Table of Contents

There is also an implementation in Dehnen’s falcON suite: *mkplum(1falcON)*

For more advanced Plummer models, see *mcluster(1NEMO)*
.

**out=***snapfile*- Output data is written into
*snapfile*, in standard*snapshot(5NEMO)*format.

No default **nbody=***integer*- Number of particles in the model.

No default. **mlow=***real*- inner core mass fraction within which no stars will
be populated.

[Default: 0] **mfrac=***real*- mass fraction of the (otherwise infinitely extended)
Plummer model; see rfrac immediately below Note that the total mass is
still normalized to 1.

[Default:*rfrac*=22.8042468] **rfrac=***real*- radius fraction of the (otherwise
infinitely extended) Plummer model. If
*mfrac = 1.0*then particles will be sprinkled in all over space. If*mfrac*< 1.0 or*rfrac*> 0.0 then each particle is constrained to lie within both the radial and (cumulative) mass bound. For example, if*rfrac*(*mfrac*) >*rfrac*then*rfrac*is the limiting factor, but if*rfrac*(*mfrac*) <*rfrac*then*mfrac*limits the extent of the Plummer realization. Note: specifying either value may have no effect if the default value of the other parameter is still the limiting factor; Beware! (Default:*mfrac*=0.999;*rfrac*=22.8042468 , chosen so that the cumulative mass at*rfrac*is*mfrac*).

Default: .... **seed=***integer*- seed for the random number generator. A value of
0 (the default) will be converted into a unique new value using UNIX’s clock
time, in seconds since 1970.0). See also
*xrandom(1NEMO)*for more options.

[Default: 0] **time=***time*- Time at which the snapshot applies

[Default: 0.0] **zerocm=t|f**- Reset center of mass to zero?

[Default:**t**]. **scale=***scale_factor*- A scale factor or scale to virial units
(M=G=-4E=1). Use -1 for virial units (see also UNITS below), and 1 to get
a model in structural (natural) units. Note: large scale factors means small
systems with large velocity disperson.

[Default:**-1**]. **quiet=***level*- Level of quit start. 0 is noisy, 1=somewhat quiet,
2=more quiet. See "QUIET START" below

[Default:**0**]. **massname=***name*- Identification of the mass spectrum. It is normally
only a function of mass, so
**n(m)**will suffice. If nothing specified, all stars will have the same mass (total mass M=1).

[Default: not used]. **massexpr=***expr*- Expression for the mass-spectrum. In addition
to the mass
*m*from the**massname**it may contain any variables contained in the**masspars**to be specified next.

[Default:**pow(m,p)**]. **masspars=***pars*- List of parameters and their values. They
can be used by name in the
**massexpr**specified before.

[Default:**p,0.0**]. **massrange=***mlow,mhigh*- Valid massrange. A lower and higher
cutoff must be supplied. The massrange has arbitrary units, since all masses
will be rescaled to set the total mass M=1.

[Default:**1,1**]. **headline=***string*- Optional headline, which is written as the
first item in the snapshot file, the next item being the snapshot itself.

[Default: not used]. **nmodel=***integer*- Number of models to generate. Although
mostly meant for benchmarks, generating more then 1 model can be useful
to process very large snapshots (that normally won’t fit in memory) in a
serialized fashion. See also
*snapsplit*. Most NEMO programs will only read the first snapshot.

[Default:**1**] **mode=0|1|2**- The processing mode, purely for debugging benchmarks.
0=no data written. 1=data written, but no extra analysis. 2=data written,
and extra analysis done.

[Default: 1]

mkplummer - 10000 | radprof - tab=t | tabplot
- 1 3 0 2 0 1 yapp=1/xs

rotcurves plummer ’0,1,3*pi/16’ xrange=0,2 yrange=0,1 yapp=2/xs

In this example you can clearly see the difference between the radii selected:

mkplummer - 10 quiet=0
zerocm=f | snapsort - - r | snapprint - r | tabplot - 0 1 line=1,1 point=2,0.1

mkplummer - 10 quiet=1 zerocm=f | snapsort - - r | snapprint - r | tabplot -
0 1 line=1,1 point=2,0.1

mkplummer - 10 quiet=2 zerocm=f | snapsort - - r | snapprint - r | tabplot -
0 1 line=1,1 point=2,0.1

Important to note that with **zerocm=f** the center of mass will drift,
while the "mathematical center" was placed at the origin. This will counter
the quietness, if you will.

For very
large (>1000) ratio in the mass ranges the spline interpolation, used in
*frandom(3NEMO)*
, can fail using a valid [0,1] range.

mkplummer salpeter.dat 10000 massname=’n(m)’ massexpr=’pow(m,p)’
masspars=p,-2.35 massrange=0.1,10

Another method to create a Plummer sphere is by using the Osipkov-Merritt tables in NEMO, e.g.

plummer plum.dat ntab=1024

mkommod plum.dat plum.snap nbody=10000

or in ZENO their new General Spherical Profile:

plumsnap plum1.snap

plumgsp plum.gsp

gsprealize plum.gsp plum.snap zerocm=true

snapcopy plum.snap plum2.snap

with a note that ZENO files may need an extra *snapcopy(1NEMO)*
to be
compatible with NEMO *snapshot(5NEMO)*
files.

cd $NEMO/nemo/src/nbody/init/

make -f Benchfile bench0 bench1

or

/usr/bin/time mkplummer . 10000000

/usr/bin/time mkplummer bench1.snap 10000000

with some sample CPU for bench0: xps13 3.1s or 171 MB/s

t480 4.9s or 72 MB/s

the time difference betweeen bench0 and bench1 can be interpreted as
the time needed to write 535MB (for 10M particles)

H.C.Plummer
(1911), *MNRAS*, **71**, 460.

S.J. Aarseth, M. Henon and R. Wielen (1974), *Astron.
and Astrophys. 37*, p. 183.

A.H.W. Kuepper, Th. Maschberger, P. Kroupa and H. Baumgardt, 2011, MNRAS, 417, 2300 (McLuster)

Arnold et al. (2022) - https://arxiv.org/abs/2207.10681 - https://github.com/r-j-arnold/gen_fractal_star_clusters

~/src/nbody/initmkplummer.c

23-Apr-87Version 1.0: createdPIET 10-Jun-88Version 1.1: createdPIET xx-xxx-88V1.2: zerocm keyword addedPJT xx-Mar-89V2.0: full new snapshot version+docPJT 15-nov-90V2.3: mass-spectrum and cleanup for NEMO 2.xPJT 6-jun-96V2.5d: report total mass before scalingPJT 21-mar-04V2.7: added mlow=PJT+NCM 11-apr-05V2.8: added nmodel=PJT 15-sep-10V2.9: clarified rfrac and allow rfrac<0PJT 2-dec-2017documented mclusterPJT 29-mar-2021benchmarkPJT 25-sep-2023describe quiet startsPJT 1-apr-2024experimenting with how to place defaultsPJT