Abstract:
Coronal mass ejections (CMEs) and their associated shocks are major sources of space
weather. In order to forecast their impact at Earth, it is crucial to accurately model their
propagation in interplanetary space. The only tool capable of treating the large scales of
CME evolution is global magnetohydrodynamics (MHD) modeling. However, this approach
cannot resolve the small scales on which important processes occur (such as the acceleration
of the solar wind and coronal heating). The solar wind solution depends on which method
is utilized to mimic these processes. And because the evolution of a CME depends crucially
on its interaction with the solar wind, the CME evolution will also be connected to the
heating mechanisms and drivers utilized in an MHD model.
In the first part of the thesis, we show that the ad hoc approaches to coronal heating
used in global MHD models leads to unphysical conditions for CME-driven shock formation
in the lower corona (1-10 solar radii). We present this argument in two steps. First, we
present a CME simulation in which the solar wind was accelerated and heated by reducing
the value of the polytropic index (to less than the adiabatic value) in the lower corona.
As it is not well understood, we do not model the CME initiation process - we utilize an
out-of-equilibrium Titov-Demoulin flux rope to begin the eruption. We analyze several
aspects of the CME, such as its kinematics and energy evolution, the shock formation
and evolution, the plasma
flows in the CME-sheath and their connection to the CME
magnetic field vector, and the plasma pile-up at the front of the CME. We find that some
characteristics are inconsistent with the observed properties of CMEs, and we connect these
to the ad hoc treatment of the solar wind heating. Second, we use data of CME shock-accelerated
solar energetic particle events to constrain the profile of the Alfven speed in the
lower corona. We show that the Alfven speed profile from global MHD models with ad hoc
heating is not aligned with these observations, but that local (one dimensional) models with
physically-motivated Alfven wave dissipation as a heating mechanism were in agreement.
In the second part of the thesis, we study the resonant absorption of surface Alfven
waves (SAW), a process which heats the solar wind. It is driven by a transverse gradient
in the local Alfven speed (in relation to the magnetic field direction). In the solar corona,
we expect this mechanism to occur at the boundaries of open and closed magnetic fields.
We make the first estimation of SAW energy dissipation in the solar corona and find that
it is comparable to the ad hoc heating a polytropic model at the boundary of open and
closed magnetic fields and in subpolar open field regions. Next, we implemented the SAW
damping mechanism into the new solar corona component of the Space Weather Modeling
Framework, in which Alfven wave energy transport is self-consistently coupled to the MHD
equations. The model already included wave dissipation along open magnetic field lines,
mimicking turbulence. We demonstrate that including SAW dissipation in the model improved
agreement with observations of coronal temperature both near the Sun and in the
inner heliosphere by comparing with data from Ulysses and the Solar Terrestrial Relations
Observatory (STEREO). Also, the inclusion of SAW dissipation steepened the Alfven speed
profile in the lower corona, aligning the Alfven profile better with observational constraints
of shock formation.
In the final part of the thesis, we modeled a CME in this newly developed solar wind
background, and studied the interaction between the CME and the wind. We generate the
eruption with a flux rope. We constrain the parameters of the flux rope with data from
the 13 May 2005 eruption, including H-alpha images of the pre-eruption magnetic field,
coronagraph images of the CME's shape and velocity. Because the flux rope traveled faster
than the local magnetosonic speed, it acted as a piston and drove a shock wave ahead of it.
The CME-driven shock had a strong impact on the solar wind environment through which it
propagates: it altered the wave energy by concentrating it in the sheath through advection,
and also increasing its value through momentum transfer. This simulation demonstrated
how Alfven waves are focused into the sheaths of ICMEs. The wave energy is then dissipated
at the shock due to SAW damping. The shock heating accounted for 10% of the total change
in thermal energy of the CME. The resulting temperature distribution of the CME is more
aligned with observations than from a CME modeled in a polytropic solar wind.
This thesis has improved our understanding of the interaction between a CME and the
solar wind through which it propagates. Our picture of CME-evolution in the lower corona
will be tested by future missions Solar Probe (which will sample this region directly) and the Solar Orbiter.