with the filament disappearances and ejected from same location, from total 2018 Filament Disappearance events (23%) from total filaments 8854 and 15,874 CME events during 1996-2010, these details are given in table 1. Table: 1: Counts of Filament Disappearances All Disappearances Associated with CME
5
1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 Total Ratio
107 112 237 204 318 296 207 247 92 65 70 7 9 6 41 2018 23% of total filaments
4 4 12 30 56 56 39 40 13 8 7 1 1 0 7 278 14% of total disappearance
We plot the result of table 1 in fig. 3 for two cases: count all filament disappearances, and associated simultaneous CME events. From figure 1, we showed that the associated events have the same curve behavior of all filament disappearance. We found that the number of the associated events increased with the increase of the solar activity and decreased with quiet sun. This is result gives us an indication that there is a strong correlation between CMEs and filament disappearances which are selected by using our conditions. 4.2 Annual Number of Associated events: The plot in figure 2, represent the relationship between annual numbers of filament disappearances with annual numbers of associated CMEs during 1996-2010. We found a strong correlation (R=0.90) between the both annual numbers. Pervious statistical studies of DBs show that about 30% of filament or prominence disappearances are not associated with CMEs (Pojoga and Huang, 2003; Gopalswamy et al., 2003). Yang and Wang (2001) found that most of filament disappearances seem to have no corresponding CME events, Even for the limb events, only 10 to 30% (very low) filament disappearances are associated with CMEs. 4.3
The characteristics of CME-Filament Disappearance
4.3.1 Disappearance Duration of Filaments The Histogram in figure 3, represent the duration of the filament disappearances which is associated with CMEs, we found that most of filament disappearances which are associated with CMEs have duration more than nine hours, with a maximum duration of 15 hours, can eject CMEs while disappearing, and a little filament disappearance events located in the histogram having duration litter than nine hours. the count of the short duration group decayed as the duration of filament disappearance increase. On the other hand, the second long duration category shows a normal distribution with a maximum at 15 hours. The duration of filament disappearance which is associated with CMEs can be classified into two groups: a)
Short-lived < 9 hours.
b)
Long-lived > 9 hours.
4.3.2 The Interval Time We plot the histogram of interval time between filament disappearance start time and CME ejection time and we found that the most events of CMEs occurred during the start stage of filament disappearances (as shown in figure 4), we found the best interval time < 13 hours. Taliashvili et al. (2008) studied two prominences and found that no CHs have been observed near these prominences, after 2h of DBs start time a CME was detected.
6
4.3.3 Filament Disappearance Locations The filament disappearances which are associated with CMEs mostly have two locations (figure 5), this indicate that the associated disappearance of filament events have length greater than 10 degrees. The latitude of filament disappearances is asymmetric with more filaments in the northern solar hemisphere. We found that the central meridians of filament disappearances which are associated with CMEs are approximately symmetric (figure 6 and 7). 4.3.4 CME Angular width From figure 8, we found that the angular width of all CME–filament disappearance associated events has a wide range between 20° and 150°, with the popular events ranged between 60° and 80°. 4.3.5 CME Linear Speed From figure 9 we found that most CME events have slow linear speed (~300Km/s), whoever in mean linear speed of associated CMEs (486 km/s) is faster than the none associated CMEs (408 km/s). All linear speed of CMEs is ranged between 100 and 700 km/s. Sheeley et al. (1999), Andrews & Howard (2001) and Moon et al. (2002) found that Normal velocity CMEs are categorized as being associated with either a flare or a disappearing filament whereas extreme velocity CMEs are typically associated with both a flare and a filament eruption. Normal velocity CMEs associated with filament disappearances typically show constant acceleration in the corona, whereas those associated with flares usually show a constant speed or decreasing speed. Extremely fast CMEs (v > 1500 km/sec) are as likely to show constant acceleration as constant or decreasing speed (Feynman & Ruzmaikin 2004). 4.3.6 CME Acceleration Most CME which are associated with filament disappearance have a small acceleration, The CMEs which are associated with filament disappearance (mean value ~ 5 m/s2) are accelerated more than none associated CME events (mean value ~ 2.5 m/s2). 4.3.7 CME Mass We show that the most CME events have a mass < 2 × 10ଵହ gram. The CME/filament disappearance associated events have a mean mass value of (1.7854431e+12 kg) greater than the mean mass value of none associated events (1.3014749e+12 kg). 4.3.8 CME Kinetic Energy We show that most CME events which are associated with filament disappearance have a kinetic energy < 2 × 10ଷଵ erg, while the mean kinetic energy value of (4.186306e+30 erg) is greater than the mean kinetic energy value of none associated events (2.1464794e+30 erg). 5 Conclusion We have studied the relationship between filament disappearances and CMEs during solar period 1996-2010, we used the observed disappearing filaments in Hα data from Meudon obtained from NOAA. There are 8854 records for filament disappearances. We used the coronal mass ejections data (CMEs) from SOHO/LASCO satellite. The initial CME sample consists of 15,874 events, during the period 1996-2010. We obtained 278 events (14%) simultaneous filament disappearances and CME ejections from the same location (from a total of 2018 Filament Disappearance events and 15,874 CME events during 1996-2010), the details are given in table 1. We found that the correlation coefficient between disappearing filaments and CMEs increase with solar activity, the associated events have the same curve behavior of all filament disappearance, the associated events increased with the increase of the solar activity and significantly decreased with quiet sun. This result gives us an indication that there is a strong correlation between CMEs and filament disappearances cases selected by using our conditions, whoever
7
some CMEs events may be ejected during decay stage of the filament disappearance. The filament disappearances which are associated with CMEs mostly have two locations, this indicates that the associated disappearance of filament events have a length greater than 10 degrees. The latitude of filament disappearances is asymmetric with more filaments in the northern solar hemisphere, the central meridians of associated filament disappearances are approximately symmetric. The CMEs which are simultaneously with filament disappearance have a smaller angular width, and larger acceleration, velocity, and mass than none associated CMEs. The angular width of associated CME events with filament disappearance has a wide range between 20° and 150°, with the popular events ranged between 60° and 80°. Also, most CME events have slow linear speed (~300Km/s), mean linear speed of associated CMEs (486 km/s) is faster than none associated CMEs (408 km/s), all linear speed of CMEs ranged between 100 and 700 km/s. while most CMEs which are associated with filament disappearance have a small acceleration, The CMEs which are associated with filament disappearance (mean value ~ 5 m/s2) are accelerated more than none associated CME events (mean value ~ 2.5 m/s2), we show that most CME events have a mass < 2 × 10ଵହ gram, The CME/filament disappearance associated events have a mean mass value of (1.7854431e+12 kg) greater than the mean mass value of none associated events 1.3014749 × 10ଵଶ kg, most associated CME events have a kinetic energy < 2 × 10ଷଵ erg, while the mean kinetic energy value of 4.186306 × 10ଷ erg is greater than the mean kinetic energy value of none associated events 2.1464794 × 10ଷ erg. Table 2: summarizes our conclusions PA Width Accel
Mean value
Mass
Energy
None Associated CME
177.51
44.90
2.47
1.30e+15
2.15e+30
Associated CME
50.70
85.26
4.94
1.78e+15
4.19e+30
6 •
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Filament Disappearance events during 1996-2010 350 All Disappearances Associated
300
Count of events
250 200 150 100 50 0 -50 1996
1998
2000
2002
2004
2006
2008
2010
Year
Fig. 1: Counts of all filament disappearances (Solid line) and the associated events with CMEs (dashed line) during 1996-2010.
11
Relationship between annual count of filament disappearance and associated annual CME counts Annual count of Associated Filament Disappearances
350 y = 45.025 + 4.8296x R= 0.90101 300
250
200
150
100
50
0 0
10
20
30
40
50
60
Annual Count of Associated CMEs
Fig. 2: The relationship between annual counts of all filament disappearances with annual counts of associated filament disappearance with CMEs during 1996-2010.
12
Histogram of Disappearance Duration of Filaments 30
25
Count of events
20
15
10
5
0 0
2
4
6
8
10
12
14
16
18
20
22
24
Disappearance Duration of Filament (Hour)
Fig. 3: Histogram of disappearance Duration of filaments during 1996-2010.
13
Histogram of Interval between Filament Disappearance start time and CME time 25
Count of events
20
15
10
5
0 0
2
4
6
8
10
12
14
16
18
Interval (hour)
Fig. 4: Histogram of interval between start time of filament disappearance and CME time during 19962010.
14
Associated CME events with filament disappearance 200
Count of events
150
100
50
0 1
2
3
Locations
Fig. 5: Histogram of locations of filament disappearance which are associated with CMEs during 1996-2010.
15
Histogram of Filament disappearances Latitudes of three locations during 1996-2010 60 Latitude of Location 1 Latitude of location 2 Latitude of location 3
50
Count of events
40
30
20
10
0 -80
-60
-40
-20
0
20
40
60
80
100
Latitude
Fig. 6: Histogram of filament disappearance latitudes of three locations during 1996-2010.
16
Central Meridian of Location 1 Central Meridian of Location 3 Central Meridian of Location 2
Histogram of Central Meredian 40 35 30
Count
25 20 15 10 5 0 -80
-60
-40
-20
0
20
40
60
80
100
Range
Fig. 7: Histogram of filament disappearance central meridian of three locations during 1996-2010.
17
Histogram of CME Angular Width 30
25
Count of events
20
15
10
5
0 10
30
50
70
90
110
130
150
170
190
210
CME Angular Width (Degree)
Fig. 8: Histogram of angular width of CMEs which are associated with filament disappearance during 1996-2010.
18
Histogram of Linear Speed 40 35
Count of events
30 25 20 15 10 5 0 0
200
400
600
800
1000 1200 1400 1600 1800
CME Linear Speed (Km/s)
Fig. 9: Histogram of linear speed of CMEs which are associated with filament disappearance during 1996-2010.
19
S0273-1177(14)00692-9 http://dx.doi.org/10.1016/j.asr.2014.11.002 JASR 12016
To appear in:
Advances in Space Research
Received Date: Revised Date: Accepted Date:
25 November 2013 4 October 2014 4 November 2014
Please cite this article as: Mawad, R., Shaltout, M., Yousef, M., Yousef, S., Ewaida, M., Filaments Disappearance in Relation to Coronal Mass Ejections during the Solar Cycle 23, Advances in Space Research (2014), doi: http:// dx.doi.org/10.1016/j.asr.2014.11.002
This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain.
Filaments Disappearance in Relation to Coronal Mass Ejections during the Solar Cycle 23 R. Mawad1,3 , Mosalam Shaltout2, M. Yousef3, S. Yousef4 and M. Ewaida5 1. Astronomy & Meteorology Department, Faculty of Science, Al-Azhar University, Egypt 2. National Research Institute of Astronomy and Geophysics, Helwan, Egypt 3. Space Weather Monitoring Center, Physics Dept., Helwan University, Egypt 4. Astronomy Department, Cairo University, Faculty of Science, Egypt 5. Physics Department, Faculty of Science, Menofia University, Egypt (Correspondence to: [email protected]) ABSTRACT: We have studied the relationship between filament disappearances with CMEs during solar period 1996-2010. We used the observed disappearing filaments in Hα data from Meudon given in NOAA, and coronal mass ejections data (CMEs) from SOHO/LASCO. We obtained 278 CME events (14%) contemporary filament disappearances and CME ejections (from a total of 2018 filament disappearance events and 15,874 CME events during 19962010). We found that the number of associated CME-Filament Disappearance events increased with the increase of the solar activity and significantly decreased with quiet sun. The longer filament disappearances have activity and ability to contemporary association with CMEs more than shorter filament disappearances. The filament disappearance powers the associated CMEs. CMEs which are associated with filament disappearance are ejected with higher speeds, massive, more energetic, and smaller angular width compared to non-associated CME events. In addition, the associated filament disappearance CMEs have two types depending on their duration; short-lived (<9 hours), and long-lived (>9 hours). Keywords: Filament, Filament Disappearance, Coronal Mass Ejection, CME. 1 Introduction: Filaments and prominences refer to the same physical structures on the Sun, either projected onto the disk or extended above the solar limb. The majority of the previous statistical studies regarded the connection between filament (or prominence) eruptions and CMEs have focused on prominences because they could easily be detected, observed, and measured against the dark sky background. Many studies show that the disappearances of prominences/filaments are often associated with Coronal Mass Ejections (CMEs) (Webb and Hundhausen, 1987). The Catalogue of Solar Filament Disappearances 1964-1980 (Wright, 1991) offered the most useful data set to investigate whether quiescent filaments (disparition brusques, DBs), However, although the connection between DBs and CMEs is clearly demonstrated in individual cases (e.g. Schmieder et al., 2000), conflicting overall conclusions are obtained for the correspondence between these two phenomena: from a nearly one-to-one (Gilbert et al., 2000) to a poor correlation (Yang and Wang, 2000). During the lifetime of prominences/filaments, incidents may occur that lead to the sudden disappearance of the prominence, a phenomenon also called “disparition brusque” (DB). This sometimes violent event results from instability of the prominence structure, and takes place on a very short time-scale (from a few minutes to several hours). In some cases, it is followed by a reappearance of the prominence at the same location. Many studies show that the disappearances of prominences / filaments are often associated with Coronal Mass Ejections (Pojoga and Huang, 2003). Yang and Wang, (2001) compared the data of filament and prominence disappearances which are observed from Big Bear Solar Observatory Hα full disk images observed between January 1997 and June 1999 (431 filament and prominence disappearance events), and CME data from LASCO aboard Solar and Heliospheric Observatory (SOHO), they found that most of filament disappearances seem to have no corresponding CME events. Even for the limb events, only 10 to 30% (very low) filament disappearances are associated with CMEs.
Yang and Wang (2001) found that there are three possible reasons: (1) They did not make a distinct between the thermal filament disappearance and the filament eruptions. Even for filament eruptions, only the dynamic filament eruptions might cause CMEs (Mouradian et. al, 1995). (2) It is possible that some filament disappearances on the disk might be associated with very weak halo CMEs which are difficult to be detected. (3) They recently noticed that some erupting filaments come back to the sun, if they have no continuous acceleration and their speeds are lower than the escaping speed of the gravity of the sun. Different types of prominence activity that are often referred to as disappearances, and these types may have a different relationship with CMEs. Detailed studies of individual events (Pettit, Edison 1943, Mouradian and SoruEscaut 1989, Tonooka et al. 2000) clearly indicate that there are different scenarios that lead to the same result: the disappearance of the prominence or filament. In many cases, the actual eruption of the prominence takes place, while in other situations the prominence vanishes with no portion of it appearing to escape from the Sun. Few studies that investigate the DB-CME correspondence take into account the specific type of disappearance (often for a limited number of well-observed events), many other broader studies do not consider such differentiation (Yang and Wang, 2000) and (Pojoga et. al., 2003). Moreover, CMEs, associated with the prominences, are not difficult to detect. Many classifications of prominence have been proposed in the past. Gilbert et al. (2000) developed definitions of active prominences (APs) and eruptive prominences (EPs) and studied the relationship between APs, EPs, and CMEs for 54 events. They found that 94% of the EPs had an association with CMEs compared to only 46% for APs. Gopalswamy et al. (2003) defined a prominence as a radial or a transverse event. They showed that the radial events have a strong correlation to the CMEs, 83% of the radial events were associated with CMEs compared to 24% for transverse events (Ju Jing, et. al., 2004). Filaments are thin condensed sheets of chromospheric material located in the low corona. They are suspended above neutral lines between two opposite magnetic polarities. Their temperature and density are two orders of magnitudes smaller and greater than that of the ambient corona respectively. When observed in Hα, they appear as dark ribbons against the chromosphere. When they appear on the limb, they are bright features and are called prominence. Some filaments and prominences end their existence by eruption (Yang and Wang, 2001). (ojoga and Huang (2003) classified the filament disappearances to three classes: eruptive, quasi-eruptive and vanishing filaments. They Studied the Sudden disappearances of prominences/filaments as identified from the Prairie View Solar Observatory Hα images and Meudon Observatory spectroheliograms for the period January 1, 2000 to March 31, 2000. The Hα events were compared with CME data from LASCO C2 and C3 coronagraphs aboard SOHO. Their study shows that the eruptive events are strongly associated with CMEs while the other types are not. The disappearance of filament event of September 26, 1997 was detected by LASCO C2 and EIT. By the end of the next day, this filament disappearance resulted in a halo CME. From northwest on 2003 February 18, with a LASCO and EIT combined image, a filament with more substantial thickness and length was seen in the northern hemisphere and slightly to the west on February 17 in the BBSO Hα image. The disappearance of this filament the next day accompanied the limb CME at 02:42 (Feynman and Ruzmaikin, 2006). LASCO coronagraph images can only detect apparent speeds and widths of the CMEs since the images are twodimensional projections of the white light emission on the plane of the sky (POS). The three dimensional structure and actual speed of CMEs remain unknown due to the projection ambiguity (Xie et al., 2004). some authors prefer to studying the `solar mass ejection' (SME), rather than `coronal mass ejection' (CME), because the origin and
2
evolution of transient events in the solar atmosphere is not yet known from current white-light coronagraph observations and in situ solar wind measurements (Bothmer and Schwenn, 1998). The Catalogue of Solar Filament Disappearances 1964-1980 (Wright, 1991) offered us the most useful data set to investigate whether Quiescent filaments (disparition brusques, DBs) and MCs can be associated and related their magnetic structures (Bothmer, 1993; Rust, 1994). The solar latitude of the filaments was ~30-60°. Nine of MCs cases identified in Helios and near Earth solar wind data to be uniquely associated with quiescent filament disappearances (DBs) at mid to high solar latitudes outside active regions. In eight of the nine cases was found agreement between the magnetic flux tube structure of the MC and that of the associated filament as inferred from the orientation of the filament axis and its magnetic polarity, on the assumption of left-handed (right-handed) magnetic helicity dominance of filaments in the northern (southern) solar hemisphere (Bothmer and Schwenn, 1998). Normal velocity CMEs are categorized as being associated with either a flare or a disappearing filament whereas extreme velocity CMEs are typically associated with both a flare and a filament eruption. Normal velocity CMEs associated with filament disappearances typically show constant acceleration in the corona, whereas those associated with flares usually show a constant speed or decreasing speed (Sheeley et al. 1999; Andrews & Howard 2001; Moon et al. 2002). Extremely fast CMEs (v > 1500 km/sec) are as likely to show constant acceleration as constant or decreasing speed (Feynman & Ruzmaikin 2004). Constantin, et. al. (2007) studied a complex filament composed by a main body (a huge polar filament), and a tail (a small filament situated between active regions) was observed between 6 and 14 January 2001. They have analyzed its dynamics. The tail suffered a thermal sudden disappearance and reappeared after two days. A decaying active region plays the role of attractor for the complex filament. A spectacular CME, produced after a helical up-awarded movement of plasma, movement observed in the coronal loops of the main body of the filament during three days before the CME onset. They have analyzed also the CME shape and movement using SOHO data. We will develop our study of the association between filament disappearances and CMEs to be differing from previous studies by the following items:
Studying the association between filament disappearances and CMEs during a time interval (from 1996 to 2010).
Measuring the location of CME is very important for better accuracy than the previous studies. Temporal and spatial conditions are used to select the filament Disappearance-CME associated events.
Assuming the simultaneous association of filament disappearances with CMEs when CMEs are ejected during the disappearing times of filaments.
2
Working Method: For selecting the filament Disappearance-CME associated events, we used the following conditions:-
2.1 The Temporal Condition: We put the criteria that the CME time must be within filament disappearance time: Fstart < CMEt < Fend Where CMEt is the CME ejection
(1)
time, Fstart is the filament disappearance start time, and Fend is the filament
disappearance end time (Musalam Shaltout and Mawad, R., 2006). 2.2 Spatial Condition: LASCO coronagraph images can only detect apparent speeds and widths of the CMEs since the images are twodimensional projections of the white light emission on the plane of the sky (POS). The three dimensional structure and actual speed of CMEs remain unknown due to the projection ambiguity (Xie et al., 2004). The Filament has solar latitude and central meridian (longitude), it is positioned in 3 dimensional coordinates (i.e. we have different
3
position coordinates). The selections of the CMEs which are ejected due to filament disappearance must have the same filament locations. It is our task now to make sure that both CMEs and the associated filaments have the same location. This can be done by two ways: [1] In the meanwhile, (Gopalswamy et al., 2001) reported that 11 out of 34 metric type II bursts from source longitudes <60º were not associated with LASCO CMEs, indicating approximately a third of CMEs originating from the disk center were invisible to LASCO. In addition, from the longitudinal variation of CME association with EIT waves (Biesecker et al., 2002; Cliver et al., 2005) estimated 40% of the CMEs from source longitudes <60º are invisible to LASCO. Different visibilities have been reported in various studies, since the visibility would be different between energetic and average CMEs (S. Yashiro et al., 2005). Only 15% of disk C-class flares had associated CMEs. The limb flares had more CMEs (30%) since CMEs are most visible when they originate from the limb. The CME association rates for M-class flares are 43% for disk events and 51% for limb events. This association rate is similar to that of Andrews (2003), who reported 55% for M-class flares. The CME association rates for the flares between X1 and X3 levels are 91% for disk events and 82% for limb events (Yashiro et al., 2005). The CME association rates are 15% (12–18%) and 30% (24–36%) for the disk and limb events, respectively. The ratio indicates that 50% of disk CMEs were invisible with the assumption that all limb CMEs are visible (Yashiro et al., 2005). From Yashiro research we can neglect any filament that has longitude lesser than 60º, it is one method for solving our problem. [2] (B. Vrsňak et al., 2005), used the condition | (ΨCME – ΨF) | < Φ/4 (i.e. the location of the flare or filament is between middle quarter of the CME width). The second method is more accurate than the first method, but this method is more redirected (Mosalam Shaltout and Mawad, R., 2009), we have tested this method but it gives us very little Filament-CME associated list, and we cannot correlate it, we assuming the condition: | (ΨCME – ΨF) | < Φ/2
(2)
(i.e. the location of the filament is bounded by half of CME width). Now, we have to convert the longitude and latitude of the disappearing filament to position angle, it is the current problem. This can be done by converting the spherical coordinate (latitude and longitude) of filament to plane coordinate (position angle) in order to match the CME plane images. We use the spherical triangle of the heliocentric celestial coordinates. The F point is the Filament location on the solar sphere. The solar sphere is parallel to celestial sphere, N is the north pole of the ecliptic and north of the sun, P point is the north pole of the earth, β is the celestial latitude, λ is the ecliptic longitude, Ψ CME is the position angle which we need to calculate. Now we want to convert the sphere of the sun to plan disk, to simulate it such as viewing the disk of the sun. The FPN angle must be 90°, from the spherical triangle NPF we can use the cos-cos formula to determine the ΨCME, then: Cos ΨF Cos (90°-λ) = Sin ΨF Cot (90° –β) – Sin(90° -λ) Cot 90° Cos ΨF sin λ = sin ΨF Tan β
4
Then: ΨF=Tan-1[ sin λ / tan β]
(3)
From this formula we can calculate the position angle of the disappearing filament from its latitude and longitude as shown in disk or flat plane (2-dimensions) (Mosalam Shaltout and Mawad, R., 2009). Then the spatial condition is: | (ΨCME – Ψ F ) | < Φ/2 , In the case of a filament consisting of several sections then: | (ΨCME – Ψ F1 ) | < Φ/2 , | (ΨCME – Ψ F2 ) | < Φ/2 , | (ΨCME – Ψ F3 ) | < Φ/2 , ΨF1 < ΨCME < ΨF2 , ΨF2 < ΨCME < ΨF3 , or ΨF1 < ΨCME < ΨF3 ,
(4)
Where ΨF1 , ΨF2 and Ψ F3 are the position angles of three locations of the filament disappearances, and Φ is the angular width of CME. 3 Data Sources: We selected the sudden filament disappearance from Meudon as given by National Geophysical Data Center (NOAA) available on URL: ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SOLAR_FILAMENTS/ While the CMEs data are obtained from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) mission existing on URL: http://cdaw.gsfc.nasa.gov/CME_list/. The initial CME sample consists of 15,874 events are observed by SOHO/LASCO, and 1993 filament disappearance events are observed from NOAA, during the period 1996-2010. The filament data have the field: time, locations, importance, radial extent, blue and shift. While the CME data have the fields: time, position angle, angular width, linear speed, initial speed, final speed, speed at 20Rsun, acceleration, mass, and kinetic energy. We have selected the disappearing filaments (DSF) from all data list (8854 filaments). The results are compiled in table 3. 4
Results and Discussions
4.1 Listing the CME-Filament Disappearance According to the above conditions (1) and (2), we obtained 278 events (14%) simultaneous with the filament disappearances and ejected from same location, from total 2018 Filament Disappearance events (23%) from total filaments 8854 and 15,874 CME events during 1996-2010, these details are given in table 1. Table: 1: Counts of Filament Disappearances All Disappearances Associated with CME
5
1996 1997 1998 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 Total Ratio
107 112 237 204 318 296 207 247 92 65 70 7 9 6 41 2018 23% of total filaments
4 4 12 30 56 56 39 40 13 8 7 1 1 0 7 278 14% of total disappearance
We plot the result of table 1 in fig. 3 for two cases: count all filament disappearances, and associated simultaneous CME events. From figure 1, we showed that the associated events have the same curve behavior of all filament disappearance. We found that the number of the associated events increased with the increase of the solar activity and decreased with quiet sun. This is result gives us an indication that there is a strong correlation between CMEs and filament disappearances which are selected by using our conditions. 4.2 Annual Number of Associated events: The plot in figure 2, represent the relationship between annual numbers of filament disappearances with annual numbers of associated CMEs during 1996-2010. We found a strong correlation (R=0.90) between the both annual numbers. Pervious statistical studies of DBs show that about 30% of filament or prominence disappearances are not associated with CMEs (Pojoga and Huang, 2003; Gopalswamy et al., 2003). Yang and Wang (2001) found that most of filament disappearances seem to have no corresponding CME events, Even for the limb events, only 10 to 30% (very low) filament disappearances are associated with CMEs. 4.3
The characteristics of CME-Filament Disappearance
4.3.1 Disappearance Duration of Filaments The Histogram in figure 3, represent the duration of the filament disappearances which is associated with CMEs, we found that most of filament disappearances which are associated with CMEs have duration more than nine hours, with a maximum duration of 15 hours, can eject CMEs while disappearing, and a little filament disappearance events located in the histogram having duration litter than nine hours. the count of the short duration group decayed as the duration of filament disappearance increase. On the other hand, the second long duration category shows a normal distribution with a maximum at 15 hours. The duration of filament disappearance which is associated with CMEs can be classified into two groups: a)
Short-lived < 9 hours.
b)
Long-lived > 9 hours.
4.3.2 The Interval Time We plot the histogram of interval time between filament disappearance start time and CME ejection time and we found that the most events of CMEs occurred during the start stage of filament disappearances (as shown in figure 4), we found the best interval time < 13 hours. Taliashvili et al. (2008) studied two prominences and found that no CHs have been observed near these prominences, after 2h of DBs start time a CME was detected.
6
4.3.3 Filament Disappearance Locations The filament disappearances which are associated with CMEs mostly have two locations (figure 5), this indicate that the associated disappearance of filament events have length greater than 10 degrees. The latitude of filament disappearances is asymmetric with more filaments in the northern solar hemisphere. We found that the central meridians of filament disappearances which are associated with CMEs are approximately symmetric (figure 6 and 7). 4.3.4 CME Angular width From figure 8, we found that the angular width of all CME–filament disappearance associated events has a wide range between 20° and 150°, with the popular events ranged between 60° and 80°. 4.3.5 CME Linear Speed From figure 9 we found that most CME events have slow linear speed (~300Km/s), whoever in mean linear speed of associated CMEs (486 km/s) is faster than the none associated CMEs (408 km/s). All linear speed of CMEs is ranged between 100 and 700 km/s. Sheeley et al. (1999), Andrews & Howard (2001) and Moon et al. (2002) found that Normal velocity CMEs are categorized as being associated with either a flare or a disappearing filament whereas extreme velocity CMEs are typically associated with both a flare and a filament eruption. Normal velocity CMEs associated with filament disappearances typically show constant acceleration in the corona, whereas those associated with flares usually show a constant speed or decreasing speed. Extremely fast CMEs (v > 1500 km/sec) are as likely to show constant acceleration as constant or decreasing speed (Feynman & Ruzmaikin 2004). 4.3.6 CME Acceleration Most CME which are associated with filament disappearance have a small acceleration, The CMEs which are associated with filament disappearance (mean value ~ 5 m/s2) are accelerated more than none associated CME events (mean value ~ 2.5 m/s2). 4.3.7 CME Mass We show that the most CME events have a mass < 2 × 10ଵହ gram. The CME/filament disappearance associated events have a mean mass value of (1.7854431e+12 kg) greater than the mean mass value of none associated events (1.3014749e+12 kg). 4.3.8 CME Kinetic Energy We show that most CME events which are associated with filament disappearance have a kinetic energy < 2 × 10ଷଵ erg, while the mean kinetic energy value of (4.186306e+30 erg) is greater than the mean kinetic energy value of none associated events (2.1464794e+30 erg). 5 Conclusion We have studied the relationship between filament disappearances and CMEs during solar period 1996-2010, we used the observed disappearing filaments in Hα data from Meudon obtained from NOAA. There are 8854 records for filament disappearances. We used the coronal mass ejections data (CMEs) from SOHO/LASCO satellite. The initial CME sample consists of 15,874 events, during the period 1996-2010. We obtained 278 events (14%) simultaneous filament disappearances and CME ejections from the same location (from a total of 2018 Filament Disappearance events and 15,874 CME events during 1996-2010), the details are given in table 1. We found that the correlation coefficient between disappearing filaments and CMEs increase with solar activity, the associated events have the same curve behavior of all filament disappearance, the associated events increased with the increase of the solar activity and significantly decreased with quiet sun. This result gives us an indication that there is a strong correlation between CMEs and filament disappearances cases selected by using our conditions, whoever
7
some CMEs events may be ejected during decay stage of the filament disappearance. The filament disappearances which are associated with CMEs mostly have two locations, this indicates that the associated disappearance of filament events have a length greater than 10 degrees. The latitude of filament disappearances is asymmetric with more filaments in the northern solar hemisphere, the central meridians of associated filament disappearances are approximately symmetric. The CMEs which are simultaneously with filament disappearance have a smaller angular width, and larger acceleration, velocity, and mass than none associated CMEs. The angular width of associated CME events with filament disappearance has a wide range between 20° and 150°, with the popular events ranged between 60° and 80°. Also, most CME events have slow linear speed (~300Km/s), mean linear speed of associated CMEs (486 km/s) is faster than none associated CMEs (408 km/s), all linear speed of CMEs ranged between 100 and 700 km/s. while most CMEs which are associated with filament disappearance have a small acceleration, The CMEs which are associated with filament disappearance (mean value ~ 5 m/s2) are accelerated more than none associated CME events (mean value ~ 2.5 m/s2), we show that most CME events have a mass < 2 × 10ଵହ gram, The CME/filament disappearance associated events have a mean mass value of (1.7854431e+12 kg) greater than the mean mass value of none associated events 1.3014749 × 10ଵଶ kg, most associated CME events have a kinetic energy < 2 × 10ଷଵ erg, while the mean kinetic energy value of 4.186306 × 10ଷ erg is greater than the mean kinetic energy value of none associated events 2.1464794 × 10ଷ erg. Table 2: summarizes our conclusions PA Width Accel
Mean value
Mass
Energy
None Associated CME
177.51
44.90
2.47
1.30e+15
2.15e+30
Associated CME
50.70
85.26
4.94
1.78e+15
4.19e+30
6 •
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Filament Disappearance events during 1996-2010 350 All Disappearances Associated
300
Count of events
250 200 150 100 50 0 -50 1996
1998
2000
2002
2004
2006
2008
2010
Year
Fig. 1: Counts of all filament disappearances (Solid line) and the associated events with CMEs (dashed line) during 1996-2010.
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Relationship between annual count of filament disappearance and associated annual CME counts Annual count of Associated Filament Disappearances
350 y = 45.025 + 4.8296x R= 0.90101 300
250
200
150
100
50
0 0
10
20
30
40
50
60
Annual Count of Associated CMEs
Fig. 2: The relationship between annual counts of all filament disappearances with annual counts of associated filament disappearance with CMEs during 1996-2010.
12
Histogram of Disappearance Duration of Filaments 30
25
Count of events
20
15
10
5
0 0
2
4
6
8
10
12
14
16
18
20
22
24
Disappearance Duration of Filament (Hour)
Fig. 3: Histogram of disappearance Duration of filaments during 1996-2010.
13
Histogram of Interval between Filament Disappearance start time and CME time 25
Count of events
20
15
10
5
0 0
2
4
6
8
10
12
14
16
18
Interval (hour)
Fig. 4: Histogram of interval between start time of filament disappearance and CME time during 19962010.
14
Associated CME events with filament disappearance 200
Count of events
150
100
50
0 1
2
3
Locations
Fig. 5: Histogram of locations of filament disappearance which are associated with CMEs during 1996-2010.
15
Histogram of Filament disappearances Latitudes of three locations during 1996-2010 60 Latitude of Location 1 Latitude of location 2 Latitude of location 3
50
Count of events
40
30
20
10
0 -80
-60
-40
-20
0
20
40
60
80
100
Latitude
Fig. 6: Histogram of filament disappearance latitudes of three locations during 1996-2010.
16
Central Meridian of Location 1 Central Meridian of Location 3 Central Meridian of Location 2
Histogram of Central Meredian 40 35 30
Count
25 20 15 10 5 0 -80
-60
-40
-20
0
20
40
60
80
100
Range
Fig. 7: Histogram of filament disappearance central meridian of three locations during 1996-2010.
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Histogram of CME Angular Width 30
25
Count of events
20
15
10
5
0 10
30
50
70
90
110
130
150
170
190
210
CME Angular Width (Degree)
Fig. 8: Histogram of angular width of CMEs which are associated with filament disappearance during 1996-2010.
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Histogram of Linear Speed 40 35
Count of events
30 25 20 15 10 5 0 0
200
400
600
800
1000 1200 1400 1600 1800
CME Linear Speed (Km/s)
Fig. 9: Histogram of linear speed of CMEs which are associated with filament disappearance during 1996-2010.
19