Welcome

Hello and welcome to my webpage! I'm a professor researching theoretical astrophysics at the California Institute of Technology. Most of my research focuses on the physics of vibrating fluid spheres. Although this sounds esoteric, the applications within astronomy are nearly limitless! As a graduate student, I studied tidal interactions in merging white dwarf systems, heartbeat stars (oscillating stars in eccentric binary systems), and compact triple star systems. More recently, I have studied magnetic fields inside of red giants, the deep interior of Saturn as revealed by its rings, and the long term evolution evolution of Saturn's moons.

I am currently working on projects involving everything from exoplanets to supergiant stars to black holes. Specific topics include:

  • The transport of angular momentum inside of stars and the resulting spin rates of white dwarfs, neutron stars, and black holes.
  • The occurrence and appearance of pre-supernova outbursts in massive stars, and their effect on subsequent supernovae.
  • The orbital migration of exoplanets tidally interacting with their host stars.
  • The internal structure of Saturn from ring seismology.
Read more about my research below!

Research Topics

Some of my recent research topics are listed below. Click on the images to read more on my research page!

Migration and Heating of Planetary Moons

Jupiter and Saturn's rapid rotation slowly pushes their moons outward via tidal effects, which also leads to tidal heating of the moons. Recent measurements show the moons migrate faster and are heated more than expected, which is likely explained by a process called resonance locking.

Tidally Trapped Pulsations

Stars in close binary systems are tidally distorted, causing their pulsations to be focused and trapped in certain parts of the star. While this distorts their asteroseismic signals, it also helps us identify the star's pulsation modes as they are modulated over the orbital cycle.

Merging White Dwarfs

White dwarfs with short orbital periods will emit gravitational waves, causing the orbit to decay until the white dwarfs merge. I study the interactions between the stars before they merge. What happens after the white dwarfs merge? A type Ia supernova? A helium burning supergiant? A heavier white dwarf? Take your pick!

Black Hole Spin

As the cores of stars contract during their lifetime, the inner layers may begin to rotate faster than the outer layers, with crucial consequences for the spins of neutron stars and black holes. I've been studying the processes in stars that redistribute angular momentum to determine the birth spin rates of compact objects.

Pre-Supernova Outbursts

Stars more than ten times the mass of the Sun explode as supernovae when they end their lives. My research suggests that some of these stars may undergo violent outbursts in the last several years of their lives, giving us a warning sign that they are about to explode. If we can identify these warning signs, we will be able to observe supernovae in much greater detail.

Heartbeat Stars

Click Here for Interactive Model of KIC 8164262!!!

Heartbeat are eccentric short-period binary stars. The characteristic "heartbeat'' signal (resembling an EKG diagram) in their light curves is produced by a combination of tidal distortion, reflection, and Doppler boosting near orbital periastron. Hearbeat stars are a great chance to directly observe tidal effects in action!

The Magnetic Greenhouse Effect

Asteroseismology allows us to peer into the hearts of stars, often yielding surprises! In red giant stars, we have learned how to detect powerful magnetic fields buried within the stars' central cores, providing the first ever measurements of magnetic fields in the deep interiors of stars.

Saturn Ring Seismology

What is inside of Saturn? We don't know! But there are some clues are hidden within Saturn's rings. The rings can be used as a seismograph, allowing us to detect "Saturn quakes", which can help us learn what lies deep within the planet's interior.

Neutron Star Spin

The initial spin period of a pulsar is determined by the massive star which spawned it during a core-collapse supernova. Waves created by vigorous nuclear fusion in the last hours of the star's life may be crucial in determining how fast the neutron star progeny spins when it is born.

Supernova Seismology

Core-collapse supernovae are violent events that give birth to neutron stars and black holes. If the core of the massive star is rapidly rotating, the collapse generates powerful gravitational waves, which could be used to peer into the heart of the supernova.

Triple Star Systems

In close triple star systems, the stars can interact in unexpected ways. One compact triple system imaged by the Kepler satellite has shown that the motions of a pair of stars can excite oscillations within a close third star. These oscillations may alter how close triple systems evolve.

Undergraduate Research

I enjoy working with motivated undergrads, however I only have time to mentor one or two at a time. If you are a non-Caltech student interested in doing an undergraduate research project with me, please send me an email with the subject heading "Undergraduate research project". I usually look for summer undergraduates in February, and likely won't be able to respond until then.