vice.singlezone.schmidt
=======================

Type : bool

Default : False

If True, the simulation will adopt a gas-dependent scaling of the
star formation efficiency timescale :math:`\tau_\star`. At each
timestep, :math:`\tau_\star` is determined via:

.. math:: \tau_\star(t) = \tau_{\star,\text{specified}}(t)
	\left(
	\frac{M_g}{M_{g,\text{Schmidt}}}
	\right)^{-\alpha}

where :math:`\tau_{\star,\text{specified}}(t)` is the user-specified
value of the attribute ``tau_star``, :math:`M_g` is the mass of the
interstellar medium, :math:`M_{g,\text{Schmidt}}` is the normalization
thereof (attribute ``MgSchmidt``), and :math:`\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.

.. seealso::
	- 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

.. [1] Kennicutt (1998), ApJ, 498, 541
.. [2] Schmidt (1959), ApJ, 129, 243
.. [3] Schmidt (1963), ApJ, 137, 758