research focuses on solar eruptions a.k.a. coronal mass ejections (CMEs),
the most energetic events in our solar system. I believe in using as many
"tools" as possible to study these events, therefore I have been
combining numerical simulations, "artificial" observations and
So far, my main interests have been: (i) the study of the interaction of
multiple CMEs between the Sun and the Earth, (ii) the study of
phenomena associated with the initiation of solar eruptions: the
formation and deflection of the ejecta and the shock wave and the
acceleration of energetic particles, (iii) the study of
observations of CME in the heliosphere by coronagraphs and
heliospheric imagers and their association with in situ measurements, and (iv), recently, the study of in situ measurements associated with solar transients.
The introduction and conclusion of my dissertation give a good but somewhat dated
(ca. 2006) overview of the scientific background and challenges of the study of successive CMEs
(introduction and conclusion of my dissertation).
A CME observed by STEREOA/SECCHI/COR2
In slightly more details, I have been involved in the following research
|MHD model of 2 interacting CMEs from Lugaz et al., ApJ, 2005b
|| STEREO-B/HI1 view of 2 interacting CMEs
from Lugaz et al., ApJ, 2012
MHD modeling of the low coronal evolution of a CME
from Lugaz et al., ApJ, 2011
have studied the interaction of two and three coronal mass ejections from the
Sun to the Earth in three-dimensions using a magneto-hydrodynamical (MHD)
code. We studied the formation of a complex ejecta and multiple-magnetic
cloud events. Here is an ScienceNews article from October 2012 about the interaction of solar eruptions.
have studied heliospheric observations of CME-CME interaction by
STEREO/SECCHI with the help of MHD simulations (for the January 2007 events)
or without it (for the May 2010 events).
have also been involved with Ilia Roussev, Carla Jacobs, Klaus Galsgaard and
others in the development of more realistic models of CME initiation and
their consequences for the properties of CMEs. In 2012, this resulted in a Nature Physics article and a UNH press
release . From 2010 to 2012, I was also involved in the
development of the Low Corona (LC) model by Cooper Downs and its use to study
of EUV waves. In particular, I used this model to study the coronal evolution of
a CME, interchange reconnection and the formation of dimming regions.
I spent some time developing new analysis techniques for heliospheric imagers (wide-angle coronagraphs), referred to as the Harmonic Mean (HM) techniques.
I have been funded since 2008 by NASA (Living With a Star and Solar and
Heliospheric programs) and NSF (National Space Weather Program, SHINE and
Currently Funded Proposals:
- NSF: SHINE The Non-Ideal Evolution of CMEs: Numerical Studies, AGS1239704: 250k$, 03/2012 - 02/2015.
- NASA: Living with a Star (LWS) Evolution of the Magnetic Fied in Solar Transients Between the Corona and 1 AU, NNX15AB87G: 536k$, 12/2014 - 11/2018.
- NASA: Solar and Heliospheric Physics Numerical Investigation of CME Evolution in the Corona and Inner Heliosphere, NNX13AH94G: 365k$ (incl. subaward), 11/2011 - 10/2014.
- NASA: Living with a Star Targeted Research and Technology (LWS TR&T) - NNX08AQ16G: 360k$ (incl. sub-awards), 05/2008 - 04/2012.
- NSF: National Space Weather Program, AGS0819653: 190k$, 08/2008 - 07/2012.
- NSF: Solar-Terrestrial, AGS1239699: 305k$ (incl. sub-award), 12/2011 - 12/2014.
- Japanese Society for the Promotion of Science (JSPS), Short-Term Post-doctoral fellowship at Kyoto University, ~35k$, 10/2010 - 05/2011.
My list of publications can be found here or under the publication tab.
Publications on CME initation and coronal evolution of CMEs (simulations)
Publications on the Harmonic Mean (HM) method for data from heliospheric imagers
Publications on CME-CME interaction
Publications on numerical simulations of STEREO/SECCHI observations (simulations)
Publications on the Jovian magnetosphere (Master work)
A pdf version of my resume including a list of publications can once again be found here.