-
Notifications
You must be signed in to change notification settings - Fork 2
/
cme_stats.py
1998 lines (1263 loc) · 71.7 KB
/
cme_stats.py
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
49
50
51
52
53
54
55
56
57
58
59
60
61
62
63
64
65
66
67
68
69
70
71
72
73
74
75
76
77
78
79
80
81
82
83
84
85
86
87
88
89
90
91
92
93
94
95
96
97
98
99
100
101
102
103
104
105
106
107
108
109
110
111
112
113
114
115
116
117
118
119
120
121
122
123
124
125
126
127
128
129
130
131
132
133
134
135
136
137
138
139
140
141
142
143
144
145
146
147
148
149
150
151
152
153
154
155
156
157
158
159
160
161
162
163
164
165
166
167
168
169
170
171
172
173
174
175
176
177
178
179
180
181
182
183
184
185
186
187
188
189
190
191
192
193
194
195
196
197
198
199
200
201
202
203
204
205
206
207
208
209
210
211
212
213
214
215
216
217
218
219
220
221
222
223
224
225
226
227
228
229
230
231
232
233
234
235
236
237
238
239
240
241
242
243
244
245
246
247
248
249
250
251
252
253
254
255
256
257
258
259
260
261
262
263
264
265
266
267
268
269
270
271
272
273
274
275
276
277
278
279
280
281
282
283
284
285
286
287
288
289
290
291
292
293
294
295
296
297
298
299
300
301
302
303
304
305
306
307
308
309
310
311
312
313
314
315
316
317
318
319
320
321
322
323
324
325
326
327
328
329
330
331
332
333
334
335
336
337
338
339
340
341
342
343
344
345
346
347
348
349
350
351
352
353
354
355
356
357
358
359
360
361
362
363
364
365
366
367
368
369
370
371
372
373
374
375
376
377
378
379
380
381
382
383
384
385
386
387
388
389
390
391
392
393
394
395
396
397
398
399
400
401
402
403
404
405
406
407
408
409
410
411
412
413
414
415
416
417
418
419
420
421
422
423
424
425
426
427
428
429
430
431
432
433
434
435
436
437
438
439
440
441
442
443
444
445
446
447
448
449
450
451
452
453
454
455
456
457
458
459
460
461
462
463
464
465
466
467
468
469
470
471
472
473
474
475
476
477
478
479
480
481
482
483
484
485
486
487
488
489
490
491
492
493
494
495
496
497
498
499
500
501
502
503
504
505
506
507
508
509
510
511
512
513
514
515
516
517
518
519
520
521
522
523
524
525
526
527
528
529
530
531
532
533
534
535
536
537
538
539
540
541
542
543
544
545
546
547
548
549
550
551
552
553
554
555
556
557
558
559
560
561
562
563
564
565
566
567
568
569
570
571
572
573
574
575
576
577
578
579
580
581
582
583
584
585
586
587
588
589
590
591
592
593
594
595
596
597
598
599
600
601
602
603
604
605
606
607
608
609
610
611
612
613
614
615
616
617
618
619
620
621
622
623
624
625
626
627
628
629
630
631
632
633
634
635
636
637
638
639
640
641
642
643
644
645
646
647
648
649
650
651
652
653
654
655
656
657
658
659
660
661
662
663
664
665
666
667
668
669
670
671
672
673
674
675
676
677
678
679
680
681
682
683
684
685
686
687
688
689
690
691
692
693
694
695
696
697
698
699
700
701
702
703
704
705
706
707
708
709
710
711
712
713
714
715
716
717
718
719
720
721
722
723
724
725
726
727
728
729
730
731
732
733
734
735
736
737
738
739
740
741
742
743
744
745
746
747
748
749
750
751
752
753
754
755
756
757
758
759
760
761
762
763
764
765
766
767
768
769
770
771
772
773
774
775
776
777
778
779
780
781
782
783
784
785
786
787
788
789
790
791
792
793
794
795
796
797
798
799
800
801
802
803
804
805
806
807
808
809
810
811
812
813
814
815
816
817
818
819
820
821
822
823
824
825
826
827
828
829
830
831
832
833
834
835
836
837
838
839
840
841
842
843
844
845
846
847
848
849
850
851
852
853
854
855
856
857
858
859
860
861
862
863
864
865
866
867
868
869
870
871
872
873
874
875
876
877
878
879
880
881
882
883
884
885
886
887
888
889
890
891
892
893
894
895
896
897
898
899
900
901
902
903
904
905
906
907
908
909
910
911
912
913
914
915
916
917
918
919
920
921
922
923
924
925
926
927
928
929
930
931
932
933
934
935
936
937
938
939
940
941
942
943
944
945
946
947
948
949
950
951
952
953
954
955
956
957
958
959
960
961
962
963
964
965
966
967
968
969
970
971
972
973
974
975
976
977
978
979
980
981
982
983
984
985
986
987
988
989
990
991
992
993
994
995
996
997
998
999
1000
# cme_stats.py
#
# analyses HELCATS ICMECAT data for paper on CME statistics Moestl et al. 2019
#Author: C. Moestl, IWF Graz, Austria
#twitter @chrisoutofspace, https://github.com/cmoestl
#last update November 2018
#python 3.5.5 with sunpy, seaborn ipython 4.2.0
#needs file cme_stats_module.py
#current status:
#work in progress
from scipy import stats
import scipy.io
from matplotlib import cm
import sys
import matplotlib
import matplotlib.pyplot as plt
import matplotlib.dates as mdates
import numpy as np
import astropy.constants as const
import sunpy.time
import time
import pickle
import seaborn as sns
import os
import urllib
import json
import cme_stats_module
from cme_stats_module import dynamic_pressure
from cme_stats_module import getcat
from cme_stats_module import decode_array
from cme_stats_module import time_to_num_cat
from cme_stats_module import gaussian
from cme_stats_module import get_omni2_data
from cme_stats_module import load_url_current_directory
#ignore warnings
#import warnings
#warnings.filterwarnings('ignore')
#use one time to control plots
#plt.show(block=True)
#CHECK for MAVEN program for MARS EVENTS at MAVEN -> HI / MSL LIST FOR VERIFICATION
#url_hicat='https://www.helcats-fp7.eu/catalogues/data/HCME_WP3_V05.json'
#download, see URLLIB https://docs.python.org/3/howto/urllib2.html
#with urllib.request.urlopen(url_plasma) as url:
# pr = json.loads (url.read().decode())
#hicat_file='cats/HCME_WP3_V05.json'
#h = json.loads(open(hicat_file).read())
##kill first row which stems from the description part
#hmf_speed=np.zeros(len(h['data']))
#fpf_speed=np.zeros(len(h['data']))
#for k in np.arange(0,len(h['data']),1):
# hmf_speed[k]=h['data'][k][25]
# fpf_speed[k]=h['data'][k][9]
#for line in open('cats/MSL_event_table_forstner_2019.txt'):
#line = line.split() # to deal with blank
# print(line)
#http://docs.astropy.org/en/stable/io/ascii/
#alternative
#from astropy.io import ascii
#data = ascii.read('cats/MSL_event_table_forstner_2019.txt')
##########################################################################################
######################################## MAIN PROGRAM ####################################
##########################################################################################
### ORDER: 1 durations, 2 B field, 3 time inside, 4 ICME frequency
plt.close('all')
print()
print('Start cme_stats.py main program.')
print('ICME parameters at all 4 terrestrial planets.')
print('Christian Moestl, IWF Graz, Austria, last update: November 2018.')
######################## get cats
#solar radius
Rs_in_AU=float(const.R_sun/const.au)
filename_icmecat='cats/HELCATS_ICMECAT_v20_SCEQ.sav'
i=getcat(filename_icmecat)
#now this is a scipy recarray
#access each element of the array see http://docs.scipy.org/doc/numpy/user/basics.rec.html
#access variables
#i.icmecat['id']
#look at contained variables
#print(i.icmecat.dtype)
#get spacecraft and planet positions
pos=getcat('cats/positions_2007_2023_HEEQ_6hours.sav')
pos_time_num=time_to_num_cat(pos.time)[0]
print()
print()
print('Spacecraft positions available:')
print(pos.keys())
print()
########## LOAD OMNI2 data for sunspot data
load_url_current_directory('omni2_all_years.dat', \
'ftp://nssdcftp.gsfc.nasa.gov/pub/data/omni/low_res_omni/omni2_all_years.dat')
#if omni2 hourly data is not yet converted and saved as pickle, do it:
if not os.path.exists('omni2_all_years_pickle.p'):
#load OMNI2 dataset from .dat file with a function from dst_module.py
o=get_omni2_data()
#contains: o. time,day,hour,btot,bx,by,bz,bygsm,bzgsm,speed,speedx,den,pdyn,dst,kp
#save for faster loading later
pickle.dump(o, open('omni2_all_years_pickle.p', 'wb') )
else: o=pickle.load(open('omni2_all_years_pickle.p', 'rb') )
print('loaded OMNI2 data')
######## load a file with the time and B total of the original in situ data,
#to be used in part (3) - has 355 MB to download
#STA, STB, Wind, MES, VEX, MAVEN
load_url_current_directory('insitu_data_time_btot_moestl_2019_paper.p', \
'https://oeawcloud.oeaw.ac.at/index.php/s/z7nZVbH8qBjaTf5/download')
#info for myself: file insitu_data_time_btot_moestl_2019_paper.p
#was done with program extract_data in process_data package (not on github)
[win_time,win_btot,sta_time,sta_btot,stb_time,stb_btot, \
mav_time, mav_btot, vex_time, vex_btot, mes_time, mes_btot]= \
pickle.load(open( "insitu_data_time_btot_moestl_2019_paper.p", "rb" ) )
print('loaded time/Btotal data for STEREO-A/B, Wind, VEX, MESSENGER, MAVEN')
########################### get all parameters from ICMECAT for easier handling
# id for each event
iid=i.icmecat['id']
# need to decode all strings
iid=decode_array(iid)
# observing spacecraft
isc=i.icmecat['sc_insitu'] #string
isc=decode_array(isc)
# all times need to be converted from the IDL format to matplotlib format,
# also make strings for each date
icme_start_time=i.icmecat['ICME_START_TIME']
[icme_start_time_num,icme_start_time_str]=time_to_num_cat(icme_start_time)
mo_start_time=i.icmecat['MO_START_TIME']
[mo_start_time_num,mo_start_time_str]=time_to_num_cat(mo_start_time)
mo_end_time=i.icmecat['MO_END_TIME']
[mo_end_time_num,mo_end_time_str]=time_to_num_cat(mo_end_time)
# this time exists only for Wind
icme_end_time=i.icmecat['ICME_END_TIME']
[icme_end_time_num,icme_end_time_str]=time_to_num_cat(icme_end_time)
# get variables from ICMECAT
sc_heliodistance=i.icmecat['SC_HELIODISTANCE']
sc_long_heeq=i.icmecat['SC_LONG_HEEQ']
sc_lat_heeq=i.icmecat['SC_LAT_HEEQ']
mo_bmax=i.icmecat['MO_BMAX']
mo_bmean=i.icmecat['MO_BMEAN']
mo_bstd=i.icmecat['MO_BSTD']
mo_bzmean=i.icmecat['MO_BZMEAN']
mo_bzmin=i.icmecat['MO_BZMIN']
mo_duration=i.icmecat['MO_DURATION']
mo_mva_axis_long=i.icmecat['MO_MVA_AXIS_LONG']
mo_mva_axis_lat=i.icmecat['MO_MVA_AXIS_LAT']
mo_mva_ratio=i.icmecat['MO_MVA_RATIO']
sheath_speed=i.icmecat['SHEATH_SPEED']
sheath_speed_std=i.icmecat['SHEATH_SPEED_STD']
mo_speed=i.icmecat['MO_SPEED']
mo_speed_st=i.icmecat['MO_SPEED_STD']
sheath_density=i.icmecat['SHEATH_DENSITY']
sheath_density_std=i.icmecat['SHEATH_DENSITY_STD']
mo_density=i.icmecat['MO_DENSITY']
mo_density_std=i.icmecat['MO_DENSITY_STD']
sheath_temperature=i.icmecat['SHEATH_TEMPERATURE']
sheath_temperature_std=i.icmecat['SHEATH_TEMPERATURE_STD']
mo_temperature=i.icmecat['MO_TEMPERATURE']
mo_temperature_std=i.icmecat['MO_TEMPERATURE_STD']
sheath_pdyn=i.icmecat['SHEATH_PDYN']
sheath_pdyn_std=i.icmecat['SHEATH_PDYN_STD']
mo_pdyn=i.icmecat['MO_PDYN']
mo_pdyn_std=i.icmecat['MO_PDYN_STD']
#calculate icme_durations in hours
icme_durations=(mo_end_time_num-icme_start_time_num)*24 #hours
#same for magnetic obstacle (MO)
mo_durations=(mo_end_time_num-mo_start_time_num)*24 #hours
#get indices of events by different spacecraft
ivexind=np.where(isc == 'VEX')
istaind=np.where(isc == 'STEREO-A')
istbind=np.where(isc == 'STEREO-B')
iwinind=np.where(isc == 'Wind')
imesind=np.where(isc == 'MESSENGER')
iulyind=np.where(isc == 'ULYSSES')
imavind=np.where(isc == 'MAVEN')
#take MESSENGER only at Mercury, only events after orbit insertion
imercind=np.where(np.logical_and(isc =='MESSENGER', \
icme_start_time_num > mdates.date2num(sunpy.time.parse_time('2011-03-18'))))
############### set limits of solar minimum, rising/declining phase and solar maximum
minstart=mdates.date2num(sunpy.time.parse_time('2007-01-01'))
minend=mdates.date2num(sunpy.time.parse_time('2009-12-31'))
risestart=mdates.date2num(sunpy.time.parse_time('2010-01-01'))
riseend=mdates.date2num(sunpy.time.parse_time('2011-06-30'))
maxstart=mdates.date2num(sunpy.time.parse_time('2011-07-01'))
maxend=mdates.date2num(sunpy.time.parse_time('2014-12-31'))
declstart=mdates.date2num(sunpy.time.parse_time('2015-01-01'))
declend=mdates.date2num(sunpy.time.parse_time('2017-12-31'))
############### extract events by limits of solar min,
############### rising, max, too few events for MAVEN and Ulysses
iallind_min=np.where(np.logical_and(icme_start_time_num > minstart,icme_start_time_num < minend))[0]
iallind_rise=np.where(np.logical_and(icme_start_time_num > risestart,icme_start_time_num < riseend))[0]
iallind_max=np.where(np.logical_and(icme_start_time_num > maxstart,icme_start_time_num < maxend))[0]
iwinind_min=iallind_min[np.where(isc[iallind_min]=='Wind')]
iwinind_rise=iallind_rise[np.where(isc[iallind_rise]=='Wind')]
iwinind_max=iallind_max[np.where(isc[iallind_max]=='Wind')]
ivexind_min=iallind_min[np.where(isc[iallind_min]=='VEX')]
ivexind_rise=iallind_rise[np.where(isc[iallind_rise]=='VEX')]
ivexind_max=iallind_max[np.where(isc[iallind_max]=='VEX')]
imesind_min=iallind_min[np.where(isc[iallind_min]=='MESSENGER')]
imesind_rise=iallind_rise[np.where(isc[iallind_rise]=='MESSENGER')]
imesind_max=iallind_max[np.where(isc[iallind_max]=='MESSENGER')]
istaind_min=iallind_min[np.where(isc[iallind_min]=='STEREO-A')]
istaind_rise=iallind_rise[np.where(isc[iallind_rise]=='STEREO-A')]
istaind_max=iallind_max[np.where(isc[iallind_max]=='STEREO-A')]
istbind_min=iallind_min[np.where(isc[iallind_min]=='STEREO-B')]
istbind_rise=iallind_rise[np.where(isc[iallind_rise]=='STEREO-B')]
istbind_max=iallind_max[np.where(isc[iallind_max]=='STEREO-B')]
# select the events at Mercury extra after orbit insertion
# no events available for solar minimum!
imercind_min=iallind_min[np.where(np.logical_and(isc[iallind_min] =='MESSENGER',icme_start_time_num[iallind_min] > mdates.date2num(sunpy.time.parse_time('2011-03-18'))))]
imercind_rise=iallind_rise[np.where(np.logical_and(isc[iallind_rise] =='MESSENGER',icme_start_time_num[iallind_rise] > mdates.date2num(sunpy.time.parse_time('2011-03-18'))))]
imercind_max=iallind_max[np.where(np.logical_and(isc[iallind_max] =='MESSENGER',icme_start_time_num[iallind_max] > mdates.date2num(sunpy.time.parse_time('2011-03-18'))))]
print()
print()
##################### (1a) ICME DURATION VS DISTANCE and linear fit #####################
sns.set_context("talk") #sns.set_style("darkgrid")
sns.set_style("ticks",{'grid.linestyle': '--'})
print('-------------------------------------------------')
print()
print('1a ICME DURATION VS DISTANCE')
print()
fig=plt.figure(1,figsize=(12,11 ))
fsize=15
ax1 = plt.subplot2grid((2,1), (0, 0))
#x axis
xfit=np.linspace(0,2,1000)
#force through origin, fit with y=kx
scx=sc_heliodistance[:,np.newaxis]
durfit_f, _, _, _ =np.linalg.lstsq(scx,icme_durations, rcond=None)
scxmin=sc_heliodistance[iallind_min][:,np.newaxis]
durfitmin_f, _, _, _ =np.linalg.lstsq(scxmin,icme_durations[iallind_min],rcond=None)
scxrise=sc_heliodistance[iallind_rise][:,np.newaxis]
durfitrise_f, _, _, _ =np.linalg.lstsq(scxrise,icme_durations[iallind_rise],rcond=None)
scxmax=sc_heliodistance[iallind_max][:,np.newaxis]
durfitmax_f, _, _, _ =np.linalg.lstsq(scxmax,icme_durations[iallind_max],rcond=None)
#make the y axis for the fits forced through the origin
ydurfitall_f=durfit_f*xfit
ydurfitmin_f=durfitmin_f*xfit
ydurfitrise_f=durfitrise_f*xfit
ydurfitmax_f=durfitmax_f*xfit
plt.plot(sc_heliodistance,icme_durations,'o',color='blue',markersize=4, alpha=0.4)
#for plotting min/rise/max differently
#plt.plot(sc_heliodistance[iallind_min],icme_durations[iallind_min],'o',color='dimgre',markersize=3, alpha=0.4,label='D min')
#plt.plot(sc_heliodistance[iallind_rise],icme_durations[iallind_rise],'o',color='grey',markersize=3, alpha=0.7,label='D rise')
#plt.plot(sc_heliodistance[iallind_max],icme_durations[iallind_max],'o',color='black',markersize=3, alpha=0.8,label='D max')
#plot fits
plt.plot(xfit,ydurfitall_f,'-',color='blue', lw=3, alpha=0.9,label='fit')
plt.plot(xfit,ydurfitmin_f,'--',color='black', lw=2, alpha=0.9,label='min fit')
plt.plot(xfit,ydurfitrise_f,'-.',color='black', lw=2, alpha=0.9,label='rise fit')
plt.plot(xfit,ydurfitmax_f,'-',color='black', lw=2, alpha=0.9,label='max fit')
print()
print('linear fit results, hours vs AU')
print('overall: D[h]={:.2f} R[AU] '.format(durfit_f[0]))
print('minimum: D[h]={:.2f} R[AU] '.format(durfitmin_f[0]))
print('rise phase: D[h]={:.2f} R[AU]'.format(durfitrise_f[0]))
print('maximum: D[h]={:.2f} R[AU]'.format(durfitmax_f[0]))
label_level=85
plt.annotate('overall:',xy=(0.1,label_level),fontsize=11)
plt.annotate('D[h]={:.2f} R[AU]'.format(durfit_f[0]),xy=(0.3,label_level),fontsize=11)
plt.annotate('minimum:',xy=(0.1,label_level-6),fontsize=11)
plt.annotate('D[h]={:.2f} R[AU] '.format(durfitmin_f[0]),xy=(0.3,label_level-6),fontsize=11)
plt.annotate('rise phase:',xy=(0.1,label_level-12),fontsize=11)
plt.annotate('D[h]={:.2f} R[AU]'.format(durfitrise_f[0]),xy=(0.3,label_level-12),fontsize=11)
plt.annotate('maximum:',xy=(0.1,label_level-18),fontsize=11)
plt.annotate('D[h]={:.2f} R[AU]'.format(durfitmax_f[0]),xy=(0.3,label_level-18),fontsize=11)
#planet limits
plt.axvspan(np.min(pos.mars[0]),np.max(pos.mars[0]), color='orangered', alpha=0.2)
plt.axvspan(np.min(pos.mercury[0]),np.max(pos.mercury[0]), color='darkgrey', alpha=0.2)
plt.axvspan(np.min(pos.venus[0]),np.max(pos.venus[0]), color='orange', alpha=0.2)
plt.axvspan(np.min(pos.earth[0]),np.max(pos.earth[0]), color='mediumseagreen', alpha=0.2)
#plt.axvspan(np.min(pos.sta[0]),np.max(pos.sta[0]), color='red', alpha=0.2) #STEREO-A
#plt.axvspan(np.min(pos.stb[0]),np.max(pos.stb[0]), color='blue', alpha=0.2) #STEREO-B
#Parker Probe minimum
plt.plot([0.046,0.046],[0,110], color='black', linestyle='--', linewidth=1)
label_level=100
plt.annotate('Mars', xy=(1.5,label_level), ha='center',fontsize=fsize)
plt.annotate('Mercury', xy=(0.38,label_level), ha='center',fontsize=fsize)
plt.annotate('Venus', xy=(0.72,label_level), ha='center',fontsize=fsize)
plt.annotate('Earth', xy=(1,label_level), ha='center',fontsize=fsize)
plt.annotate('PSP', xy=(0.05,label_level), ha='left',fontsize=fsize)
ax1.set_xticks(np.arange(0,2,0.2))
plt.xlim(0,max(sc_heliodistance)+0.3)
plt.ylim(0,110)
plt.legend(loc=4,fontsize=fsize-1)
plt.xlabel('Heliocentric distance R [AU]',fontsize=fsize)
plt.ylabel('ICME duration D [hours]',fontsize=fsize)
plt.yticks(fontsize=fsize)
plt.xticks(fontsize=fsize)
#plt.grid()
##################### (1b) ICME DURATION VS TIME ########################################
print('')
print('1b ICME DURATION VS TIME')
#tests for gaussians and Hathaway's function for solar cycle, not used
#Wind
#tfit=mdates.date2num(sunpy.time.parse_time('2009-04-01'))+np.arange(0,365*10)
#t0=mdates.date2num(sunpy.time.parse_time('2009-01-01'))
#Gaussian
#sigma=1000
#bfitmax=30
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='mediumseagreen',linestyle='-',markersize=0, label='Earth fit')
#Hathaway 2015 equation 6 page 40
#average cycle sunspot number
#A=100 #amplitude ##195 for sunspot
#b=100*12 #56*12 for months to days
#c=0.8
#4 free parameters A, b, c, t0
#Fwind=A*(((tfit-t0)/b)**3) * 1/(np.exp((((tfit-t0)/b)**2))-c)
#plt.plot_date(tfit, Fwind,'o',color='mediumseagreen',linestyle='-',markersize=0, label='Earth fit')
#xaxis: 10 years, daily data point
#xfit2=mdates.date2num(sunpy.time.parse_time('2007-01-01'))+np.arange(0,365*10)
#MESSENGER
#sigma=1000
#bfitmax=10
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit2-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='darkgrey',linestyle='-',markersize=0, label='Mercury fit')
#VEX
#inital guess
#sigma=1000
#bfitmax=20
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit2-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit2, ygauss*1/max(ygauss)*bfitmax,'o',color='orange',linestyle='-',markersize=0, label='Venus fit')
#for Mars: reconstruct likely parameters if sigma is quite similar for all fits, take mean of those sigmas and adjust bfitmax as function of distance with power law)
#plot reconstructed function for Mars
#bfitmax=40
#plt.plot_date(xfit2, Fwind,'o',color='steelblue',linestyle='--',markersize=0, label='Mars reconstr.')
################## plot
ax2 = plt.subplot2grid((2,1), (1, 0))
markers=6
linew=0
#plot durations for all planets
ax2.plot_date(icme_start_time_num[imesind],icme_durations[imesind], \
'o',color='darkgrey',markersize=markers,linestyle='-',linewidth=linew,label='MESSENGER')
ax2.plot_date(icme_start_time_num[ivexind],icme_durations[ivexind], \
'o',color='orange',markersize=markers,linestyle='-',linewidth=linew, label='Venus')
ax2.plot_date(icme_start_time_num[iwinind],icme_durations[iwinind], \
'o',color='mediumseagreen',markersize=markers, linestyle='-', linewidth=linew, label='Earth')
ax2.plot_date(icme_start_time_num[imavind],icme_durations[imavind], \
'o',color='steelblue',markersize=markers,linestyle='-',linewidth=linew, label='Mars')
#limits solar min/rise/maxax2.set_ylim(0,80)
vlevel=130
spanalpha=0.05
plt.axvspan(minstart,minend, color='green', alpha=spanalpha)
plt.annotate('solar minimum',xy=(minstart+(minend-minstart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(minstart+10,vlevel),ha='left')
plt.annotate('>',xy=(minend-10,vlevel),ha='right')
plt.axvspan(risestart,riseend, color='yellow', alpha=spanalpha)
plt.annotate('rising phase',xy=(risestart+(riseend-risestart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(risestart+10,vlevel),ha='left')
plt.annotate('>',xy=(riseend-10,vlevel),ha='right')
plt.axvspan(maxstart,maxend, color='red', alpha=spanalpha)
plt.annotate('solar maximum',xy=(maxstart+(maxend-maxstart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(maxstart+10,vlevel),ha='left')
plt.annotate('>',xy=(maxend,vlevel),ha='right')
#plot means as horizontal lines for each sub interval
plt.plot_date( [minstart,minend], [np.mean(icme_durations[iwinind_min]),np.mean(icme_durations[iwinind_min])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [minstart,minend], [np.mean(icme_durations[ivexind_min]),np.mean(icme_durations[ivexind_min])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [minstart,minend], [np.mean(icme_durations[imesind_min]),np.mean(icme_durations[imesind_min])], color='darkgrey', linestyle='-', markersize=0)
plt.plot_date( [risestart,riseend], [np.mean(icme_durations[iwinind_rise]),np.mean(icme_durations[iwinind_rise])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [risestart,riseend], [np.mean(icme_durations[ivexind_rise]),np.mean(icme_durations[ivexind_rise])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [risestart,riseend], [np.mean(icme_durations[imesind_rise]),np.mean(icme_durations[imesind_rise])], color='darkgrey', linestyle='-', markersize=0)
plt.plot_date( [maxstart,maxend], [np.mean(icme_durations[iwinind_max]),np.mean(icme_durations[iwinind_max])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [maxstart,maxend], [np.mean(icme_durations[ivexind_max]),np.mean(icme_durations[ivexind_max])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [maxstart,maxend], [np.mean(icme_durations[imesind_max]),np.mean(icme_durations[imesind_max])], color='darkgrey', linestyle='-', markersize=0)
plt.xlim(mdates.date2num(sunpy.time.parse_time('2007-01-01')), mdates.date2num(sunpy.time.parse_time('2016-12-31')))
plt.ylabel('ICME duration D [hours]',fontsize=fsize)
plt.xlabel('year',fontsize=fsize)
plt.tight_layout()
plt.yticks(fontsize=fsize)
plt.xticks(fontsize=fsize)
plt.legend(loc=1,fontsize=fsize-1)
#panel labels
plt.figtext(0.01,0.98,'a',color='black', fontsize=fsize, ha='left',fontweight='bold')
plt.figtext(0.01,0.485,'b',color='black', fontsize=fsize, ha='left',fontweight='bold')
plt.show()
plt.savefig('plots_stats/icme_durations_distance_time_paper.pdf', dpi=300)
plt.savefig('plots_stats/icme_durations_distance_time_paper.png', dpi=300)
#Sunspot number
#ax3 = ax2.twinx()
#ax3.plot_date(o.time, o.spot, '-', color='black', alpha=0.5,linewidth=0.2)
#ax3.set_ylabel('Sunspot number')
#ax3.set_ylim([0,220])
#results on durations
print()
print()
print('DURATION results, mean +/- std [hours]')
print()
print('Mercury ', round(np.mean(icme_durations[imercind]),1),' +/- ', round(np.std(icme_durations[imercind]),1))
#print('min ', round(np.mean(icme_durations[imercind_min]),1), ' +/- ', round(np.std(icme_durations[imercind_min]),1))
print('min no events')
print('rise ', round(np.mean(icme_durations[imercind_rise]),1), ' +/- ', round(np.std(icme_durations[imercind_rise]),1))
print('max ', round(np.mean(icme_durations[imercind_max]),1), ' +/- ', round(np.std(icme_durations[imercind_max]),1))
print()
print('Venus ', round(np.mean(icme_durations[ivexind]),1),' +/- ', round(np.std(icme_durations[ivexind]),1))
print('min ', round(np.mean(icme_durations[ivexind_min]),1), ' +/- ', round(np.std(icme_durations[ivexind_min]),1))
print('rise ', round(np.mean(icme_durations[ivexind_rise]),1), ' +/- ', round(np.std(icme_durations[ivexind_rise]),1))
print('max ', round(np.mean(icme_durations[ivexind_max]),1), ' +/- ', round(np.std(icme_durations[ivexind_max]),1))
print()
print('Earth ', round(np.mean(icme_durations[iwinind]),1),' +/- ', round(np.std(icme_durations[iwinind]),1))
print('min ', round(np.mean(icme_durations[iwinind_min]),1), ' +/- ', round(np.std(icme_durations[iwinind_min]),1))
print('rise ', round(np.mean(icme_durations[iwinind_rise]),1), ' +/- ', round(np.std(icme_durations[iwinind_rise]),1))
print('max ', round(np.mean(icme_durations[iwinind_max]),1), ' +/- ', round(np.std(icme_durations[iwinind_max]),1))
print()
print('MAVEN only declining phase')
print('decl ',round(np.mean(icme_durations[imavind]),1),' +/- ', round(np.std(icme_durations[imavind]),1))
print()
print()
#################################### (2) Bfield plot ICMECAT ############################
print('-------------------------------------------------')
print('2 MO FIELD VS DISTANCE and time, 3 figure panels')
print()
sns.set_context("talk")
sns.set_style("ticks",{'grid.linestyle': '--'})
fig=plt.figure(2,figsize=(12,12 ))
fsize=15
ax1 = plt.subplot2grid((2,2), (0, 0))
# xfit starts here at 1 Rs because there should not be a 0 in xfit ** bmaxfit[0] later
xfit=np.linspace(Rs_in_AU,2,1000)
print('Fit results for B in Form: y=B0*x^k')
####### power law fits for all events
bmaxfit=np.polyfit(np.log10(sc_heliodistance),np.log10(mo_bmax),1)
b=10**bmaxfit[1]
bmaxfitfun=b*(xfit**bmaxfit[0])
print('bmax: ',round(10**bmaxfit[1],2),' x ^', round(bmaxfit[0],2))
bmeanfit=np.polyfit(np.log10(sc_heliodistance),np.log10(mo_bmean),1)
b=10**bmeanfit[1]
bmeanfitfun=b*(xfit**bmeanfit[0])
print('bmean: ', round(10**bmeanfit[1],2),' x ^',round(bmeanfit[0],2))
##fit with only minimum events
bmeanfit_min=np.polyfit(np.log10(sc_heliodistance[iallind_min]),np.log10(mo_bmean[iallind_min]),1)
bmeanfitfun_min=(10**bmeanfit_min[1])*(xfit**bmeanfit_min[0])
print('bmean_min: ', round(10**bmeanfit_min[1],2),' x ^', round(bmeanfit_min[0],2))
##fit with only rising events
bmeanfit_rise=np.polyfit(np.log10(sc_heliodistance[iallind_rise]),np.log10(mo_bmean[iallind_rise]),1)
bmeanfitfun_rise=(10**bmeanfit_rise[1])*(xfit**bmeanfit_rise[0])
print('bmean_rise: ', round(10**bmeanfit_rise[1],2),' x ^', round(bmeanfit_rise[0],2))
##fit with only maximum events
bmeanfit_max=np.polyfit(np.log10(sc_heliodistance[iallind_max]),np.log10(mo_bmean[iallind_max]),1)
bmeanfitfun_max=(10**bmeanfit_max[1])*(xfit**bmeanfit_max[0])
print('bmean_max: ', round(10**bmeanfit_max[1],2),' x ^',round(bmeanfit_max[0],2))
################# plots 2a
plt.plot(sc_heliodistance,mo_bmean,'o',color='black',markersize=5, alpha=0.7,label='$\mathregular{<B>}$')
plt.plot(xfit,bmeanfitfun,'-',color='black', lw=2, alpha=0.7,label='$\mathregular{<B> \\ fit}$')
plt.plot(sc_heliodistance,mo_bmax,'o',color='dodgerblue',markersize=5, alpha=0.7,label='$\mathregular{B_{max}}$')
plt.plot(xfit,bmaxfitfun,'-',color='dodgerblue', lw=2, alpha=0.7,label='$\mathregular{B_{max} \\ fit}$')
#plt.text(1.1,120,'$\mathregular{<B> [nT]= {:.2f} R[AU]^{{:.2f}}}$'.format(10**bmeanfit[1],bmeanfit[0]), fontsize=10)
plt.text(1.1,60,r'<B> [nT]= {:.2f} R[AU]^{:.2f}'.format(10**bmeanfit[1],bmeanfit[0]), fontsize=10)
#mars limits
plt.axvspan(np.min(pos.mars[0]),np.max(pos.mars[0]), color='orangered', alpha=0.2)
#plt.figtext(0.8,0.8,'Mars',color='orangered')
plt.axvspan(np.min(pos.mercury[0]),np.max(pos.mercury[0]), color='darkgrey', alpha=0.2)
#plt.figtext(0.25,0.8,'Mercury',color='darkgrey')
plt.axvspan(np.min(pos.venus[0]),np.max(pos.venus[0]), color='orange', alpha=0.2)
#plt.figtext(0.42,0.8,'Venus',color='orange')
plt.axvspan(np.min(pos.earth[0]),np.max(pos.earth[0]), color='mediumseagreen', alpha=0.2)
#plt.figtext(0.6,0.8,'Earth',color='mediumseagreen')
#plt.figtext(0.65,0.2,' D[h]={:.2f} R[AU] + {:.2f}'.format(durfit[0],durfit[1]))
plt.xlim(0,1.8)
plt.ylim(0,max(mo_bmax)+20)
plt.legend(loc=1,fontsize=fsize)
plt.xlabel('Heliocentric distance R [AU]',fontsize=fsize)
plt.ylabel('Magnetic field in MO B [nT]',fontsize=fsize)
plt.yticks(fontsize=fsize)
plt.xticks(fontsize=fsize)
#plt.grid()
######################## 2b logarithmic plot with Sun
#for the bmean fit, append one value for the coronal field
#patsourakos georgoulis 2016: 0.03 G for 10 Rs #10^5 nT is 1 Gauss
mo_bmean_sun=np.append(mo_bmean,10**5*0.03)
mo_bmax_sun=np.append(mo_bmax,10**5*0.03)
sc_heliodistance_sun=np.append(sc_heliodistance,10*Rs_in_AU)
print()
bmeanfit_sun=np.polyfit(np.log10(sc_heliodistance_sun),np.log10(mo_bmean_sun),1)
b=10**bmeanfit_sun[1]
bmeanfitfun_sun=b*(xfit**bmeanfit_sun[0])
print('bmean_sun: ', round(10**bmeanfit_sun[1],2),' x ^',round(bmeanfit_sun[0],2))
bmaxfit_sun=np.polyfit(np.log10(sc_heliodistance_sun),np.log10(mo_bmax_sun),1)
b=10**bmaxfit_sun[1]
bmaxfitfun_sun=b*(xfit**bmaxfit_sun[0])
print('bmax_sun: ', round(10**bmaxfit_sun[1],2),' x ^',round(bmaxfit_sun[0],2))
ax3 = plt.subplot2grid((2,2), (0, 1))
plt.plot(sc_heliodistance_sun,np.log10(mo_bmean_sun),'o',color='black',markersize=5, alpha=0.7,label='$\mathregular{<B>}$')
plt.plot(xfit,np.log10(bmeanfitfun_sun),'-',color='black', lw=2, alpha=0.7,label='$\mathregular{<B> fit}$')
plt.plot(xfit,np.log10(bmaxfitfun_sun),'-',color='dodgerblue', lw=2, alpha=0.7,label='$\mathregular{B_{max} fit}$')
plt.ylim(0,6)
#Planet labels and shades
ax3.annotate('Mars', xy=(1.5,4), ha='center',fontsize=fsize-2)
ax3.annotate('Mercury', xy=(0.38,4), ha='center',fontsize=fsize-2)
ax3.annotate('Venus', xy=(0.72,4), ha='center',fontsize=fsize-2)
ax3.annotate('Earth', xy=(1,4), ha='center',fontsize=fsize-2)
plt.plot([0.046,0.046],[0,10], color='black', linestyle='--', linewidth=1)
plt.axvspan(np.min(pos.mars[0]),np.max(pos.mars[0]), color='orangered', alpha=0.2)
plt.axvspan(np.min(pos.mercury[0]),np.max(pos.mercury[0]), color='darkgrey', alpha=0.2)
plt.axvspan(np.min(pos.venus[0]),np.max(pos.venus[0]), color='orange', alpha=0.2)
plt.axvspan(np.min(pos.earth[0]),np.max(pos.earth[0]), color='mediumseagreen', alpha=0.2)
plt.xlim(0,1.8)
plt.legend(loc=1,fontsize=fsize)
plt.xlabel('Heliocentric distance R [AU]',fontsize=fsize)
plt.ylabel('Magnetic field in MO log(B) [nT]',fontsize=fsize)
plt.yticks(fontsize=fsize)
plt.xticks(fontsize=fsize)
#panel labels
plt.figtext(0.03,0.96,'a',color='black', fontsize=fsize, ha='left',fontweight='bold')
plt.figtext(0.515,0.96,'b',color='black', fontsize=fsize, ha='left',fontweight='bold')
plt.figtext(0.03,0.49,'c',color='black', fontsize=fsize, ha='left',fontweight='bold')
################################# 2c MO B vs. time
ax2 = plt.subplot2grid((2,2), (1, 0), colspan=2)
markers=6
linew=0
plt.plot_date(icme_start_time_num[imesind],mo_bmean[imesind],'o',color='darkgrey',markersize=markers,linestyle='-',linewidth=linew,label='MESSENGER')
plt.plot_date(icme_start_time_num[ivexind],mo_bmean[ivexind],'o',color='orange',markersize=markers,linestyle='-',linewidth=linew, label='Venus')
plt.plot_date(icme_start_time_num[iwinind],mo_bmean[iwinind],'o',color='mediumseagreen',markersize=markers, linestyle='-', linewidth=linew, label='Earth')
plt.plot_date(icme_start_time_num[imavind],mo_bmean[imavind],'o',color='steelblue',markersize=markers,linestyle='-',linewidth=linew, label='Mars')
#NOT USED:
#add gaussian fits for MESSENGER, VEX, Wind (MAVEN too few data points)
#instead of gaussian, fit solar cycle functions in Hathaway 2015 solar cycle living reviews equation 6
#xaxis: 10 years, daily data point
#xfit=mdates.date2num(sunpy.time.parse_time('2007-01-01'))+np.arange(0,365*10)
#MESSENGER
#sigma=1000
#bfitmax=80
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='darkgrey',linestyle='-',markersize=0, label='Mercury fit')
#VEX
#inital guess
#sigma=1000
#bfitmax=40
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='orange',linestyle='-',markersize=0, label='Venus fit')
#Wind
#sigma=1000
#bfitmax=10
#mu=mdates.date2num(sunpy.time.parse_time('2013-01-01'))
#ygauss=1/(sigma*np.sqrt(2*np.pi))*np.exp(-((xfit-mu)**2)/(2*sigma**2) )
#normalize with 1/max(ygauss)
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='mediumseagreen',linestyle='-',markersize=0, label='Earth fit')
#for Mars: reconstruct likely parameters if sigma is quite similar for all fits, take mean of those sigmas and adjust bfitmax as function of distance with power law)
#plot reconstructed function for Mars
#bfitmax=6
#plt.plot_date(xfit, ygauss*1/max(ygauss)*bfitmax,'o',color='steelblue',linestyle='--',markersize=0, label='Mars reconstr.')
plt.legend(loc=1,fontsize=fsize-2)
#limits solar min/rise/max
vlevel=150
plt.axvspan(minstart,minend, color='green', alpha=0.1)
plt.annotate('solar minimum',xy=(minstart+(minend-minstart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(minstart+10,vlevel),ha='left')
plt.annotate('>',xy=(minend-10,vlevel),ha='right')
plt.axvspan(risestart,riseend, color='yellow', alpha=0.1)
plt.annotate('rising phase',xy=(risestart+(riseend-risestart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(risestart+10,vlevel),ha='left')
plt.annotate('>',xy=(riseend-10,vlevel),ha='right')
plt.axvspan(maxstart,maxend, color='red', alpha=0.1)
plt.annotate('solar maximum',xy=(maxstart+(maxend-maxstart)/2,vlevel),color='black', ha='center')
plt.annotate('<',xy=(maxstart+10,vlevel),ha='left')
plt.annotate('>',xy=(maxend,vlevel),ha='right')
plt.plot_date( [minstart,minend], [np.mean(mo_bmean[iwinind_min]), \
np.mean(mo_bmean[iwinind_min])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [minstart,minend], [np.mean(mo_bmean[ivexind_min]), \
np.mean(mo_bmean[ivexind_min])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [minstart,minend], [np.mean(mo_bmean[imesind_min]), \
np.mean(mo_bmean[imesind_min])], color='darkgrey', linestyle='-', markersize=0)
plt.plot_date( [risestart,riseend], [np.mean(mo_bmean[iwinind_rise]), \
np.mean(mo_bmean[iwinind_rise])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [risestart,riseend], [np.mean(mo_bmean[ivexind_rise]), \
np.mean(mo_bmean[ivexind_rise])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [risestart,riseend], [np.mean(mo_bmean[imesind_rise]), \
np.mean(mo_bmean[imesind_rise])], color='darkgrey', linestyle='-', markersize=0)
plt.plot_date( [maxstart,maxend], [np.mean(mo_bmean[iwinind_max]), \
np.mean(mo_bmean[iwinind_max])], color='mediumseagreen', linestyle='-',markersize=0 )
plt.plot_date( [maxstart,maxend], [np.mean(mo_bmean[ivexind_max]), \
np.mean(mo_bmean[ivexind_max])], color='orange', linestyle='-', markersize=0)
plt.plot_date( [maxstart,maxend], [np.mean(mo_bmean[imesind_max]), \
np.mean(mo_bmean[imesind_max])], color='darkgrey', linestyle='-', markersize=0)
plt.ylabel('Magnetic field in MO [nT]', fontsize=fsize)
plt.xlabel('Year', fontsize=fsize)
fsize=14
plt.xlim(mdates.date2num(sunpy.time.parse_time('2007-01-01')), mdates.date2num(sunpy.time.parse_time('2016-12-31')))
plt.ylabel('Magnetic field in MO [nT]', fontsize=fsize)
plt.xlabel('Year', fontsize=fsize)
plt.tight_layout()
plt.yticks(fontsize=fsize)
plt.xticks(fontsize=fsize)
plt.legend(loc=1,fontsize=fsize-1)
plt.tight_layout()
plt.savefig('plots_stats/icme_total_field_distance_time_paper.pdf', dpi=300)
plt.savefig('plots_stats/icme_total_field_distance_time_paper.png', dpi=300)
########### RESULTS
print()
print()
print('Magnetic field B MO_BMEAN results, mean +/- std [nT]')
print()
print('Mercury ', round(np.mean(mo_bmean[imercind]),1),' +/- ', round(np.std(mo_bmean[imercind]),1))
#print('min ', round(np.mean(mo_bmean[imercind_min]),1), ' +/- ', round(np.std(mo_bmean[imercind_min]),1))
print('min no events')
print('rise ', round(np.mean(mo_bmean[imercind_rise]),1), ' +/- ', round(np.std(mo_bmean[imercind_rise]),1))
print('max ', round(np.mean(mo_bmean[imercind_max]),1), ' +/- ', round(np.std(mo_bmean[imercind_max]),1))
print()
print('Venus ', round(np.mean(mo_bmean[ivexind]),1),' +/- ', round(np.std(mo_bmean[ivexind]),1))
print('min ', round(np.mean(mo_bmean[ivexind_min]),1), ' +/- ', round(np.std(mo_bmean[ivexind_min]),1))
print('rise ', round(np.mean(mo_bmean[ivexind_rise]),1), ' +/- ', round(np.std(mo_bmean[ivexind_rise]),1))
print('max ', round(np.mean(mo_bmean[ivexind_max]),1), ' +/- ', round(np.std(mo_bmean[ivexind_max]),1))
print()
print('Earth ', round(np.mean(mo_bmean[iwinind]),1),' +/- ', round(np.std(mo_bmean[iwinind]),1))
print('min ', round(np.mean(mo_bmean[iwinind_min]),1), ' +/- ', round(np.std(mo_bmean[iwinind_min]),1))
print('rise ', round(np.mean(mo_bmean[iwinind_rise]),1), ' +/- ', round(np.std(mo_bmean[iwinind_rise]),1))
print('max ', round(np.mean(mo_bmean[iwinind_max]),1), ' +/- ', round(np.std(mo_bmean[iwinind_max]),1))
print()
print('MAVEN only declining phase')
print('decl ',round(np.mean(mo_bmean[imavind]),1),' +/- ', round(np.std(mo_bmean[imavind]),1))
############### (3) TIME SPENT INSIDE CMEs in %, as function of solar cycle ##############
print()
print('-------------------------------------------------')
print('3 Time spent inside CMEs for each planet, 3 figure panels')
print()
#make bin for each year for yearly histograms
yearly_start_times=[mdates.date2num(sunpy.time.parse_time('2007-01-01')),
mdates.date2num(sunpy.time.parse_time('2008-01-01')),
mdates.date2num(sunpy.time.parse_time('2009-01-01')),
mdates.date2num(sunpy.time.parse_time('2010-01-01')),
mdates.date2num(sunpy.time.parse_time('2011-01-01')),
mdates.date2num(sunpy.time.parse_time('2012-01-01')),
mdates.date2num(sunpy.time.parse_time('2013-01-01')),
mdates.date2num(sunpy.time.parse_time('2014-01-01')),
mdates.date2num(sunpy.time.parse_time('2015-01-01')),
mdates.date2num(sunpy.time.parse_time('2016-01-01')),
mdates.date2num(sunpy.time.parse_time('2017-01-01'))]
yearly_end_times=[mdates.date2num(sunpy.time.parse_time('2007-12-31')),
mdates.date2num(sunpy.time.parse_time('2008-12-31')),
mdates.date2num(sunpy.time.parse_time('2009-12-31')),
mdates.date2num(sunpy.time.parse_time('2010-12-31')),
mdates.date2num(sunpy.time.parse_time('2011-12-31')),
mdates.date2num(sunpy.time.parse_time('2012-12-31')),
mdates.date2num(sunpy.time.parse_time('2013-12-31')),
mdates.date2num(sunpy.time.parse_time('2014-12-31')),
mdates.date2num(sunpy.time.parse_time('2015-12-31')),
mdates.date2num(sunpy.time.parse_time('2016-12-31')),
mdates.date2num(sunpy.time.parse_time('2017-12-31'))]
yearly_mid_times=[mdates.date2num(sunpy.time.parse_time('2007-07-01')),
mdates.date2num(sunpy.time.parse_time('2008-07-01')),
mdates.date2num(sunpy.time.parse_time('2009-07-01')),
mdates.date2num(sunpy.time.parse_time('2010-07-01')),
mdates.date2num(sunpy.time.parse_time('2011-07-01')),
mdates.date2num(sunpy.time.parse_time('2012-07-01')),
mdates.date2num(sunpy.time.parse_time('2013-07-01')),
mdates.date2num(sunpy.time.parse_time('2014-07-01')),
mdates.date2num(sunpy.time.parse_time('2015-07-01')),
mdates.date2num(sunpy.time.parse_time('2016-07-01')),
mdates.date2num(sunpy.time.parse_time('2017-07-01'))]
########### 1a Determine SOLAR WIND ONLY MISSIONS STA, STB, Wind
########### all are available in 1 minute time resolution
#define arrays and fill with nan
total_data_days_yearly_win=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_win.fill(np.nan)
total_data_days_yearly_sta=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_sta.fill(np.nan)
total_data_days_yearly_stb=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_stb.fill(np.nan)
total_data_days_yearly_mes=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_mes.fill(np.nan)
total_data_days_yearly_merc=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_merc.fill(np.nan)
total_data_days_yearly_vex=np.zeros(np.size(yearly_mid_times))
total_data_days_yearly_vex.fill(np.nan)