I love running and exploring simulations of galaxies and gas evolution in the universe. I recently received my PhD from the University of Wisconsin - Madison working with Professor Elena D'Onghia on simulations of the formation of the Magellanic Stream. My work predicted the existence of the "Magellanic Corona" - a warm circumgalactic medium around the Large Magellanic Cloud that is the source of the ionized gas in the Stream today. The Magellanic Corona has recently been observed in high ions using HST/COS absorption-line spectroscopy.
I have also been working with an undergraduate student on developing wavelet transformation and analysis code in Python to map stellar moving groups in the Milky Way using Gaia data.
More information on my recent endeavors can be found at the Mad Astro Dynamics group website.
In the past, I have completed projects on characterizing light curves of "ultra-long period" Cepheid variable stars, detecting and analyzing the evolution of canopy regions on the Sun using AIA images from the Solar Dynamics Observatory, and constraining theoretical mechanisms of jet formation in proto-planetary nebulae. I also received a Master's degree in Theoretical Physics from the University of Edinburgh in 2017 where I performed calculations in self-dual Yang-Mills theory to learn more about the connection between quantum field theory and quantum gravity using the double copy.
ASTROPHYSICISTPHOTOGRAPHERDANCER
The bulk of my work over the past few years has been in running N-body hydrodynamical simulations of the formation of the Magellanic Stream. These simulations have shown that a warm circumgalactic medium around the Large and Small Magellanic Clouds (LMC/SMC), the Magellanic Corona, is a key ingredient in being able to account for the high ionization fraction and total mass of the Stream. Previous works had not been able to explain the massive amount of ionized gas (~2 billion solar masses) which makes up the majority of the Stream's mass budget. Since the Magellanic Corona is expected to be around the virial temperature of the LMC (3×105 K for an LMC halo of 2×1011 solar masses), this gas should be ionized. Therefore, as the Magellanic Clouds fall in towards the Milky Way, the Magellanic Corona is warped and stretched by the Milky Way's gravitational potential and its own hot circumgalactic gas. This work was published in September 2020 in Nature:
Lucchini, S., D'Onghia, E., Fox, A. J., et al. 2020, Nature, 585, 203, doi: 10.1038/s41586-020-2663-4, arXiv:2009.04368
Lucchini, S., D'Onghia, E., Fox, A. J., et al. 2020, Nature, 585, 203, doi: 10.1038/s41586-020-2663-4, arXiv:2009.04368
Upon the inclusion of the Magellanic Corona, the interaction history of the Magellanic Clouds will be changed. The Magellanic Corona not only provides additional gravitational potential, but the hydrodynamical friction and ram-pressure forces also cause the SMC's orbit around the LMC to decay more quickly. My second paper presented improved models in which the present-day positions and velocities of the Magellanic Clouds match their observed values within 3 sigma. Exploring the parameter space of possible orbits through analytical integration, we selected 10 and ran them in full hydrodynamical simulations using GIZMO. 7 out of the 10 formed Streams all with similar properties. The interaction history that best matched the present-day velocities of the Clouds includes two interactions over 3.4 billion years tidally producing a Trailing Stream and gaseous Bridge. The most interesting result is that in all 7 simulated Streams, the stripped gas ends up very close to the Sun, as close as 20 kiloparsecs away, which is a significant paradigm shift from previous models which predicted distances out to 100-200 kiloparsecs away. This work was published in November 2021 as a Letter in the Astrophysical Journal:
Lucchini, S., D'Onghia, E., & Fox, A. J. 2021, ApJL, 921, L36, doi: 10.3847/2041-8213/ac3338, arXiv:2110.11355
Lucchini, S., D'Onghia, E., & Fox, A. J. 2021, ApJL, 921, L36, doi: 10.3847/2041-8213/ac3338, arXiv:2110.11355
I have also been working with two undergraduates at UW - Madison on the detection and characterization of stellar moving groups in the Milky Way. We have developed a new, open-source Wavelet Transformtion code, MGwave (soon to be available on GitHub) to analyze Gaia data. Selecting stars near the Sun, we use MWwave to identify substructures in velocity space. The figure shows the histogram of stars in azimuthal velocity vs radial velocity space (in Galactocentric coordinates), and its corresponding wavelet transformed image in which purple (green) regions denote over (under) densities and the red (blue) crosses show the locations of the maxima (minima). Using the third data release from Gaia, we detected three new moving groups (circled) and three additional groups previously not seen in Gaia data (squares). This work has been published in MNRAS:
Lucchini, S., Pellett, E., D'Onghia, E., & Aguerri, J. A. L. MNRAS, 519, 1. (2023) arXiv:2206.10633
Lucchini, S., Pellett, E., D'Onghia, E., & Aguerri, J. A. L. MNRAS, 519, 1. (2023) arXiv:2206.10633
With the third data release from Gaia, we now have over 30 million stars with full 3D position and 3D velocity data. This allows us to explore the kinematic structure of the Milky Way throughout the disk. In the image, we're showing the locations of the maxima in the wavelet image as we progress through Galactocentric radius. The points are colored by their radius value and you can see that many of the structures that we see in the solar neighborhood (shown as squares) are connected throughout the rest of the disk. This indicates that these moving groups are large-scale structures likely formed through gravitational effects instead of local, transient features. The properties of these extended moving groups can then tell us about the gravitational potential and non-axisymmetric features of the Milky Way.