Ram pressure stripping of galaxies: The long- and short-pulse limits
Joachim Köppen Kiel September 2017

### Some brief explanations

• This utility allows the user to estimate the consequences of ram pressure stripping on the gas disk of a galaxy:
Is the ram pressure pulse longer than the period for vertical oscillations in the galactic disk (typically 100 Myr), one may treat the problem by a quasi-static argument (Gunn & Gott, 1972): gas is removed from the disk, if the ram pressure exceeds the maximum of the vertical restoring force. This may also be called the long-pulse limit, and the result depends on the maximum ram pressure.
If, on the other hand, the pulse is much shorter, it depends the amount of momentum deposited in the gas element whether the gas can escape. This is called the short-pulse limit, and the outcome depends on the time-integrated ram pressure

How much gas is removed from a given galaxy as the result of a certain ram pressure history, is uniquely characterized on these two parameters if the ram pressure is a pulse with e.g. a Lorentzian time profile.
• The solution is best shown in the plane spanned by time-integrated ram pressure and maximum ram pressure pmax. This utility allows the user to explore this diagram.
• For a given galaxy and a specified deficiency (i.e. stripped mass fraction) the -pmax diagram marks the long-pulse limit with a black line, the short-pulse limit with a blue line, and the red curve as the interpolating curve between the two limits. The red dot marks the intersection of the two limits. The green line indicates the relation between and pmax for a Lorentzian pulse with the specified pulse duration.
• For the long-pulse limit the relations between the maximum ram pressure value and the parameters for the outcome: stripping radius, lost mass fraction, deficiency are shown.
• Likewise, for the short-pulse limit the dependence of the outcome parameters on the time-integrated ram pressure are displayed.

• The model for the galaxy consists of a stellar bulge, a disk of stars and gas, and a dark matter halo. Each component is specified by its parameters: total mass inside a truncation radius and a radial scale length, with a scale height for the disk's components. For comparison purposes, a point mass in the galactic centre may be added.
• The maximum restoring force in the criterion of Gunn & Gott is computed from the gravitational potential of the entire galaxy
• Likewise, this potential is used to compute circular and escape speeds for the short-pulse limit.
• The display is controlled by:
• X, Y: chose the abscissa and the ordinate among:
• maximum ram pressure
• time integrated ram pressure AKA (vΣ)ICM
• gas mass fraction: the fraction of the inital mass that remains.
• deficiency = log10(initial mass/remaining mass).
• stripping radius = the outer radius of the remaining gas disk.
• wipe&plot: clear the plot area and draws the last curve in red. Changing any parameter value (and hitting the Enter key) will overplot the new curve in red.
• overplot: after changing any parameter value, these button will overplot the new curve in the corresponding colour.

Central point mass
Mass [MSUN]
Bulge ( = Plummer sphere)
Mass [MSUN]
Stellar disk ( = Miyamoto-Nagai)
Mass [MSUN]
Thickness [kpc]
Gas disk ( = Miyamoto-Nagai)
Mass [MSUN]
Thickness [kpc]
Dark matter halo ( = Plummer sphere)
Mass [MSUN]