MOCCA

MOCCA-SURVEY-2, file initmodel.dat

Arkadiusz Hypki — Wed, 20 Jan 2021 09:35:36 GMT

File initmodel.dat contains initial parameters of single stars and binaries of a star cluster.

List of columns in the initmodel.dat file:

MOCCA-SURVEY-2, file snapshot.dat

Arkadiusz Hypki — Wed, 20 Jan 2021 09:34:37 GMT

File snapshot.dat contains snapshots of all single stars and binaries of a star cluster for every 200 Myrs.

List of columns in the snapshot.dat file:
name: im, type: INTEGER, column: 1
star/binary name (inames/inameb)

name: hist1, type: LONG, column: 22
compact history for the first starOne number which holds compact information aboutinteresting events which happened for the star:000000000001 - had dynamical collision (interaction)000000000010 - had binary merger (stellar evolution)000000000100 - had MT (increased the mass)000000001000 - had interaction000000010000 - had exchange000000100000 - went to a binary (interaction)000001000000 - went to single (dissolution in stellar evolution)000010000000 - went to single (interaction)000100000000 - separation changed by 1%001000000000 - separation changed by 10%010000000000 - eccentricity changed by 1%100000000000 - eccentricity changed by 10%E.g. if the star had two dynamical collisions and 5 MT then it has:0000000052E.g. Max value is 9, so if the star would had 100 collisions and 100 MT then it would have:0000000099The easiest way to use this column in AWK to getnumber of e.g. binary mergers is:awk '{if ( int(($36%100)/10) > 0) print $0;}' kick.dat

MOCCA-SURVEY-2, file system.dat

Arkadiusz Hypki — Wed, 20 Jan 2021 09:24:59 GMT

File system.dat contains parameters of a star cluster for every time-step.

List of columns in the system.dat file:

name: etot, type: DOUBLE, column: 4
total energy in MC units (ideally should be equal to0.25)

name: de, type: DOUBLE, column: 8
energy error in MC units in one overall time step

name: enepot, type: DOUBLE, column: 9
total potential energy changes due to collisions,binary formation, binary mergers or binarydissruptions (in MC units)

name: rcn, type: DOUBLE, column: 12
core radius in pc (not mass weighted)

name: rchut, type: DOUBLE, column: 13
core radius in pc according casertano & hut (densityweighted)

name: rchut2, type: DOUBLE, column: 14
core radius in pc according casertano & hut(density^2 weighted)

name: rcob, type: DOUBLE, column: 15
core radius in pc determined as for observations(distance at which surface brightnes is equal to halfthe central one

name: rhob, type: DOUBLE, column: 18
half-luminosity radius in pc (observational)

name: vc, type: DOUBLE, column: 24
central velocity dispersion in km/s (mass weighted)

name: vcn, type: DOUBLE, column: 25
central velocity in km/s (not mass weighted)

name: rohut, type: DOUBLE, column: 27
central density in pc according casertano & hut inMsun/pc^3

name: smsm, type: DOUBLE, column: 29
maximum mass of single ms stars in Msun

name: ssmsm, type: DOUBLE, column: 31
maximum mass of ms stars in binaries in Msun

name: ssbhm, type: DOUBLE, column: 32
maximum mass of bh in binaries in Msun

name: csb, type: DOUBLE, column: 34
central surface brightness in mag/pc^2

name: ppmax, type: DOUBLE, column: 35
maximum p_dot/p for milisecond pulsars

name: sescrt, type: DOUBLE, column: 38
total mass loss in Msun due to adjustment ot the tidalradius

name: nescrt, type: INTEGER, column: 39
total number of escapers due to adjustment ot thetidal radius

name: arc, type: DOUBLE, column: 40
average mass in Msun inside core radius (rc)

name: archut2, type: DOUBLE, column: 41
average mass in Msun inside core radius (rchut2)

name: a1p, type: DOUBLE, column: 42
average mass in Msun inside 1% lagrangian radius

name: a10p, type: DOUBLE, column: 43
average mass in Msun inside 10% lagrangian radius

name: a50p, type: DOUBLE, column: 44
average mass in Msun inside 50% lagrangian radius

name: a70p, type: DOUBLE, column: 45
average mass in Msun inside 70% lagrangian radius

name: atot, type: DOUBLE, column: 46
average mass in Msun inside 100% lagrangian radius

name: nt, type: INTEGER, column: 48
actual number of objects (an object is a single star ora binary)

name: nt0, type: INTEGER, column: 49
number of objects including dissrupted binaries andmerged objects (always greater than the initial nt)

name: irchut2, type: INTEGER, column: 51
number of objects in the core (rchut2)

name: nmloev, type: INTEGER, column: 54
total number of mass loss due to stellar evolution

name: escns, type: INTEGER, column: 55
total number of ns escaped from the system

name: escsta, type: DOUBLE, column: 56
total energy of escapers (MC units)

name: ebin, type: DOUBLE, column: 57
actual binding energy of binaries in the system (MCunits)

name: ehbint, type: DOUBLE, column: 58
total binary binding energy - energy generated indynamical interactions + binding energy ofprimordial binaries (MC units)

name: ehbin3, type: DOUBLE, column: 59
total heating due to binary-star interactions (MCunits)

name: ehb3b3, type: DOUBLE, column: 60
total heating by binary-binary interactions (MCunits)

name: embin3, type: DOUBLE, column: 61
total energy loss in binary-single merger in Fewbody(MC units)

name: emb3b3, type: DOUBLE, column: 62
total energy loss in binary-binary merger in Fewbody(MC units)

name: escb3s, type: DOUBLE, column: 63
energy of star escapers in binary interactions (MCunits)

name: escbi3, type: DOUBLE, column: 64
energy of binary escapers n binary interactions (MCunits)

name: escbb3, type: DOUBLE, column: 65
internal binding energy of binary escapers in binaryinteractions (MC units)

name: ehmlev, type: DOUBLE, column: 66
total heating by mass loss due to stellar evolution(MC units)

name: ehcoll, type: DOUBLE, column: 67
total heating due to stellar collisions (MC units)

name: eccoll, type: DOUBLE, column: 68
total cooling due to stellar collisions (MC units)

name: nbin3, type: INTEGER, column: 69
number of all binaries initial primordial anddynamicaly formed

name: ncoll, type: INTEGER, column: 70
total number of stellar collisions

name: nb3fin, type: INTEGER, column: 71
total number of interactions between three-bodybinaries and field stars

name: nb3b3, type: INTEGER, column: 72
total number of binary-binary interactions

name: nescb3, type: INTEGER, column: 73
total number of escaped binaries due tointeractions

name: nesb3s, type: INTEGER, column: 74
total number of star escapers because ofinteractions

name: ndist3, type: INTEGER, column: 75
total number of dissolved binaries in binary-singleinteractions

name: ndist4, type: INTEGER, column: 76
total number of dissolved binaries in binary-binaryinteractions

name: ndiste, type: INTEGER, column: 77
total number of dissolved binaries because of binaryevolution

name: nmerg3, type: INTEGER, column: 78
total number of merged binaries in binary-singleinteractions

name: nmerg4, type: INTEGER, column: 79
total number of merged binaries in binary-binaryinteractions

name: nmerge, type: INTEGER, column: 80
total number of merged binaries due to stellarevolution

name: idestr, type: INTEGER, column: 81
number of binaries destryed due to interactions

name: ibiesc, type: INTEGER, column: 83
number of binaries escaped due to interactions

name: ibirel, type: INTEGER, column: 84
number of binaries escaped due to relaxation

name: nactbin, type: INTEGER, column: 85
nbin3-nescb3-ndist3-ndist4-ndiste-nmerg3-nmerg4-nmergeactual number of binaries

name: nexchang, type: INTEGER, column: 86
total number of exchanges in binary-singleinteractions

name: nexchang2, type: INTEGER, column: 87
total number of exchanges in binary-binaryinteractions

name: sloses, type: DOUBLE, column: 88
total mass loss in Msun due to the relaxation process

name: slosev, type: DOUBLE, column: 89
total mass loss in Msun due to stellar evolutin

name: slosco, type: DOUBLE, column: 90
total mass loss in Msun due to stellar collisions

name: slob3s, type: DOUBLE, column: 91
mass loss in Msun of stars in binary-starinteractions

name: slob3b, type: DOUBLE, column: 92
mass loss in Msun of binaries in binary-binaryinteractions

name: bsEM, type: INTEGER, column: 93
actual number of blue stragglers formed in binaryevolution mergers

name: bsEMT, type: INTEGER, column: 94
actual number of blue stragglers formed in binaryevolution mass transfers

name: bsED, type: INTEGER, column: 95
actual number of blue stragglers formed in binaryevolution binary dissolution

name: bsCSS, type: INTEGER, column: 96
actual number of blue stragglers formed incollisions

name: bsCBS, type: INTEGER, column: 97
actual number of blue stragglers formed inbinary-star interactions

name: bsCBB, type: INTEGER, column: 98
actual number of blue stragglers formed inbinary-binary interactions

name: bsEXBS, type: INTEGER, column: 99
actual number of blue stragglers formed inbinary-single exchenges

name: bsEXBB, type: INTEGER, column: 100
actual number of blue stragglers formed inbinary-binary exchenges

name: bsDBS, type: INTEGER, column: 101
actual number of blue stragglers formed inbinary-single dissolutions

name: bsDBB, type: INTEGER, column: 102
actual number of blue stragglers formed inbinary-binary dissolutions

name: nbss, type: INTEGER, column: 103
bsEM+bsEMT+bsED+bsCSS+bsCBS+bsCBB+bsEXBS+bsEXBB+bsDBS+bsDBBactual number of blue stragglers in the system

name: ibssingle, type: INTEGER, column: 104
number of single blue stragglers

name: ibsdouble, type: INTEGER, column: 105
number of binary blue stragglers

name: tbss, type: INTEGER, column: 106
tEM+tEMT+tED+tCSS+tCBS+tCBB total number of bluestragglers

name: tEM, type: INTEGER, column: 107
total number of blue stragglers formed in binaryevolutions mergers

name: tEMT, type: INTEGER, column: 108
total number of blue stragglers formed in binaryevolution mass transfers

name: tED, type: INTEGER, column: 109
actual number of blue stragglers formed in binaryevolution binary dissolutions

name: tCSS, type: INTEGER, column: 110
total number of blue stragglers formed in collisions

name: tCBS, type: INTEGER, column: 111
total number of blue stragglers formed inbinary-star interactions

name: tCBB, type: INTEGER, column: 112
total number of blue stragglers formed inbinary-binary interactions

name: fEM, type: INTEGER, column: 113
number of blue stragglers for which formation typewas binary evolution mergers

name: fEMT, type: INTEGER, column: 114
actual number of blue stragglers formed in binaryevolution mass transfers

name: fED, type: INTEGER, column: 115
actual number of blue stragglers formed in binaryevolution binary dissolution

name: fCSS, type: INTEGER, column: 116
actual number of blue stragglers formed incollisions

name: fCBS, type: INTEGER, column: 117
actual number of blue stragglers formed inbinary-star interactions

name: fCBB, type: INTEGER, column: 118
actual number of blue stragglers formed inbinary-binary interactions

name: fEXBS, type: INTEGER, column: 119
actual number of blue stragglers formed inbinary-single exchenges

name: fEXBB, type: INTEGER, column: 120
actual number of blue stragglers formed inbinary-binary exchenges

name: fDBS, type: INTEGER, column: 121
actual number of blue stragglers formed inbinary-single dissolutions

name: fDBB, type: INTEGER, column: 122
actual number of blue stragglers formed inbinary-binary dissolutions KICKS

name: ekickt, type: DOUBLE, column: 123
total kinetic energy of ns/bh after supernoveexplosion and natal kick (only single stars) (MCunits)

name: ekicktbs, type: DOUBLE, column: 124
total kinetic energy of binary cm after supernoveexplosion and natal kick (only binaries) (MC units)

name: ekicktbd, type: DOUBLE, column: 125
total kinetic energy of binary components afterbinary disruption due to supernove axplosion andnatal kick (only binaries) (MC units)

name: ekicktbm, type: DOUBLE, column: 126
total kinetic energy of merged binaries due tosupernove explosion and natal kick (MC units)

name: ekicktb2, type: DOUBLE, column: 127
total kinetic energy of second binary componentafter supernove explosion and binary disruption(only binaries) (MC units)

name: ekicktwd, type: DOUBLE, column: 128
total kinetic energy of wd after natal kicks (MCunits)

name: ikickt, type: INTEGER, column: 129
total number of ns/bh after supernove explosion andnatal kick (only single stars)

name: ikicktbs, type: INTEGER, column: 130
total number of binary cm after supernove explosionand natal kick (only binaries)

name: ikicktbd, type: INTEGER, column: 131
total number of binary components after binarydisruption due to supernove axplosion and natal kick(only binaries)

name: ikicktbm, type: INTEGER, column: 132
total number of merged binaries due to supernoveexplosion and natal kicks

name: ikicktwd, type: INTEGER, column: 133
total number of wd natal kicks

name: ntsn1, type: INTEGER, column: 134
total number of ns/bh removed from the system after snnatal kick

name: ntsn2, type: INTEGER, column: 135
total number of merged binaries removed from thesystem after sn natal kick

name: ntsnb, type: INTEGER, column: 136
total number of binaries removed from the systemafter sn natal kick

name: ntsn3, type: INTEGER, column: 137
total number of first binary components removed fromthe system after sn natal kick

name: ntsn4, type: INTEGER, column: 138
total number of second binary components removedfrom the system after sn natal kick

name: ntwd1, type: INTEGER, column: 139
total number of wd removed from the system after wdnatal kicks

name: lhg, type: INTEGER, column: 144
actual number of single hertzsprung_gap stars

name: lgb, type: INTEGER, column: 145
actual number of single giant_branch stars

name: lch, type: INTEGER, column: 146
actual number of single core_helium stars

name: lfag, type: INTEGER, column: 147
actual number of single first_agb stars

name: lsag, type: INTEGER, column: 148
actual number of single second_agb stars

name: lhms, type: INTEGER, column: 149
actual number of single helium_ms stars

name: lhhg, type: INTEGER, column: 150
actual number of single helium_hg stars

name: lhgb, type: INTEGER, column: 151
actual number of single helium_gb stars

name: lot, type: INTEGER, column: 152
actual number of single stars out of mainsequence

name: l2wd, type: INTEGER, column: 153
actual number of wd-wd binaries

name: l2ns, type: INTEGER, column: 154
actual number of ns-ns binaries

name: l2bh, type: INTEGER, column: 155
actual number of bh-bh binaries

name: lmsms, type: INTEGER, column: 156
actual number of ms-ms binaries

name: lwdms, type: INTEGER, column: 157
actual number of wd-ms binaries

name: lwdns, type: INTEGER, column: 158
actual number of wd-ns binaries

name: lwdbh, type: INTEGER, column: 159
actual number of wd-bh binaries

name: lwdot, type: INTEGER, column: 160
actual number of wd-out of ms binaries

name: lnsms, type: INTEGER, column: 161
actual number of ns-ms binaries

name: lnsbh, type: INTEGER, column: 162
actual number of ns-bh binaries

name: lnsot, type: INTEGER, column: 163
actual number of ns-out of ms binaries

name: lbhms, type: INTEGER, column: 164
actual number of bh-ms binaries

name: lbhot, type: INTEGER, column: 165
actual number of bh-out of ms binaries

name: ldgdg, type: INTEGER, column: 166
actual number of degenerate-degenerate binaries

name: ldgot, type: INTEGER, column: 167
actual number of degenerate-out binaries

name: lmsot, type: INTEGER, column: 168
actual number of ms-out of ms binaries

name: lotot, type: INTEGER, column: 169
actual number of out of ms-out of ms binaries

name: lbh2, type: INTEGER, column: 170
actual number of bh formed in collisions

name: lbh3, type: INTEGER, column: 171
actual number of bh formed in binary mergers

name: xhg, type: DOUBLE, column: 176
mass of single hertzsprung_gap stars

name: xgb, type: DOUBLE, column: 177
msss of single giant_branch stars

name: xch, type: DOUBLE, column: 178
mass of single core_helium stars

name: xsag, type: DOUBLE, column: 180
mass of single second_agb stars

name: xot, type: DOUBLE, column: 184
mass of stars out of main sequence in Msun

name: xmsms, type: DOUBLE, column: 185
mass of ms-ms binaries in Msun

name: xwdwd, type: DOUBLE, column: 186
mass of wd-wd binaries in Msun

name: xnsns, type: DOUBLE, column: 187
mass of ns-ns binaries in Msun

name: xbhbh, type: DOUBLE, column: 188
mass of bh-bh binaries in Msun

name: xwdms, type: DOUBLE, column: 189
mass of wd-ms binaries in Msun

name: xnsms, type: DOUBLE, column: 193
mass of ns-ms binaries in Msun

name: xbhms, type: DOUBLE, column: 196
mass of bh-ms binaries in Msun

name: xdgdg, type: DOUBLE, column: 198
mass of degenerate-degenerate binaries in Msun

name: xdgot, type: DOUBLE, column: 199
mass of degenerate-out of ms binaries in Msun

name: xmsot, type: DOUBLE, column: 200
mass of ms-out of ms binaries in Msun

name: xotot, type: DOUBLE, column: 201
mass of out of ms-out of ms binaries in Msun

name: nbinrc, type: INTEGER, column: 202
number of binaries inside rc

name: nbinrchut2, type: INTEGER, column: 203
number of binaries inside rchut2

name: nbin1, type: INTEGER, column: 204
number of binaries inside r1%

name: nbin10, type: INTEGER, column: 205
number of binaries inside r1% < r < r10%

name: nbin50, type: INTEGER, column: 206
number of binaries inside r10% < r < r50%

name: nbinrt, type: INTEGER, column: 207
number of binaries inside r50% < r < rt

name: xmbinrc, type: DOUBLE, column: 208
mass of binaries inside rc in Msun

name: xmbinrchut2, type: DOUBLE, column: 209
mass of binaries inside rchut2 in Msun

name: xmbin1, type: DOUBLE, column: 210
mass of binaries inside r1% in Msun

name: xmbin10, type: DOUBLE, column: 211
mass of binaries inside r1% < r < r10% in Msun

name: xmbin50, type: DOUBLE, column: 212
mass of binaries inside r10% < r < r50% in Msun

name: xmbinrt, type: DOUBLE, column: 213
mass of binaries inside r50% < r < rt in Msun

name: xebinrc, type: DOUBLE, column: 214
binding energy of binaries inside rc (MC units)

name: xebinrchut2, type: DOUBLE, column: 215
binding energy of binaries inside rchut2 (MC units)

name: xebin1, type: DOUBLE, column: 216
binding energy of binaries inside r1% (MC units)

name: xebin10, type: DOUBLE, column: 217
binding energy of binaries inside r1% < r < r10% (MCunits)

name: xebin50, type: DOUBLE, column: 218
binding energy of binaries inside r10% < r < r50% (MCunits)

name: xebinrt, type: DOUBLE, column: 219
binding energy of binaries inside r50% < r < rt (MCunits)

name: ntridisr, type: INTEGER, column: 220
total number of triples manually disrupted afterfewbody numerical integration

name: ntridisr2, type: INTEGER, column: 221
total number of quadruples manually disrupted afterfewbody numerical integration

name: iebinkt01, type: INTEGER, column: 222
number of binaries with binding energy smaller than0.1kT

name: ilostdis3, type: INTEGER, column: 223
number of binaries manually disrupted usingHeggie's probability formula or mean core distanceor some other criterion (binary-single case)

name: ilostMar0, type: INTEGER, column: 224
number triples and quadruple when mardlingcriterion is not fulfilled

name: ilostMar1, type: INTEGER, column: 225
number triples and quadruple when mardlingcriterion is fulfilled

name: ilostCpuMax, type: INTEGER, column: 226
number of interactions not finished after 10 CPU s

name: fbCases1, type: INTEGER, column: 227
number of all dynamical interactions

name: fbCases3, type: INTEGER, column: 228
number of binary-star interactions --> 1 2 3

name: fbCases4, type: INTEGER, column: 229
number of binary-binary interactions --> 1 2 3 4

name: fbCases11, type: INTEGER, column: 230
number of binary-star interactions --> [1 2] 3

name: fbCases12, type: INTEGER, column: 231
number of binary-binary interactions --> [1 2] 3 4

name: fbCases20, type: INTEGER, column: 232
number of binary-binary interactions --> [1 2] [3 4]

name: fbCases31, type: INTEGER, column: 233
number of binary-star interactions --> [3 2] 1

name: fbCases32, type: INTEGER, column: 234
number of binary-binary interactions --> [3 2] 1 4

name: fbCases60, type: INTEGER, column: 235
number of binary-binary interactions --> [3 2] [1 4]

name: fbCases100, type: INTEGER, column: 236
number of [1 2] 3 -> 1:2:3 OR [1 2] [3 4] -> 1:2:3:4

name: fbCases101, type: INTEGER, column: 237
number of [1 2] 3 -> 1:2 3 OR [1 2] [3 4] -> 1:2:3 4

name: fbCases102, type: INTEGER, column: 238
number of binary-binary interactions --> 1:2 3 4

name: fbCases110, type: INTEGER, column: 239
number of binary-binary interactions --> 1:2 [3 4]

name: fbCases130, type: INTEGER, column: 240
number of binary-star interactions --> 1:3 [2 4]

name: fbCases330, type: INTEGER, column: 241
number of binary-star interactions --> [1:3 2]

name: fbCases331, type: INTEGER, column: 242
number of binary-star interactions --> [1:3 2] 4

name: fbCases630, type: INTEGER, column: 243
number of binary-binary interactions --> [1:3 2:4]

name: nescm, type: INTEGER, column: 244
total number of massless objects removed from thesystem

name: ivnewg, type: INTEGER, column: 245
number of relaxation events when 'vnew' is < 0

name: ivrr, type: INTEGER, column: 246
total number of relaxed objects from time = 0

name: enrad, type: DOUBLE, column: 247
total energy correction due to problems with thedetermination of the new velocity in the relaxationstep in MC units

name: ebinkt0001, type: DOUBLE, column: 248
total binding energy of binaries with binding energysmaller than 0.1kT (MC units)

name: elostdis, type: DOUBLE, column: 249
binding energy lost during manual disruption usingHeggie's probability formula or mean core distanceor some other criterion (MC units)

name: elostMar1, type: DOUBLE, column: 250
energy lost during manual disruption of triple andquadruple when mardling criterion is fulfilled (MCunits)

name: elostMar0, type: DOUBLE, column: 251
energy lost during manual disruption of triple andquadruple when mardling criterion is NOT fulfilled(MC units)

name: elostCpuMax, type: DOUBLE, column: 252
energy lost during manual disruption of triple andquadruple when CPU > max [sec] (MC units)

name: nsuzon, type: INTEGER, column: 253
number of super-zones in the cluster

name: smtrt, type: DOUBLE, column: 254
mass of stars outside the tidal radius in Msun

name: ntrt, type: INTEGER, column: 255
number of stars outside the tidal radius

name: thspitzer, type: DOUBLE, column: 256
spitzer half-mass relaxation time in Myr

name: cpurelaxall, type: DOUBLE, column: 257
CPU time in second spent in relaxall function

name: cpurelax, type: DOUBLE, column: 258
CPU time in second spent in relax function

name: cpubs, type: DOUBLE, column: 259
CPU time in second spent in intb3f function

name: cpubb, type: DOUBLE, column: 260
CPU time in second spent in intb3b3 function

name: cpucoepot, type: DOUBLE, column: 261
CPU time in second spent in coepot function

name: cputimepot, type: DOUBLE, column: 262
CPU time in second spent in timepot function

name: cpuss, type: DOUBLE, column: 263
CPU time in second spent in intcol function

name: cpuformb3, type: DOUBLE, column: 264
CPU time in second spent in formb3 function

name: cpuescape, type: DOUBLE, column: 265
CPU time in second spent in escape function

name: cpuoutput, type: DOUBLE, column: 266
CPU time in second spent in output function

name: cpuprofiles, type: DOUBLE, column: 267
CPU time in second spent in profiles function

name: cpuoutput1, type: DOUBLE, column: 268
CPU time in second spent in output1 function

name: cpusnap, type: DOUBLE, column: 269
CPU time in second spent in snapshot function

name: cpumloss, type: DOUBLE, column: 270
CPU time in second spent in output-mloss function

name: cpumlossjarr, type: DOUBLE, column: 271
CPU time in second spent in mloss-jarrod function

name: cpuprofiles1, type: DOUBLE, column: 272
CPU time in second spent in profiles1 function

name: cpufb, type: DOUBLE, column: 273
CPU time in second spent in Fewbody function

name: cputree, type: DOUBLE, column: 274
CPU time in second spent in kdetree function

name: cpumlosssin, type: DOUBLE, column: 275
CPU time in second spent in mloss_single function

name: fbrestarts, type: INTEGER, column: 276
number of restarted Fewbody interactions

name: fbunfinished, type: INTEGER, column: 277
number of Fewbody interactions which were notfinished with good enough energy conservation

name: fbmaxcpu, type: INTEGER, column: 278
number of Fewbody interaction which were finisheddue to max 10 seconds limitation

name: fbnoremnant, type: INTEGER, column: 279
number of no_remnant object created for multiplemergers after calling Fewbody

name: outputId, type: INTEGER, column: 280
output ID, it's unique for whole simulation

name: fbksrestarts, type: INTEGER, column: 281
Fewbody restarts count with KS = 1

name: fbbrestarts, type: INTEGER, column: 282
Fewbody restarts count with impact parameterincreased by 10%

name: totl, type: DOUBLE, column: 283
total cluster luminosity in Lsun

name: rbh10, type: DOUBLE, column: 284
10% lagrangian radius for single BHs

name: rbh50, type: DOUBLE, column: 285
50% lagrangian radius for single BHs

name: rbh70, type: DOUBLE, column: 286
70% lagrangian radius for single BHs

name: rbh210, type: DOUBLE, column: 289
10% lagrangina radius for BH in binaries and single

name: rbh250, type: DOUBLE, column: 290
50% lagrangina radius for BH in binaries and single

name: rbh270, type: DOUBLE, column: 291
70% lagrangina radius for BH in binaries and single

name: rbc10, type: DOUBLE, column: 294
10% lagrangina radius for binaries with period < 10d

name: rbc50, type: DOUBLE, column: 295
50% lagrangina radius for binaries with period < 10d

name: rbc70, type: DOUBLE, column: 296
70% lagrangina radius for binaries with period < 10d

name: smbc, type: DOUBLE, column: 297
mass of all binaries with period < 10d

name: kbc, type: INTEGER, column: 298
number of all binaries with period < 10d

name: rbs10, type: DOUBLE, column: 299
10% lagrangina radius for binaries with period > 10d

name: rbs50, type: DOUBLE, column: 300
50% lagrangina radius for binaries with period > 10d

name: rbs70, type: DOUBLE, column: 301
70% lagrangina radius for binaries with period > 10d

name: smbs, type: DOUBLE, column: 302
mass of all binaries with period > 10d

name: kbs, type: INTEGER, column: 303
number of all binaries with period > 10d

name: rbhm10, type: DOUBLE, column: 304
10% lagrangina radius for binaries with mass >2average mass*

name: rbhm50, type: DOUBLE, column: 305
50% lagrangina radius for binaries with mass >2average mass*

name: rbhm70, type: DOUBLE, column: 306
70% lagrangina radius for binaries with mass >2average mass*

name: smbhm, type: DOUBLE, column: 307
mass of all binaries with mass > 2average mass*

name: kbhm, type: INTEGER, column: 308
number of all binaries with mass > 2average mass*

name: rblm10, type: DOUBLE, column: 309
10% lagrangina radius for binaries with mass <2average mass*

name: rblm50, type: DOUBLE, column: 310
50% lagrangina radius for binaries with mass <2average mass*

name: rblm70, type: DOUBLE, column: 311
70% lagrangina radius for binaries with mass <2average mass*

name: smblm, type: DOUBLE, column: 312
mass of all binaries with mass < 2average mass*

name: kblm, type: INTEGER, column: 313
number of all binaries with mass < 2average mass*

name: rimbh10, type: DOUBLE, column: 314
10% lagrangina radius for all objects without IMBH

name: rimbh50, type: DOUBLE, column: 315
50% lagrangina radius for all objects without IMBH

name: rimbh70, type: DOUBLE, column: 316
70% lagrangina radius for all objects without IMBH

name: smimbh, type: DOUBLE, column: 317
mass of the system without IMBH

name: kimbh, type: INTEGER, column: 318
number of all objects without IMB

name: rbss10, type: DOUBLE, column: 319
10% lagrangina radius for BSS

name: rbss50, type: DOUBLE, column: 320
50% lagrangina radius for BSS

name: rbss70, type: DOUBLE, column: 321
70% lagrangina radius for BSS

name: rbcv10, type: DOUBLE, column: 324
10% lagrangina radius for all CVs

name: rbcv50, type: DOUBLE, column: 325
50% lagrangina radius for all CVs

name: rbcv70, type: DOUBLE, column: 326
70% lagrangina radius for all CVs

name: rbcv110, type: DOUBLE, column: 329
10% lagrangina radius for MS-WD CVs

name: rbcv150, type: DOUBLE, column: 330
50% lagrangina radius for MS-WD CVs

name: rbcv170, type: DOUBLE, column: 331
70% lagrangina radius for MS-WD CVs

name: rbcv210, type: DOUBLE, column: 334
10% lagrangina radius for WD-WD CVs

name: rbcv250, type: DOUBLE, column: 335
50% lagrangina radius for WD-WD CVs

name: rbcv270, type: DOUBLE, column: 336
70% lagrangina radius for WD-WD CVs

name: r1popMix, type: DOUBLE, column: 348
r1% lagr for population mix

name: r10popMix, type: DOUBLE, column: 349
r10% lagr for population mix

name: r70popMix, type: DOUBLE, column: 351
r70% lagr for population mix

name: arcpop1, type: DOUBLE, column: 352
avg mass for rc for population 1

name: archut2pop1, type: DOUBLE, column: 353
avg mass for rchut2 for population 1

name: ar1pop1, type: DOUBLE, column: 354
avg mass for r1% lagr for population 1

name: ar10pop1, type: DOUBLE, column: 355
avg mass for r10% lagr for population 1

name: arhpop1, type: DOUBLE, column: 356
avg mass for r_h for population 1

name: ar70pop1, type: DOUBLE, column: 357
avg mass for r70% lagr for population 1

name: arcpop2, type: DOUBLE, column: 358
avg mass for rc for population 2

name: archut2pop2, type: DOUBLE, column: 359
avg mass for rchut2 for population 2

name: ar1pop2, type: DOUBLE, column: 360
avg mass for r1% lagr for population 2

name: ar10pop2, type: DOUBLE, column: 361
avg mass for r10% lagr for population 2

name: arhpop2, type: DOUBLE, column: 362
avg mass for r_h for population 2

name: ar70pop2, type: DOUBLE, column: 363
avg mass for r70% lagr for population 2

name: arcpopMix, type: DOUBLE, column: 364
avg mass for rc for population mix

name: archut2popMix, type: DOUBLE, column: 365
avg mass for rchut2 for population mix

name: ar1popMix, type: DOUBLE, column: 366
avg mass for r1% lagr for population mix

name: ar10popMix, type: DOUBLE, column: 367
avg mass for r10% lagr for population mix

name: arhpopMix, type: DOUBLE, column: 368
avg mass for r_h for population mix

name: ar70popMix, type: DOUBLE, column: 369
avg mass for r70% lagr for population mix

name: nescb3pop1, type: INTEGER, column: 370
total number of escaped binaries for pop 1

name: nescb3pop2, type: INTEGER, column: 371
total number of escaped binaries for pop 2

name: nescb3popMix, type: INTEGER, column: 372
total number of escaped binaries for pop Mix

name: nesb3spop1, type: INTEGER, column: 373
total number of star escapers because ofinteractions for pop1

name: nesb3spop2, type: INTEGER, column: 374
total number of star escapers because ofinteractions for pop2

name: nesb3spopMix, type: INTEGER, column: 375
total number of star escapers because ofinteractions for popMix

name: ndist3pop1, type: INTEGER, column: 376
total number of dissolved binaries (bin-sin, pop 1)

name: ndist3pop2, type: INTEGER, column: 377
total number of dissolved binaries (bin-sin, pop 2)

name: ndist3popMix, type: INTEGER, column: 378
total number of dissolved binaries (bin-sin, popMix)

name: ndist4pop1, type: INTEGER, column: 379
total number of dissolved binaries (bin-bin, pop 1)

name: ndist4pop2, type: INTEGER, column: 380
total number of dissolved binaries (bin-bin, pop 2)

name: ndist4popMix, type: INTEGER, column: 381
total number of dissolved binaries (bin-bin, popMix)

name: ndistepop1, type: INTEGER, column: 382
total number of dissolved binaries (binEvol, pop 1)

name: ndistepop2, type: INTEGER, column: 383
total number of dissolved binaries (binEvol, pop 2)

name: ndistepopMix, type: INTEGER, column: 384
total number of dissolved binaries (binEvol, popMix)

name: nmerg3pop1, type: INTEGER, column: 385
total number of merged binaries (bin-sin, pop 1)

name: nmerg3pop2, type: INTEGER, column: 386
total number of merged binaries (bin-sin, pop 2)

name: nmerg3popMix, type: INTEGER, column: 387
total number of merged binaries (bin-sin, pop Mix)

name: nmerg4pop1, type: INTEGER, column: 388
total number of merged binaries (bin-bin, pop 1)

name: nmerg4pop2, type: INTEGER, column: 389
total number of merged binaries (bin-bin, pop 2)

name: nmerg4popMix, type: INTEGER, column: 390
total number of merged binaries (bin-bin, pop Mix)

name: nmergepop1, type: INTEGER, column: 391
total number of merged binaries (binEvol, pop 1)

name: nmergepop2, type: INTEGER, column: 392
total number of merged binaries (binEvol, pop 2)

name: nmergepopMix, type: INTEGER, column: 393
total number of merged binaries (binEvol, pop Mix)

name: kickloss, type: DOUBLE, column: 394
kick mass loss is counted separately (not through thesloses variable)

name: timenr, type: INTEGER, column: 395
timestep as an integer number, it starts with 0 and itis increased by 1 after finishing the full timestep ofMOCCA. It is needed to easily join differ ent tables ofMOCCA output with each other.

name: pop1c, type: INTEGER, column: 396
number of stars (not objects) from population 1

name: pop2c, type: INTEGER, column: 397
number of stars (not objects) from population 2

name: popMixc, type: INTEGER, column: 398
number of stars (not objects) from mixed population

name: pop1b, type: INTEGER, column: 399
number of binaries from population 1

name: pop2b, type: INTEGER, column: 400
number of binaries from population 2

name: popMixb, type: INTEGER, column: 401
number of binaries from mixed population

name: tphysDiff, type: DOUBLE, column: 402
overall time-step (tphys - tphysLast)

name: semiDetBH, type: INTEGER, column: 403
number of semi-detached binaries with BH

name: semiDetNS, type: INTEGER, column: 404
number of semi-detached binaries with NS

name: semiDetWD, type: INTEGER, column: 405
number of semi-detached binaries with WD

name: semiDetBHm, type: DOUBLE, column: 406
total mass of semi-detached binaries with BH

name: semiDetNSm, type: DOUBLE, column: 407
total mass of semi-detached binaries with NS

name: semiDetWDm, type: DOUBLE, column: 408
total mass of semi-detached binaries with WD

name: iobt, type: INTEGER, column: 409
total number of obliterated object

name: bsPop1, type: INTEGER, column: 410
number of started bin-sin interactions (pop1)

name: bsPop2, type: INTEGER, column: 411
number of started bin-sin interactions (pop2)

name: bsPopMix, type: INTEGER, column: 412
number of started bin-sin interactions (popMix)

name: bbPop1, type: INTEGER, column: 413
number of started bin-bin interactions (pop1)

name: bbPop2, type: INTEGER, column: 414
number of started bin-bin interactions (pop2)

name: bbPopMix, type: INTEGER, column: 415
number of started bin-bin interactions (popMix)

name: colPop1, type: INTEGER, column: 416
number of collision interactions (pop1)

name: colPop2, type: INTEGER, column: 417
number of collision interactions (pop2)

name: colPopMix, type: INTEGER, column: 418
number of collision interactions (popMix)

name: formPop1, type: INTEGER, column: 419
number of binary formation interactions (pop1)

name: formPop2, type: INTEGER, column: 420
number of binary formation interactions (pop2)

name: formPopMix, type: INTEGER, column: 421
number of binary formation interactions (popMix)

name: obsBinFrac, type: DOUBLE, column: 422
Observational binary fraction asN_binary/(N_stars + N_binaries).N_binary is a number of observational binaries, defined as a binary:1. consisting of two MS stars2. with more massive star > 0.4 MSun3. with mass ratio q > 0.54. with more massive star being less than M_turnoff.N_stars is an observatio
nal single star, defined as a star:1. which is a MS star2. with mass > 0.4 MSun.

name: obsBinFracMS, type: DOUBLE, column: 423
Observational binary fraction for MS stars: asN_ms-ms/(N_ms-ms + N_ms).N_ms-ms is a number of observational MS-MS binaries, defined as a binary:1. co nsisting of two MS stars2. with any mass.N_ms is an observational MS single star, defined as a star:1. which is a MS star2. with any mass.

name: escbh, type: INTEGER, column: 424
total number of BHs escaped from the system

name: binEvolMix, type: DOUBLE, column: 425
number of mass transfer events in binary evolutionwhich create mixed population or mass transfer eventswhich occured already for mixed population sta rs

name: pop1cMS, type: INTEGER, column: 426
number of MS stars from population 1(computed separately star by star, not as bound objects)

name: pop2cMS, type: INTEGER, column: 427
number of MS stars from population 2(computed separately star by star, not as bound objects)

name: popMixcMS, type: INTEGER, column: 428
number of MS stars from mixed population(computed separately star by star, not as bound objects)

name: pop1cMSout, type: INTEGER, column: 429
number of out-of-MS stars from population 1(computed separately star by star, not as bound objects)

name: pop2cMSout, type: INTEGER, column: 430
number of out-of-MS stars from population 2(computed separately star by star, not as bound objects)

name: popMixcMSout, type: INTEGER, column: 431
number of out-of-MS stars from mixed population(computed separately star by star, not as bound objects)

name: pop1cWD, type: INTEGER, column: 432
number of WD stars from population 1(computed separately star by star, not as bound objects)

name: pop2cWD, type: INTEGER, column: 433
number of WD stars from population 2(computed separately star by star, not as bound objects)

name: popMixcWD, type: INTEGER, column: 434
number of WD stars from mixed population(computed separately star by star, not as bound objects)

name: pop1cNS, type: INTEGER, column: 435
number of NS stars from population 1(computed separately star by star, not as bound objects)

name: pop2cNS, type: INTEGER, column: 436
number of NS stars from population 2(computed separately star by star, not as bound objects)

name: popMixcNS, type: INTEGER, column: 437
number of NS stars from mixed population(computed separately star by star, not as bound objects)

name: pop1cBH, type: INTEGER, column: 438
number of BH stars from population 1(computed separately star by star, not as bound objects)

name: pop2cBH, type: INTEGER, column: 439
number of BH stars from population 2(computed separately star by star, not as bound objects)

name: popMixcBH, type: INTEGER, column: 440
number of BH stars from mixed population(computed separately star by star, not as bound objects)

name: influSin, type: DOUBLE, column: 441
number of single stars in IMBH influence radius

name: influBin, type: DOUBLE, column: 442
number of binaries in IMBH influence radius

name: influSinNS, type: DOUBLE, column: 443
number of single NSs in IMBH influence radius

name: influBinNS, type: DOUBLE, column: 444
number of binaries with NSs in IMBH influence radius

name: influSinBH, type: DOUBLE, column: 445
number of single BHs in IMBH influence radius

name: influBinBH, type: DOUBLE, column: 446
number of binaries with BHs in IMBH influence radius

name: influSinWD, type: DOUBLE, column: 447
number of single WDs in IMBH influence radius

name: influBinWD, type: DOUBLE, column: 448
number of binaries with WDs in IMBH influence radius

name: influSinMSout, type: DOUBLE, column: 449
number of single out-ofMS in IMBH influence radius

name: influBinMSout, type: DOUBLE, column: 450
number of binaries with out-ofMS in IMBH influenceradius

name: influSinMS, type: DOUBLE, column: 451
number of single MS in IMBH influence radius

name: influBinMS, type: DOUBLE, column: 452
number of binaries with MS in IMBH influenceradius

name: influSinm, type: DOUBLE, column: 453
mass of single stars in IMBH influence radius

name: influBinm, type: DOUBLE, column: 454
mass of binaries in IMBH influence radius

name: influSinNSm, type: DOUBLE, column: 455
mass of single NSs in IMBH influence radius

name: influBinNSm, type: DOUBLE, column: 456
mass of binaries with NSs in IMBH influence radius

name: influSinBHm, type: DOUBLE, column: 457
mass of single BHs in IMBH influence radius

name: influBinBHm, type: DOUBLE, column: 458
mass of binaries with BHs in IMBH influence radius

name: influSinWDm, type: DOUBLE, column: 459
mass of single WDs in IMBH influence radius

name: influBinWDm, type: DOUBLE, column: 460
mass of binaries with WDs in IMBH influence radius

name: influSinMSoutm, type: DOUBLE, column: 461
mass of single out-ofMS in IMBH influence radius

name: influBinMSoutm, type: DOUBLE, column: 462
mass of binaries with out-ofMS in IMBH influenceradius

name: influSinMSm, type: DOUBLE, column: 463
mass of single MS in IMBH influence radius

name: influBinMSm, type: DOUBLE, column: 464
mass of binaries with MS in IMBH influenceradius

name: aplusPop1, type: DOUBLE, column: 465
A parameter for pop 1 (all non compact stars)

name: aplusPop2, type: DOUBLE, column: 466
A parameter for pop 2 (all non compact stars)

name: aplusPopMix, type: DOUBLE, column: 467
A parameter for mixed pop (all non compact stars)

name: t0merge, type: DOUBLE, column: 468
number of binaries merged at the time T=0 (after justreading the data)

name: nescspop1, type: INTEGER, column: 469
total number of escaped singles for pop 1

name: nescspop2, type: INTEGER, column: 470
total number of escaped singles for pop 2

name: nescspopMix, type: INTEGER, column: 471
total number of escaped singles for pop Mix

name: bhsinfluSin, type: INTEGER, column: 472
number of single stars in BH subsystem influence radius

name: bhsinfluBin, type: INTEGER, column: 473
number of binaries in BH subsystem influence radius

name: bhsinfluSinNS, type: INTEGER, column: 474
number of single NSs in BH subsystem influence radius

name: bhsinfluBinNS, type: INTEGER, column: 475
number of binaries with NSs in BH subsystem influence radius

name: bhsinfluSinBH, type: INTEGER, column: 476
number of single BHs in BH subsystem influence radius

name: bhsinfluBinBH, type: INTEGER, column: 477
number of binaries with BHs in BH subsystem influence radius

name: bhsinfluSinWD, type: INTEGER, column: 478
number of single WDs in BH subsystem influence radius

name: bhsinfluBinWD, type: INTEGER, column: 479
number of binaries with WDs in BH subsystem influence radius

name: bhsinfluSinMSout, type: INTEGER, column: 480
number of single out-ofMS in BH subsystem influence radius

name: bhsinfluBinMSout, type: INTEGER, column: 481
number of binaries with out-ofMS in BH subsystem influenceradius

name: bhsinfluSinMS, type: INTEGER, column: 482
number of single MSs in BH subsystem influence radius

name: bhsinfluBinMS, type: INTEGER, column: 483
number of binaries with MSs in BH subsystem influence radius

name: bhsinfluSinm, type: DOUBLE, column: 484
mass of single stars in BH subsystem influence radius

name: bhsinfluBinm, type: DOUBLE, column: 485
mass of binaries in BH subsystem influence radius

name: bhsinfluSinNSm, type: DOUBLE, column: 486
mass of single NSs in BH subsystem influence radius

name: bhsinfluBinNSm, type: DOUBLE, column: 487
mass of binaries with NSs in BH subsystem influence radius

name: bhsinfluSinBHm, type: DOUBLE, column: 488
mass of single BHs in BH subsystem influence radius

name: bhsinfluBinBHm, type: DOUBLE, column: 489
mass of binaries with BHs in BH subsystem influence radius

name: bhsinfluSinWDm, type: DOUBLE, column: 490
mass of single WDs in BH subsystem influence radius

name: bhsinfluBinWDm, type: DOUBLE, column: 491
mass of binaries with WDs in BH subsystem influence radius

name: bhsinfluSinMSoutm, type: DOUBLE, column: 492
mass of single out-ofMS in BH subsystem influence radius

name: bhsinfluBinMSoutm, type: DOUBLE, column: 493
mass of binaries with out-ofMS in BH subsystem influenceradius

name: bhsinfluSinMSm, type: DOUBLE, column: 494
mass of single MSs in BH subsystem influence radius

name: bhsinfluBinMSm, type: DOUBLE, column: 495
mass of binaries with MSs in BH subsystem influence radius

name: pop1oc, type: INTEGER, column: 496
number of bound objects from population 1

name: pop2oc, type: INTEGER, column: 497
number of bound objects from population 2

name: popMixoc, type: INTEGER, column: 498
number of bound objects from mixed population

name: nEscSinRel, type: INTEGER, column: 499
total number of single star escapers because ofrelaxation

name: rns10, type: DOUBLE, column: 500
10% lagrangian radius for single NSs

name: rns50, type: DOUBLE, column: 501
50% lagrangian radius for single NSs

name: rns70, type: DOUBLE, column: 502
70% lagrangian radius for single NSs

name: rns210, type: DOUBLE, column: 505
10% lagrangina radius for NS in binaries and single

name: rns250, type: DOUBLE, column: 506
50% lagrangina radius for NS in binaries and single

name: rns270, type: DOUBLE, column: 507
70% lagrangina radius for NS in binaries and single

name: bhSubInflu, type: DOUBLE, column: 510
influence radius for BH subsystem

name: sturnm, type: DOUBLE, column: 511
sturn mass computed by standalone_turnoff function

name: ilostdis4, type: INTEGER, column: 512
number of binaries manually disrupted usingEbind

name: rwd10, type: DOUBLE, column: 513
10% lagrangian radius for single WDs

name: rwd50, type: DOUBLE, column: 514
50% lagrangian radius for single WDs

name: rwd70, type: DOUBLE, column: 515
70% lagrangian radius for single WDs

name: rwd210, type: DOUBLE, column: 518
10% lagrangina radius for WD in binaries and single

name: rwd250, type: DOUBLE, column: 519
50% lagrangina radius for WD in binaries and single

name: rwd270, type: DOUBLE, column: 520
70% lagrangina radius for WD in binaries and single

name: esrb3s, type: DOUBLE, column: 523
energy of star escapers - relaxation

name: slrb3s, type: DOUBLE, column: 524
mass loss of single stars due to relaxation

name: ererb3, type: DOUBLE, column: 525
energy of binary escapers - relaxation

name: errb3n, type: DOUBLE, column: 526
internal binding energy of binary escapers - relaxation (MC units)

name: slrb3b, type: DOUBLE, column: 527
mass loss of binaries due to relaxation

name: nescrs, type: INTEGER, column: 528
total number of star escapers due to relaxation

name: nesrb3, type: INTEGER, column: 529
total number of star escapers due to relaxation

name: igtrt, type: INTEGER, column: 530
total number of cases in which positions of relaxed starsare greater than the tidal radius - relaxation is not done

name: iplus1, type: INTEGER, column: 531
total number of cases in which i+1 is greater than lmaxin the relaxation loop - relaxation is not done

name: ikrel, type: INTEGER, column: 532
total number of cases in which the deflection angle isgreater than PI - relaxation is not done

name: vcl, type: DOUBLE, column: 533
central velocity dispersion in km/s (luminosity weighted)

name: u5, type: DOUBLE, column: 534
central potential for the 5th object (scalled to (km/s)^2)

name: u25, type: DOUBLE, column: 535
central potential for the 25th object (scalled to (km/s)^2)

name: u50, type: DOUBLE, column: 536
central potential for the 50th object (scalled to (km/s)^2)

name: u75, type: DOUBLE, column: 537
central potential for the 75th object (scalled to (km/s)^2)

name: u100, type: DOUBLE, column: 538
central potential for the 100th object (scalled to (km/s)^2)

[BEANS] Very short introduction to the web interface

Arkadiusz Hypki — Mon, 15 Oct 2018 11:37:12 GMT

This short tutorial describes:

the web interface to BEANS software
how to create a dataset
upload a file into BEANS to the newly created dataset (as a new table)
make a simple plot based on the table

Our own BEANS server is located at beans.camk.edu.pl. If you have there an account, please go there and log in.

The main page of BEANS looks like this:

The main menu on the top contains (from the left):

"Search" button - it is used to quick search of notebooks, datasets and tables
"Data" button - it is used, among others, to create new notebooks and datasets
"Account" button - it gives access to some user specific options and to manage groups of users
on the right there is button which shows statuses of jobs

In order to create a dataset choose in menu "Data" -> "New dataset".

Under the tab "Import files" one can upload one or many files into BEANS to this specific dataset. Just drag a file on the panel or click to it to add the file.

For testing create a simple text file on your hard drive:

Please notice, that the first line contains the header with the names of the columns. Once the file is imported there will be possible to use column names (x, y) in scripts and plots.

Save the file and upload it to the dataset. Once you are done you should see a new table on the bottom.

Now, we are ready to create a notebook and a plot. Choose in menu "Data" -> "New notebook". This will create the empty notebook.

Every notebook is a scrollable list of entries of different types. Menu for notebook is on the top - it will scroll down with the view so it will be always at hand.

For this tutorial we will create only one entry - a plot entry. Choose in notebook's menu "Insert". This will open a dialog for you with the list of possible entries to add.

Let's choose "Plot" entry and then "Save" button. This will add the "plot" entry to the notebook. Let's click to this entry with the mouse button and the menu for this entry will appear.

The most left button on entry's menu allow to edit the entry. The entry (of the plot) in edit mode looks like this:

There are a few fields which (even in this simple tutorial) needs en explanation:

In the line "Read data from Datasets" there are two input boxes. In the first one you need to specify a query for datasets and in the second for the tables. In our case "New Dataset" will find one dataset - the one which was created earlier. And the query "line" in the second search box will find our file which we uploaded and created the table "line-1-10.plain".

Be careful: if you will put there too general search queries you might end up plotting the whole MOCCA database into one plot (over 100 TBs)!

later, in the input box the term "x:y" means that the plot should make a line of two columns: x vs. y. Because in our test file we had in the first row the names of the columns we can now use them to make this plot.

After clicking to "play" button (the most left one) and waiting a bit the entry should look like this:

End.

[BEANS] Log in to BEANS

Arkadiusz Hypki — Mon, 15 Oct 2018 09:23:21 GMT

BEANS is a web-based software for interactive distributed data analysis with a clear interface for querying, filtering, aggregating, and plotting data from an arbitrary number of datasets and tables (beanscode.net).

We use BEANS to analyze data from over 2000 MOCCA simulations. Our BEANS server is running on:

https://beans.camk.edu.pl

In order to log in to our BEANS server you need:

1) to ask us for an account (the access to beans.camk.edu.pl is not public)

You may contact Mirek Giersz https://www.camk.edu.pl/en/people/staff/mig/

2) once you have an account created for you, just go to https://beans.camk.edu.pl and type you username (email) and password which you receive by email

Enjoy!

Publication: A New Scenario for the Formation of an Intermediate Mass Black Hole in Globular Clusters

Arkadiusz Hypki — Fri, 06 Nov 2015 17:04:16 GMT

In a recently published paper entitled, MOCCA code for star cluster simulations - IV. A new scenario for intermediate mass black hole formation in globular clusters, Mirek Giersz from NCAC and his collaborators discuss a new scenario for the formation of an intermediate-mass black holes (IMBHs) in globular clusters (GCs). The existence of IMBHs is an active topic of research that has been the subject of considerable debate. The discovery of this elusive population of black holes (BHs) will not only account for the missing link between stellar mass and supermassive BHs but will also be a major advancement in our understanding of the formation of massive BHs and their relation to galaxy formation. GCs are dense stellar systems that can contain up to a million stars. It has been suggested that these dense clusters of stars may harbour an IMBH.

While analysing results from over 400 simulations of different star cluster models that were simulated using the MOCCA code (MOnte Carlo Cluster simulAtor) for star cluster evolution (one of the most advanced codes for stellar dynamics developed from scratch at Nicolaus Copernicus Center (NCAC), Giersz and his collaborators discovered that an IMBH was forming in some of these models. A more detailed analysis of these models showed that the IMBHs formed via dynamical interactions of hard binaries containing a stellar-mass BH with other stars and binaries. The published results discuss the necessary conditions to initiate the process of IMBH formation and the influence of an IMBH on the host global GC properties. This new scenario for IMBH formation does not require any special specific conditions and IMBHs form solely through dynamical interactions and mass transfer in binaries, with the latter playing an especially important role by inducing collisions. There are two different regimes which result in the build-up of BH mass in this new scenario. In the first regime, the BH mass builds up slowly during the late cluster evolution and has a small mass accretion rate (SLOW scenario). In the second regime, the build-up of the BH mass starts very early during the cluster evolution and has an extremely high mass build-up rate (FAST scenario). Results show that the formation of an IMBH is a highly stochastic process, generally, the formation probability of an IMBH is higher when the cluster is more concentrated (has higher central densities).

The authors also use their simulation results to discuss the observational signatures associated with the presence of an IMBH in GCs. These include the spatial and kinematic structure of the host cluster, possible radio, X-ray and gravitational wave emissions due to dynamical collisions or mass transfer and the creation of hyper-velocity main-sequence escapers during strong dynamical interactions between binaries and an IMBH. The authors also provide examples of Galactic GCs that have similar properties to the present-day properties of simulated models that feature the formation of an IMBH.

Authors: Mirek Giersz (NCAC), Nathan Leigh (University of Alberta and American Museum of Natural History), Arkadiusz Hypki (NCAC and Leiden University), Nora Lützgendorf (ESA, Space Science Department) and Abbas Askar (NCAC).

Picture: Artist's View of a Black Hole in a Globular Cluster - Credit: NASA/ESA and G. Bacon (STScI)

Publication: The state of globular clusters at birth - II. Primordial binaries

Arkadiusz Hypki — Mon, 05 Jan 2015 07:18:00 GMT

In Jan 2015 the second paper from the series of papers about the state of globular clusters at birth was published in the Montly Notices of the Royal Astronomical Society (Leigh et al. 2015).

In this paper, we constrain the properties of primordial binary populations in Galactic globular clusters.

Using the MOCCA Monte Carlo code for cluster evolution, our simulations cover three decades in present-day total cluster mass. Our results are compared to the observations of Milone et al. using the photometric binary populations as proxies for the true underlying distributions, in order to test the hypothesis that the data are consistent with a universal initial binary fraction near unity and the binary orbital parameter distributions of Kroupa.

With the exception of a few possible outliers, we find that the data are to first-order consistent with the universality hypothesis. Specifically, the present-day binary fractions inside the half-mass radius can be reproduced assuming either high initial binary fractions near unity with a dominant soft binary component as in the Kroupa distribution combined with high initial densities (10^4-10^6 M⊙ pc^-3), or low initial binary fractions (~5-10 per cent) with a dominant hard binary component combined with moderate initial densities near their present-day values (10^2-10^3 M⊙ pc^-3). This apparent degeneracy can potentially be broken using the binary fractions outside the half-mass radius - only high initial binary fractions with a significant soft component combined with high initial densities can reproduce the observed anticorrelation between the binary fractions outside the half-mass radius and the total cluster mass.

We further illustrate using the simulated present-day binary orbital parameter distributions and the technique first introduced in Leigh et al. that the relative fractions of hard and soft binaries can be used to further constrain both the initial cluster density and the initial mass-density relation. Our results favour an initial mass-density relation of the form rh ∝ Mclus^{α} with α < 1/3, corresponding to an initial correlation between cluster mass and density.

References

see paper on ADS

Publication: The state of globular clusters at birth: emergence from the gas-embedded phase

Arkadiusz Hypki — Tue, 14 Jan 2014 22:25:00 GMT

Globular clusters are one of the simplest dynamical systems. This does not mean, however, that the knowledge of their evolution and interactions between the various physical processes operating in their life is a simple matter. Globular clusters associated with the Milky Way are among the oldest objects in the Galaxy. Their ages are comparable to the age of the Universe. They are characterized by a number of interesting observational features. Some of the most interesting are: the correlation between the number of binaries, and the mass of the cluster - the larger the number of binaries, the lower mass of the globular cluster and the correlation between the slope of the present day mass function (PMF) and the cluster concentration parameter - the higher the concentration the higher the slope of the PMF.Thanks to a numerical code MOCCA, developed at NCAC, the study of the evolution of real-size globular clusters has become a feasible task, to be completed on time of the order of days! MOCCA code is now one of the best numerical codes used to study the evolution of large stellar systems, under the influence of various physical processes. It provides detailed information on the evolution of the cluster and the evolution of stars and binaries, which live in the cluster.

Within the framework of international cooperation of Mirek Giersz and Arkadiusz Hypki from NCAC with Nathan Leigh from ESA and his collaborators there an attempt was made to explain the observed correlation between the mass of the cluster and the number of binaries and the concentration parameter and the slope of PFM. These correlations can either be reproduced from universal initial conditions combined with some dynamical mechanisms that transform the cluster structure and PFM over time, or it must arise during the gas-embedded phase of cluster formation. There were performed more than 130 MOCCA dynamicalsimulations of star clusters characterized by different initial: masses, sizes, concentrations and MF... For the range of initial conditions considered here, our results are consistent with an universal initial binary fraction about 10% and an universal initial MF resembling the standard Kroupa distribution. However, we require some dependence of the initial concentration on the total cluster mass, such that the concentration increases with increasing cluster mass. Thus, we conclude that the dynamical processes considered here could not alone have reproduced the observed distribution of concentrations. The origin of this trend is likely connected to the gas-embedded phase of cluster evolution. Specifically, we argue that cluster expansion due to rapid gas expulsion could account for the least concentrated clusters with the flattest MF, and that cluster contraction due to prolonged gas retention could help to create the most concentrated clusters with the steepest MF.

More info in the paper:The state of globular clusters at birth: emergence from the gas-embedded phase, Nathan Leigh, Mirek Giersz, Jeremy Webb, Arkadiusz Hypki, Guido De Marchi, Pavel Kroupa, Alison Sills.

MOCCA team at the MODEST-13 meeting

Arkadiusz Hypki — Fri, 06 Sep 2013 21:27:00 GMT

On August 19-23, 2013 there was a MODEST-13 meeting in the beautiful city of Almaty in Kazakhstan. The conference was organized by Fesenkov Astrophysical Institute .

MODEST is a continuous series of meetings which take place in different cites around the world. It's main purpose is to bring together scientists working in the fields of stellar dynamics, stellar evolution, stellar hydrodynamics, evolution and observations of star cluster, galaxy and related objects. MODEST-13 meeting in Almaty gathered world class astrophysicists working on interesting and ambitious projects of the mentioned areas of research.

Mirek Giersz gave a talk about a new channel of formation of Intermediate Mass Black Holes (IMBHs) in dense star clusters. He showed that NSs and BHs can be formed during the evolution of star clusters due to dynamical interactions. He spotted also two distinct scenarios for IMBHs formation: fast and slow. In the fast scenario IMBHs buildup starts in the beginning of the star cluster evolution and the masses of IMBHs are in general higher than from slow scenario. The slow scenario starts typically after several Gyrs of star cluster evolution and less dynamical interactions ends with merger event. For slow scenario there is also clearly visible binary evolution pattern - semi-major axes with BHs shrink due to dynamical interactions and then mass transfer begins.

Rainer Spurzem gave a lecture about using GPU hardware for astrophysical simulations. He presented overview of such hardware and a big role of China in the development of GPU computing clusters. Additionally, Rainer discussed the prospects of GPU supercomputing for the upcoming Exaflop/s problems.

Arkadiusz Hypki gave a talk about bimodal spatial distribution of blue straggler stars. Bimodal spatial distribution is a feature observed in many star clusters which shows that the highest number of blue straggler stars are present in the center of the cluster. Then, there is clear clear-cut dip in the intermediate region and again rise of BSS in the outer region of the cluster (but lower than the central value). However, for some star clusters there are unimodal distributions of such objects - there is no second peak. And some other clusters show completely flat spatial distribution of blue stragglers. In the presentation he showed and discussed what could be origin of such features.

The MOCCA team is grateful to the hosts for organizing such a great conference.

Publication: MOCCA code for star cluster simulations - II. Comparison with N-body simulations

Arkadiusz Hypki — Mon, 02 Sep 2013 16:55:00 GMT

In May 2013 the second paper from the series of papers about the MOCCA code was published in the Montly Notices of the Royal Astronomical Society (Giersz et al. 2013).

We describe a major upgrade of the Monte Carlo code that has previously been used for many studies of dense star clusters. We outline the steps needed in order to calibrate the results of the new Monte Carlo code against N-body simulations for large-N systems, up to N = 200 000. The new version of the Monte Carlo code (called MOCCA), in addition to features of the old version, incorporates the direct Fewbody integrator for three- and four-body interactions, and a new treatment of the escape process based on work of Fukushige & Heggie. Now stars that fulfill the escape criterion are not removed immediately, but can stay in the system for a certain time that depends on the excess of the energy of the star above the escape energy. These stars are termed potential escapers.

With the addition of the Fewbody integrator the code can follow all interaction channels that are important for the rate of creation of various types of objects observed in star clusters, and it is ensured that the energy generation by binaries is treated in a manner similar to in the N-body model.

There are at most three new parameters that have to be adjusted against N-body simulations for large N: two (or one, depending on the chosen approach) connected with the escape process, and one responsible for the determination of the interaction probabilities. The values adopted for the free parameters have at most a weak dependence on N. They allow MOCCA to reproduce N-body results with reasonable precision, not only for the rate of cluster evolution and the cluster mass distribution, but also for the detailed distributions of mass and binding energy of binaries. In addition, the code can follow the rate of formation of blue stragglers and black hole-black hole binaries. The code computes interactions between binaries and single stars up to a maximum separation r _pmax , and it is found that MOCCA needs a large value of r _pmax to obtain agreement with N-body simulations.

In spite of some limitations, such as its spherical symmetry, a Monte Carlo code such as MOCCA is at present the most advanced code for simulations of real star clusters. It can follow the cluster evolution at a level of detail comparable to that in an N-body code, but orders of magnitude faster.

References

see paper on ADS

Publication: MOCCA code for star cluster simulations - I. Blue stragglers, first results

Arkadiusz Hypki — Sun, 01 Sep 2013 16:45:00 GMT

In February 2013 the first paper from the series of papers about the MOCCA code was published in the Montly Notices of the Royal Astronomical Society (Hypki et al. 2013).

The paper presents first results concerning blue straggler stars which were obtained with the new and improved version of the Monte Carlo code, called MOCCA. It combines the Monte Carlo method for star cluster evolution and the FEWBODY code to perform scattering experiments. The FEWBODY code was added in order to track more precisely dynamical interactions between objects which can lead to the creation of various exotic objects observed in star clusters (in example blue stragglers). The MOCCA code is currently one of the most advanced codes for simulating real size star clusters. It follows the star cluster evolution closely to N-body codes but is much faster. We show that the MOCCA code is able to follow the evolution of blue stragglers stars (BSs) with details. It is a suitable tool to perform full scale evolution of real star clusters and detailed comparison with observations of exotic star cluster objects like BSs.

This paper is the first one of a series of papers about properties of BSs in star clusters. This type of stars are particularly interesting today, because by studying them one can get important constraints on the link between the stellar and dynamical evolution of star clusters. We discuss here first results concerning BSs for an arbitrary chosen test model. We investigate properties of BSs which characterize different channels of formation like masses, semi-major axes, eccentricities and orbital periods. We show how BSs from different channels change their types, and discuss the initial and final positions of BSs, their bimodal distribution in the star cluster, lifetimes and more.

A few selected conclusions from the paper are presented here.

Mass ratios for long period Evolutionary Mass Transfer BSS (EMT) fit to the equation q=M{turn-off}/M{WD}. In the nominator there are masses of long period EMT, which are just slightly larger than M{turn-off} (typically 0.1*M{turn-off} after 500\302\240Myrs). WDs are companions in the long period EMT. Thus, in the denominator there are masses of WDs calculated based on Chernoff (1990, Tab. 1). It shows that mass ratios of long period EMT have a narrow range and predictable values through the entire simulation.

For many BSs there is a significant delay before the actual detection. The last merger or the last mass transfer can happen even several Gyrs before BSs actually exceeds the turn-off point. This effect was not expected in common scenarios for creation BSs. It was rather assumed, that mergers between stars create BSs immediately. Dormant BSs seem to be important, because there were created overall 112 dormant BSS from the total 476 BSs which gives 24%.

References

link to paper on ADS