# 10. Potentials and Accellerations (*)¶

Here we lists a number of potentials, taken from
from CTEX comments in the
**$NEMO/src/orbit/potential/data** source code
directory.
Most NEMO programs that deal with potentials have three
program keywords associated with
potentials:

**potname=**describes the name**potpars=**optional parameters**potfile=**optional associated filenames (or other textual information)

Each section below details a potential
and explains the usage of the **potpars=** and **potfile=**
keywords.
The section title is the actual **potname=** to be used for
this potential.
Mostly **G=1**, unless otherwise mentioned.

Todo

describe the newer **accelerations** from *falcON*

Todo

potentials auto-build from source code ???

## 10.1. Example Potentials¶

In the latex manual this chapter is derived from the code. We thus need a new `crst`

script
that produces this. Needs to handled embedded math, such as \(\frac{ \sum_{t=0}^{N}f(t,k) }{N}\)

### 10.1.1. bar83¶

% File: bar83.c

potname=bar83 potpars={it $Omega,f_m,f_x,{cover a}$}}

Barred potential as described by Teuben and Sanders (1983), see also {bf teusan83}.

Note: the potential only valid in the z=0 plane!

### 10.1.2. bulge1¶

% File: bulge1.c

{bf potname=bulge1 potpars={it $Omega,M,R,c/a$}}

homogeneous oblate bulge with mass $M$, radius $R$, and axis ratio $c/a$

### 10.1.3. ccd¶

% File: ccd.c

{bf potname=ccd potpars={it $Omega,Iscale,Xcen,Ycen,Dx,Dy$} potfile={it image(5NEMO)}}

This potential is defined using a simple cartesian grid on which the potential values are stored. Using bilinear interpolation the values and derivatives are computed at any point inside the grid. Outside the grid (as defined by the WCS in the header) the potential is not defined and assumed 0. The lower left pixel of an image in NEMO is defined as (0,0), with WCS values Xmin,Ymin derived from the header. If the (Xcen,Ycen) parameters are used, these are the 0-based pixel coordinates of the center pixel. If (Dx,Dy) are used, these are the pixel separations. To aid astronomical images where $Dx < 0$, these are interpreted as positive. Also note that potentials are generally negative, so it is not uncommon to need $Iscale = -1$. Programs such as {it potccd} can create such a {bf ccd} grid potential from a regular potential.

Note: Since these forces are defined only in the Z=0 plane, the Z-forces are always returned as 0.

### 10.1.4. cp80¶

% File: cp80.c

{bf potname=cp80 potpars={it $Omega,epsilon$}}

Contopoulos & Papayannopoulos (1980, A&A, 92,33)
used this potential
in the study of orbits in barred galaxies. Note that their
*bar* is oriented along the Y-axis, an axis ratio is not
well defined, and for larger values of $epsilon$ the density
can be negative. The potential used is given by adding an
axisymmetric component to a m=2 fourier component:

where \(\Phi_1\) is the Isochrone potential with unit scalelength and mass, and \(\Phi_2\) the Barbanis & Woltjer (1965) potential:

and

A value of \(\epsilon=0.00001\) is the default for a moderate bar, whereas 0.001 is a strong bar!

### 10.1.5. dehnen¶

% File: dehnen.c

{bf potname=dehnen potpars={it $Omega,M,a,gamma$}}

Walter Dehnen (1993, MN {bf 265}, 250-256) introduced a family of potential-density pairs for spherical systems:

The potential is given by:

cumulative mass by

and density by

with $0 <= gamma < 3$. Special cases are the Hernquist potential ($gamma=1$), and the Jaffe model ($gamma=2$). The model with $gamma=3/2$ seems to give the best comparison withe de Vaucouleurs $R^{1/4}$ law.

See also Tremaine et al. (1994, AJ, 107, 634) in which they describe the same density models with $eta=3-gamma$ and call them $eta$-models.

### 10.1.6. dublinz¶

% File: dublinz.c

{bf potname=dublinz potpars={it $Omega,r_0,r_1,v_1,dvdr,s,h$}}

Forces defined by a double linear rotation curve defined by ($r_1,v_1$) and a gradient $dvdr$ between $r_0$ and $r_1$. As in {bf flatz} (from which this one is derived), the potential is quasi harmonic in $Z$ (linear forces), with radial scalelength $h$ and scale height $s$

### 10.1.7. expdisk¶

% File: expdisk.c

{bf potname=expdisk potpars={it $Omega,M,a$}}

Exponential disk (BT, pp.77)

### 10.1.8. flatz¶

% File: flatz.c

potname=flatz potpars=:math:Omega,r_0,v_0,s,h

forces defined by a rotation curve that is linear to $(r_0,v_0)$ and flat thereafter and quasi harmonic in $Z$, with radial scalelength $h$ and scale height $s$. See also {bf dublinz} for a variation on this theme.

### 10.1.9. halo¶

% File: halo.c

{bf potname=halo potpars={it $Omega,v_0,r_c$}}

### 10.1.10. hh64¶

% File: hh64.c

potname=hh64 potpars=:math:Omega,lambda

### 10.1.11. grow_plum¶

% File: grow_plum.c

### 10.1.12. grow_plum2¶

% File: grow_plum2.c

### 10.1.13. harmonic¶

% File: harmonic.c

{bf potname=harmonic potpars={it $Omega,omega_x^2,omega_z^2,omega_z^2$}}

Harmonic potential

### 10.1.14. hernquist¶

% File: hernquist.c

{bf potname=hernquist potpars={it $Omega,M,r_c$}}

The Hernquist potential (ApJ, 356, pp.359, 1990) is a special $gamma=1$ case of the Dehnen potential. The potential is given by:

and mass

and density

### 10.1.15. hom¶

% File: hom.c

{bf potname=hom potpars={it $Omega,M,R,tau$}}

### 10.1.16. hubble¶

% File: hubble.c

{bf potname=hubble potpars={it $Omega,M,R,b,c$}} where $M$ and $R$ are the core mass and radius. $b$ and $c$ are, if given, the intermediate and short axes can be different from the core radius.

The Hubble profile (BT, pp 39, req. 2-37 and 2-41) has a density law:

and an equally simple expression for the projected surface brightness:

The derivation of the potential is a bit more involved, since there is no direct inversion, and integration in parts is needed. The cumulative mass is given by:

and the potential

### 10.1.17. kuzmindisk¶

% File: kuzmindisk.c

{bf potname=kuzmin potpars={it $Omega,M,a$}}

Kuzmin (1956) found a closed expression for the potential of an infinitesimally thin disk with a Plummer potential in the plane of the disk (see also BT pp43, eq. 2-49a and 2-49b):

and corresponding surface brightness ({it check units})

With $GMa^2 = V_0^2$. This potential is also known as a Toomre n=1 disk, since it was re-derived by Toomre (1963) as part of a series of disks with index $n$, where this disk has $n=1$.

### 10.1.18. isochrone¶

% File: isochrone.c

{bf potname=isochrone potpars={it $Omega,M,R$}}

### 10.1.19. jaffe¶

% File: jaffe.c

{bf potname=jaffe potpars={it $Omega,M,r_c$}}

The Jaffe potential (BT, pp.237, see also MNRAS 202, 995 (1983))), is another special $gamma=2$ case of the Dehnen potential.

### 10.1.20. log¶

% File: log.c

% CTEX Line: 8 {bf potname=log potpars={it $Omega,M_c,r_c,q$}}

The Logarithmic Potential (BT, pp.45, eq. 2.54 and eq. 3.77) has been often used in orbit calculations because of its flat rotation curve. The potential is given by

with $ M_c equiv {1over 2} r_c v_0^2 $ defined as the *core mass*.

### 10.1.21. mestel¶

% File: mestel.c

% CTEX Line: 10 {bf potname=mestel potpars={it $Omega,M,R$}}

### 10.1.22. miyamoto¶

% File: miyamoto.c

% CTEX Line: 20 {bf potname=miyamoto potpars={it $Omega,a,b,M$}}

### 10.1.23. nfw¶

% File: nfw.c % CTEX Line: 29

The NFW (Navarro,Frank & White) density is given by

and the potential by

### 10.1.24. null¶

% File: null.c

% CTEX Line: 5

This potential has no other meaning other than to fool the compiler. It has no associates potential, thus the usual potname, potpars,potfile will have no meaning. Use {bf potname=zero} if you want a real potential with zero values.

### 10.1.25. op73¶

% File: op73.c

% CTEX Line: 14 {bf potname=op73 potpars={it $Omega,M_H,r_c,r_h$}}

Ostriker-Peebles 1973 potential (1973, ApJ {bf 186}, 467). Their potential is given in the form of the radial force law in the disk plane:

### 10.1.26. plummer¶

% File: plummer.c

% CTEX Line: 8 {bf potname=plummer potpars={it $Omega,M,R$}}

Plummer potential (BT, pp.42, eq. 2.47, see also MNRAS 71, 460 (1911))

### 10.1.27. plummer2¶

% File: plummer2.c

### 10.1.28. rh84¶

% File: rh84.c

% CTEX Line: 20 {bf potname=rh84 potpars={it $Omega,B,a,A,r_0,i_0,j$}}

This 2D spiral and bar potential was used by Robert and collaborators in the 70s and 80s. For counterclockwise streaming, this spiral is a trailing spiral when the pitch angle ($i_0$) is positive. Within a radius $r_0$ the potential becomes barlike, with the bar along the X axis. At large radii the spiral is logarithmic. References:

Roberts & Haussman (1984: ApJ 277, 744)

Roberts, Huntley & v.Albada (1979: ApJ 233, 67)

### 10.1.29. rotcur0¶

% File: rotcur0.c

% CTEX Line: 9 {bf potname=rotcur0 potpars={it $Omega,r_0,v_0$}}

The forces returned are the axisymmetric forces as defined by a linear-flat rotation curve as defined by the turnover point $r_0,v_0$. The potential is not computed, instead the interpolated rotation curve is returned in as the potential value.

### 10.1.30. rotcur¶

% File: rotcur.c

% CTEX Line: 14 {bf potname=rotcur potpars={it $Omega$} potfile={it table(5NEMO)}}

The forces returned are the axisymmetric forces as defined by a rotation curve as defined by a table given from an ascii table. The potential is not computed, instead the interpolated rotation curve is returned in as the potential value.

This version can only compute one version; i.e. on re-entry of inipotential(), old versions are lost.

### 10.1.31. sh76¶

% File: sh76.c

- {bf potname=sh76
potpars={it $Omega,A,alpha,epsilon$}}

This bar potential was used by Sanders and Huntley (1976) and also used in Sanders (2019). The density perturbation is given by

and the potential

where

### 10.1.32. teusan85¶

% File: teusan85.c

% CTEX Line: 25 {bf potname=teusan85}

This potential is that of a barred galaxy model as described in Teuben & Sanders (1985) This bar is oriented along the X axis. This is the 2D version for forces. This version should give (near) identical results to {bf bar83} and very simlar to {bf athan92}.

### 10.1.33. triax¶

% File: triax.c

% CTEX Line: 11 {bf potname=triax}

A growing bi/triaxial potential

### 10.1.34. twofixed¶

% File: twofixed.c

% CTEX Line: 16 {bf potname=twofixed potpars={it $Omega,M_1,x_1,y_1,z_1,M_2,x_2,y_2,z_2$}}

This potential is defined by two fixed points, with different masses and positions. Orbits in this potential exhibit a number of interesting properties. One well known limit is the {tt stark problem}, where one of the two bodies is far from the other and near-circular orbits near the central particles are studied. Another is the limit or two particles near to other and orbits that circumscribe both particles.

### 10.1.35. plummer4¶

% File: plummer4.c

% CTEX Line: 10 potname=plummer potpars=:math:Omega,M,R

Plummer potential (BT, pp.42, eq. 2.47, see also MNRAS 71, 460 (1911))

### 10.1.36. vertdisk¶

% File: vertdisk.c

### 10.1.37. tidaldisk¶

% File: tidaldisk.c % CTEX Line: 8

Tidal field exerted by a (plane-parallel) stellar disk on a cluster passing through with constant vertical velocity. Useful for simulations of disk-shocking of, say, globular clusters

The following three density models are available

thin disk:

exponential disk:

sech$^2$ disk:

Parameters (to be given by potpars=…) are:

```
par[0] = not used (reserved for pattern speed in NEMO)
par[1] = h scale-height par[1] = 0 -> thin disk
par[1] > 0 -> vertically exponential disk
par[1] < 0 -> sech^2 disk with h=|par[1]|
par[2] = Sig disk surface density
par[3] = Vz constant vertical velocity of cluster center
par[4] = Z0 cluster center z-position at t=0
par[5] = add boolean: add tidal potential or not?
```

We always assume G=1.

If you want to include the acceleration of the disk on the cluster as a whole, rather than assume a constant velocity, use vertdisk.c

Some words on the mechanics

Assume that the plane-parallel disk potential and force are given by

Then, the tidal force exerted on a star at position z w.r.t. to cluster center, which in turn is at absolute height Zc = Z0 + t Vz, is simply

Integrating this from z=0 to z gives the associated tidal potential as

Whenever the tidal force & potential are desired at a new time t, we pre-compute $Zc$ and the plane-parallel potential and force at $Z=Zc$. Note that when both $Zc$ and $Zc+z$ are outside of the mass of the disk (and $Z=0$ is not between them), both tidal force and potential vanish identically. The standard treatment of tidal forces corresponds to approximating (2) by $F(Zc) + z * F’(Zc)$. This method, however, breaks down for disks that are thin compared to the cluster, while our method is always valid, even for a razor thin disk.

### 10.1.38. polynomial¶

% File: polynomial.c

% CTEX Line: 9 {bf potname=polynomial potpars={it $Omega,a0,a1,a2,a3,….$}}

Polynomial potential

where any unused coefficients will be set to 0. Up to 16 (defined as MAXPOW) can be used.

### 10.1.39. wada94¶

% File: wada94.c

% CTEX Line: 11 {bf potname=wada94 potpars={it $Omega,c,a,epsilon$}}

Wada (1994, PASJ 46, 165) and also Wada & Have (1992, MN 258, 82) used this potential in the study of gaseous orbits in barred galaxies.

where $Phi_1$ is the Toomre potential with scalelength $a$

and

A relationship for the axisymmetric component is

-sqrt(27/4)

### 10.1.40. zero¶

% File: zero.c

% CTEX Line: 6 {bf potname=zero}

Zero potential

## 10.2. Accellerations¶

This is a falcON addition. They are defined in `$FALCON/src/public/acc`

,
where their list (for installation) is defined in `$FALCON/makepub`

.

For a new potential, say `GasPotential.cc`

, add to `$FALCON/makepub`

:

```
acc_pub :=
...
$(ACC)GasPotential.so
```

and a proper dependency as well:

```
$(ACC)GasPotential.so: $(SACC)GasPotential.cc $(ACCT) $(defacc_h) $(makefiles)
$(MAKE_ACC)
```