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Tony Piro

(626) 304-0297

Carnegie Observatories
813 Santa Barbara Street
Pasadena, California, 91101

piro[at]carnegiescience.edu

Background

I am the George Ellery Hale Distinguished Scholar in Theoretical Astrophysics at the Carnegie Observatories. My research is focused on theoretical astrophysics with a broad interest in topics involving compact objects, astrophysical explosions, accretion flows, and stellar dynamics. I draw on my expertise in nuclear physics, thermodynamics, condensed matter physics, General Relativity, and fluid and magnetohydrodanmics both to predict new observational phenomena as well as to understand the key underlying physical mechanisms responsible for current observations. Practically, I take a more classical approach to solving these problems — using a combination of analytic and simple numerical models to build physical intuition for complex phenomena.

Recent and Past Work
Scialog award for supernova study

Scialog is a unique approach to supporting early career scientists, funded by the Research Corporation for Scientific Advancement (RCSA). Instead of a normal grant submission process, a group of 45 Scialog fellows participate in a discussion-focused conference where we rotate between smaller groups to talk about a variety of hot topics. At the end of two days, the fellows form two to three person teams to write competitive proposals, which we present to a panel of judges on the third day.

My group won one of seven 2016 Scaialog awards for a collaborative project that includes numerical theorist Daniel Kasen (University of California, Berkeley) and observer Nathan Smith (University of Arizona). We propose to combine theoretical predictions with observations to solve previously unexplained mysteries about supernovae and how massive stars end their lives.

Our project makes use of many of the unique resources available at the Carnegie Observatories. The main idea is that many massive stars may have increased activity near the end of their lives, which may exhibit itself best by carefully studying the supernovae produced as the stars die. My recent theoretical work predicts what signatures should be seen and how these signatures should be interpreted. The extreme sensitivity of Carnegie’s Magellan telescopes are perfect for finding these signs of activity.

You can read more about this award at the websites of the Carnegie Observatories and RCSA.

A new kind of cosmic flash may reveal the birth of a black hole

Even though we know that black holes exist in our galaxy, it is still a fundamental problem to understand what kinds of massise stars produce them and what is the observational signature when they form. Does the star explode in a giant flash of light or does it die with a wimper?

In my recent work I showed that the answer may lie somewhere in between. Before a black hole forms inside a star, it is a neutron star for a few seconds. During this time it radiates neutrinos, which pass out of the core and carry away energy. In fact they can carry away an amount of energy equivalent to half the mass of the sun! (Remember Einstein's relation between mass and energy.) When this mass is removed, the envelope of the star suddenly feels less gravity, begins expanding, and this expansion steepens into a shock. This shock produces a flash of light when it hits the surface of the star that lasts for the next few days. Although much dimmer than a normal supernova, this flash would still be observable allowing us to actually see a black hole in the act of forming.

This idea made its way into the popular press, and you can read more at the Physics World, Universe Today, Science Daily, and Caltech

Using supernovae to measure the radii of dying stars

A Type Ia supernova is the explosion of a star that can be as bright as 10 billion stars. Thousands of these events have been observed, and they have even been used to measure the expansion history of our Universe. This led to the discovery of dark energy, for which the 2011 Nobel Prize in Physics was awarded. Nevertheless, how these stars explode and what the progenitor stars are remains a puzzle.

In previous work I made theoretical predictions of what would be seen when the burning front first reached the star's surface, showing that it is strongly dependent on the radius. But I was skeptical whether this relatively dim effect would ever be observed. Amazingly, in August 2011, supernova 2011fe exploded in the nearby Pinwheel Galaxy--the closest Type Ia in almost 40 years! Although the effect I predicted was not detected, the event was close enough that my work could be used to place constraints on the exploding star's radius. The conclusion was that the radius must have been less than 1/50th the size of our Sun. This means that it was almost certainly a white dwarf, which is the first time this has been directly confirmed.

More recently, I have done modeling of supernova 2011fe's lightcurve over the first 5 days to show that it must have had radioactive material near it's surface. This puts important constraints on the models for how the star exploded.

Measuring tides as stars inspiral due to General Relativity

Stars in close binaries produce gravitational waves, ripples in space and time first predicted by Einstein. These waves carry away energy and angular momentum, which causes a binary to shrink and may lead to merger. The most famous example is the Hulse-Taylor binary pulsar consisting of two neutron stars in an 8 hour orbit. Measurement of this system's inspiral provided the first indirect evidence of gravitational waves, for which the 1993 Nobel Prize in Physics was awarded.

White dwarf binaries also produce gravitational waves. The most extreme case was announced in the summer of 2011, which has an incredible 13 minute orbital period! In theoretical work I showed that tidal interactions spin up the white dwarfs, which removes angular momentum from the orbit. This causes the binary to inspiral more quickly than what would be expected from gravitational waves alone. Although this effect has not yet been detected, it should be found in data taken over the next year. This would provide an unprecedented measurement of tidal interactions in a compact binary, which will have important implications for what will happen when the white dwarfs eventually merge.

Research Interests

Below is a list of some of my research projects. For some I have included links to simple summaries that give an introduction to these exciting topics.

Links