  Coronal Mass Ejections (CMEs) are one of the primary drivers of extreme space
weather. They are large eruptions of mass and magnetic field from the solar
corona and can travel the distance between Sun and Earth in half a day to a few
days. Predictions of CMEs at 1 Astronomical Unit (AU), in terms of both its
arrival time and magnetic field configuration, are very important for
predicting space weather. Magnetohydrodynamic (MHD) modeling of CMEs, using
flux-rope-based models is a promising tool for achieving this goal. In this
study, we present one such model for CME simulations, based on spheromak
magnetic field configuration. We have modified the spheromak solution to allow
for independent input of poloidal and toroidal fluxes. The motivation for this
is a possibility to estimate these fluxes from solar magnetograms and extreme
ultraviolet (EUV) data from a number of different approaches. We estimate the
poloidal flux of CME using post eruption arcades (PEAs) and toroidal flux from
the coronal dimming. In this modified spheromak, we also have an option to
control the helicity sign of flux ropes, which can be derived from the solar
disk magnetograms using the magnetic tongue approach. We demonstate the
applicability of this model by simulating the 12 July 2012 CME in the solar
corona.
