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Tod Strohmayer's Webpage at NASA/GSFC

Picture of Tod Strohmayer

How to reach me:

Mail Code 662 (X-ray Astrophysics Laboratory) 
Greenbelt, MD 20771 
voice: 301-286-1256 
fax: 301-286-1684 
email: Tod.E.Strohmayer@nasa.gov

Here is my  CV

Learn about the Rossi X-ray Timing Explorer (RXTE) and its Discoveries

RXTE mission patch, link to RXTE website


My research interests in astrophysics center around the physics and properties of compact stars, with particular emphasis on neutron stars, neutron star binaries, and black holes.  For an introduction to neutron stars and what makes them so interesting, take the neutron star tour. Some of the research projects I am currently involved with include;
  • High Frequency X-ray Variability of Stellar Mass Black Holes.
  • Black Holes are the most extreme objects we can study in the universe. X-ray observations probe the regions closest to the black hole event horizon, beyond which nothing can escape. Oscillations (QPOs) in the X-ray flux with frequencies of hundreds of Hz have been found by RXTE. These can only be produced in the immediate environs of the event horizon. Black Holes curve the space-time around them in a way described by Einstein's General Theory of Relativity (GR). By studying these QPOs we can test this theory at its extremes in a unique way. GR predicts that only two parameters, the black hole mass and spin, control how space-time is curved by the black hole. This is the famous "no hair theorem" for black holes. RXTE observations have found the highest frequency QPO from a black hole, at 450 Hz (from GRO J1655-40, a Galactic microquasar which also shows relativistic jets in the radio band). The mass of this black hole is known from optical studies of its orbital dynamics. The high frequency QPOs suggest that it must be a spinning black hole. See the paper, "Discovery of a 450 Hz QPO from the Microquasar GRO J1655-40 with the Rossi X-ray Timing Explorer", for more details. The image below is a depiction of what the binary system containing the black hole GRO J1655-40 might look like if you could see it up close.
    Idealized picture 
of the black hole binary GRO J1655-40

  • Superbursts from Accreting Neutron Stars
  • The material which is accreted by a neutron star in a binary system builds up in a thin layer  on its surface. Over several hours enough material can be accumulated so that near the base of this layer it is hot and dense enough to initiate thermonuclear reactions amongst the Hydrogen and Helium nuclei. These reactions can occur in an unstable manner which causes strong heating of the neutron star surface. This heat energy produces brief flashes, or bursts, of X-rays from the neutron star. Usually such flashes only last about 10 - 20 seconds, however, a new type of X-ray burst behavior has been found in the last few years, which lasts for hours not seconds. These very long bursts are called "superbursts," and they are caused by thermonuclear burning of a much thicker and deeper layer of accreted material than that which causes the 10 - 20 second bursts. The layers responsible for the superburst are made up of the "ashes" of the light element fusion which takes place above it. It takes years for enough ash material to build up, so these events are quite rare and only seven have been observed so far. Our group has observed two of these superbursts with the PCA on RXTE. The figure below shows the X-ray intensity profiles from these superbursts, one from 4U 1820-30, the other from 4U 1636-53.
    X-ray lightcurves of two 

    4U 1820-30 is an ultra-compact binary system with an orbital period of only 11 minutes. The entire binary system would easily fit within the Sun. The image below left shows a rough scale model of the system. The Earth and Sun are shown to give an approximate idea of the size of the system.

depiction of the X-ray binary 4U 1820-30. Sun and Earth provide size scale

    The companion star in this system is a Helium white dwarf. The nuclear fusion of this Helium produces a lot of Carbon, which is a likely fuel for the superburst seen from this object. See the paper, "A Remarkable 3 Hour Thermonuclear Burst from 4U 1820-30", by Dr. Edward Brown (University of Chicago) and myself for all the details. The superbursts provide a tantalizing look at the surface and deep "ocean" of neutron stars. We also discovered spectral lines during this superburst. These spectral features could be caused by reflection and reprocessing of the burst flux from the accretion disk in 4U 1820-30. Observations of superbursts with much higher spectral resolution could provide new methods to probe both the accretion disk and the neutron star itself. A new way to do this could be to use the Swift Gamma-ray Burst Mission as a trigger for Target of Opportunity (TOO) observations. The figure below shows the spectral features seen during the superburst from 4U 1820-30.

    X-ray spectrum of 
a superburst showing emission line and absorption edge.

  • Millisecond X-ray Variability in Accreting Neutron Star Binaries.
  • In February, 1996, a few months after the launch of  RXTE,  our research group discovered extremely rapid variability in the X-ray emission from accreting neutron stars.  Some of the oscillations we have discovered occur at frequencies greater than 1,000 cycles/sec, or Hz, and are the most rapid periodic variations yet observed from cosmic sources! We use these observations to learn about neutron stars and black holes. The image below shows some of these high frequency, quasiperiodic oscillations (QPO) in 3 orbits of data obtained with the  PCA  from the low mass X-ray binary (LMXB) 4U 1728-34.  The high frequency quasiperiodic oscillations (QPO) show up as a pair of nearly parallel orange lines running up the image. The QPO frequencies also increase as the X-ray intensity increases.  For more details follow the link to "Millisecond X-ray   Variability from an  Accreting Neutron Star System" .
QPOs from the X-ray binary 4U 1728-34

  • Millisecond Oscillations During Thermonuclear X-ray Bursts
  • An 
X-ray burst from the X-ray binary 4U 1702-429 with 330 Hz oscillations. Image 
of a dynamic power spectrum.

  • Studies of Soft Gamma-ray Repeaters (SGRs) and Magnetars:
  • SGRs are rare, repetitive sources of very intense hard X-ray  flashes. There are four such sources currently known, and they are all associated with young supernova remnants, neutron stars and point like X-ray sources. A nice resource for background information on SGRs is Robert Duncan's Magnetar webpage.
  • "X-ray Spectral Characteristics of GINGA Gamma-Ray Bursts"
  • While at Los Alamos I worked on a study of the X-ray spectral properties of gamma-ray bursts. Take a look at the paper which describes the X-ray spectral properties of a sample of Gamma-ray Bursts observed with the burst detector which flew on the Japanese X-ray astronomy satellite GINGA.  X-ray Spectral Properties of Gamma-ray Bursts .
  • X-ray Spectroscopy of Neutron Star Binaries and Bursters
  • The newest X-ray astronomy missions, such as NASA's recently launched  Chandra X-ray observatory and European Space Agency 's (ESA) soon to be launched X-ray Multiple Mirror Mission (XMM) are powerful tools for high resolution spectroscopy of X-ray sources. With colleagues Jean Swank, Craig Markwardt and Tim Kallman I am studying  accreting neutron star binary systems and bursters with the high resolution spectroscopic capabilites afforded by these new X-ray observatories.

    This file was last modified on Monday, 29-Oct-2007 13:01:58 EDT

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