The graphic calculator plots the stationary transonic wind
solution of the hydrodynamic equations in spherical
symmetry for the case of
an ideal gas in a central gravitational potential.
The temperature profile is assumed isothermal, i.e.
constant and therefore independent of the distance to the center of symmetry.
Originally published by E.N. Parker in 1958
(see Parker, 1958)
the transonic solution of the fluid equations
has been later confirmed to provide a fair approximation
of the real solar wind
by the numerous spacecraft launched
into interplanetary space since the early sixties.
Beside the Sun, other stars have hot coronas from where
a transonic wind, similar to the solar wind, may emanate.
The calculator provides the ability to plot the radial velocity,
the density, the pressure and the electrostatic potential profiles of the wind from a generic
star given its mass, coronal temperature and coronal
radius (i.e. the distance between the position of the temperature
maximum in the corona and the star's center).
The total mass flux (or stellar mass loss) is explicitly computed.
The wind is assumed to be an ideal gas
of singly ionized ions and electrons. The average atomic mass (half of the ion mass plus the electron mass)
can be specified by the user. More sophisticated simulations of the solar wind, starting from
below the solar corona can be found
NB 1: Server may require several seconds to respond to a "submit" action.
NB 2: Connection will fail if you are behind a firewall not allowing access through port 7779 (e.g. on some Wireless Networks).
Choose parameters (defaults are for typical solar conditions)