vice.singlezone.schmidt¶
Type : bool
Default : False
If True, the simulation will adopt a gas-dependent scaling of the star formation efficiency timescale \(\tau_\star\). At each timestep, \(\tau_\star\) is determined via:
where \(\tau_{\star,\text{specified}}(t)\) is the user-specified
value of the attribute tau_star
, \(M_g\) is the mass of the
interstellar medium, \(M_{g,\text{Schmidt}}\) is the normalization
thereof (attribute MgSchmidt
), and \(\alpha\) is the power-law
index set by the attribute schmidt_index
.
This is an application of the Kennicutt-Schmidt star formation law to the single-zone approximation (Kennicutt 1998 [1]; Schmidt 1959 [2], 1963 [3]).
If False, this parameter does not impact the star formation efficiency that the user has specified.
Note
This attribute is irrelevant when the attribute tau_star
is a function of two variables.
See also
vice.singlezone.tau_star
vice.singlezone.schmidt_index
vice.singlezone.MgSchmidt
Example Code¶
>>> import vice
>>> sz = vice.singlezone(name = "example")
>>> sz.schmidt = True
>>> sz.schmidt = False