\documentclass[10pt]{article}
\usepackage[usenames]{color} %used for font color
\usepackage{amssymb} %maths
\usepackage{amsmath} %maths
\usepackage[utf8]{inputenc} %useful to type directly diacritic characters
\begin{document}
\begin{align*}
Dhruv Muley
Dhruv Muley
PhD student, Max-Planck-Institut für Astronomie (MPIA)
Hydrodynamical simulations of disk/planet interaction
Intro
I am a final-year PhD student at the Max Planck Institute for Astronomy, in Heidelberg, Germany, performing numerical simulations of protoplanetary disks with Hubert Klahr. Previously, I was a research assistant with Ruobing Dong at the University of Victoria from 2020-21, and studied at UC Berkeley from 2016-2020 where I worked with Jeffrey Fung, at the time a NASA Sagan Postdoctoral Fellow.
Besides research, I have been a teaching assistant for Alex Filippenko's Astronomy C10 general-astronomy class at Berkeley, leading weekly discussion sections. The course materials I composed can be found here. I have also taught for the Be a Scientist program, helping middle-school students devise and run science experiments. In my spare time, I enjoy hiking on local trails and have recently taken up salsa dancing.
Work done with Ruobing Dong at the University of Victoria on the strength and observability of temperature perturbations created in planet-driven spiral arms in circumstellar disks. We find that Saturn- or Jupiter- mass planets in adiabatic disks should be clearly detectable in 12-CO, and create a signature reminiscent of that found in the TW Hya system by Richard Teague et al., but that lower-mass planets may be more difficult to find. Buoyancy spirals are thin but prominent close to the planet, while Lindblad spirals extend farther away. (UNDER CONSTRUCTION)
The PDS 70 system, imaged in scattered-light by SPHERE. The super-Jupiter planet candidate, PDS 70b, is visible as a bright blob to the right of the coronagraph. Credit: ESO/A. Müller et al.
Planets have long been believed to have formed in circumstellar disks, but how exactly they influence disk evolution and dispersal has remained a mystery. The PDS 70 system—one of a handful in which a planet candidate has been directly imaged within its natal disk—provides a valuable window onto this process. Traditional theory states that the super-Jupiter companion, located at 22 au, should exchange angular momentum with disk material and carve out a gap of approximately equal width. Indeed, PDS 70 does have a gap—but it extends to ~65 AU, making it twice as wide as the theory predicts! To make matters more puzzling, this wide gap is not an anomaly, but rather represents many late-stage "transition disks" in the process of dispersing to give way to planetary systems.
Using the PEnGUIn hydrodynamical code, we simulated the the accretion and orbital evolution of the companion, PDS 70b, in its disk over the system's ~5 Myr lifetime. We find that when the planet reaches super-Jupiter mass, it spontaneously becomes eccentric and accretes from a broader region of the disk. This "fiducial" model accurately reproduces the gap profile observed in PDS 70, which our 100+ alternative models (varying disk temperature, density, fixed vs. moving planets, etc.) failed to do. Moreover, the fiducial setup is simple and requires little fine-tuning for its predictive power. Our results show that single, super-Jupiter planets can sculpt the characteristic wide cavities of transition disks, and that the high eccentricities measured for such planets may in part arise from disk-planet interaction.
Dwarf galaxies
Muley, Dhruv; Wheeler, Coral R.; Hopkins, Philip F.; Wetzel, Andrew; Emerick, Andrew; Kereš, Dušan. "Progenitor-mass-dependent yields amplify intrinsic scatter in dwarf-galaxy elemental abundance ratios," Monthly Notices of the Royal Astronomical Society, (2021; accepted, ArXiv: 1909.02006)
The FIRE project has, over the past decade, produced increasingly accurate simulations of galaxy evolution, addressing problems from missing-satellites to the Kennicutt-Schmidt relation. Among the remaining discrepancies is the fact that in observed stars, the ratio of α-elements (e.g., Mg, Si, Ca, Ti) to iron ([α/Fe]) exhibits a wide intrinsic scatter at any given metallicity [Fe/H]; in simulations, however, stars tend to lie on a tight [α/Fe]-[Fe/H] relation. One potential cause is that in typical simulations, all Type II supernovae (which produce most α-elements, particularly at early times) are identical, with uniform IMF-averaged yields. Thus, when they enrich the surrounding gas (which subsequently forms future generations of stars), they do so with a constant ratio of [α/Fe].
In reality, however, the yields of Type II supernovae, and thus the production of α-elements and Fe, can vary substantially for different progenitor masses. To account for this in the FIRE simulations, I spent my summer 2019 as a SURF fellow at Caltech, implementing time- (and thus progenitor-mass-) dependent yields from the NuGrid stellar evolution suite. Our simulations of dwarf galaxies show a clearly wider scatter in [α/Fe] for each [Fe/H], and we have a paper in preparation. In the future, our prescription could be used to perform mock galactic archaeology on individual stellar populations within simulated Milky Way-type galaxies.
Teaching
The Mice Galaxies, as seen by Hubble. Credit: NASA, H. Ford (JHU), G. Illingworth (UCSC/LO), M.Clampin (STScI), G. Hartig (STScI), the ACS Science Team, ESA
In Fall 2018 I was an "undergraduate student instructor" (teaching assistant) for Alex Filippenko's Astronomy C10, a general astronomy class for non-science majors at UC Berkeley. In this capacity, I led weekly discussion sections and held office hours for ~60 students in a class of 900. Selected course materials I wrote are linked below; quizzes and practice exams available upon request.
Evolution of the Kelvin-Helmholtz instability. Credit:Jim Stone
I am a third-year PhD student at the Max-Planck-Institut for Astronomie, having previously worked at the University of Victoria (2020-21) and studied at UC Berkeley (2016-20). My full curriculum vitae may be found here; also find me on LinkedIn here.
This is bold and this is strong. This is italic and this is emphasized.
This is superscript text and this is subscript text.
This is underlined and this is code: for (;;) { ... }. Finally, this is a link.
Heading Level 2
Heading Level 3
Heading Level 4
Heading Level 5
Heading Level 6
Blockquote
Fringilla nisl. Donec accumsan interdum nisi, quis tincidunt felis sagittis eget tempus euismod. Vestibulum ante ipsum primis in faucibus vestibulum. Blandit adipiscing eu felis iaculis volutpat ac adipiscing accumsan faucibus. Vestibulum ante ipsum primis in faucibus lorem ipsum dolor sit amet nullam adipiscing eu felis.
Preformatted
i = 0;
while (!deck.isInOrder()) {
print 'Iteration ' + i;
deck.shuffle();
i++;
}
print 'It took ' + i + ' iterations to sort the deck.';
I am a final-year PhD student at the Max Planck Institute for Astronomy, in Heidelberg, Germany, performing numerical simulations of protoplanetary disks with Hubert Klahr. Previously, I was a research assistant with Ruobing Dong at the University of Victoria from 2020-21, and studied at UC Berkeley from 2016-2020 where I worked with Jeffrey Fung, at the time a NASA Sagan Postdoctoral Fellow.
