Tuesdays at 4:00 PM in the Marlar Lounge, Room 37-252
MIT Kavli Institute for Astrophysics and Space Research
70 Vassar Street, Cambridge, MA
(unless location otherwise noted)
Refreshments are served at 3:45 PM.
the Astrophysics Division of the MIT Department of Physics and
the MIT Kavli Institute for Astrophysics and Space Research.
Tuesday Sep 13:
A New Era of Compact Objects
University of Arizona
Host: D. Chakrabarty
The discovery of many diverse populations of neutron stars and black holes is happening at an accelerating rate. The computational advances in calculating the properties of these compact objects, their multiwavelength observations, and the new avenues of studying them with gravitational waves have led to a new understanding of their formation, evolution, and of the fundamental physics that shapes their characteristics. In this talk, I will describe these parallel advances and show how this multi-faceted approach helps pin down our understanding of the evolution of massive stars, supernova explosions, and coalescing compact objects.
Tuesday Sep 20:
Dissecting the Multiphase Circumgalactic Gas
University of Chicago
Host: R. Simcoe
Tremendous progress has been made over the last decade in our empirical
and theoretical understanding of how galaxies form and evolve across
cosmic time. In particular, state-of-the-art cosmological simulations can
not only match the large-scale statistical properties of galaxies, but
they can also successfully reproduce the observed small-scale features.
This success shows that the basic theoretical framework for modeling galaxy
formation is on the right track. However, it appears that these models
have fallen short in matching the empirical properties of diffuse gas,
which constitutes 90% of all baryons in the universe, beyond visible galaxy
disks and into circumgalactic space. An accurate characterization of the
complex physical processes that govern the interactions between
star-forming regions and this diffuse circumgalactic medium (CGM) is a
critical next step toward a comphrehensive undersetanding of galaxy
formation and evolution. I will highlight some of the observational
efforts of my group at the University of Chicago to identify the dominant
mechanisms which define the CGM properties.
Tuesday Sep 27:
Host: P. Schechter
Abstract: Tuesday Oct 4:
Abstract: Tuesday Oct 11:
NO COLLOQUIUM: COLUMBUS DAY BREAK
Tuesday Oct 18:
How to Tell When You've Busted CDM
University of Maryland
Host: S. Hughes
Cold dark matter, along with dark energy, constitute 96% of the universe. Calculations using these components have successfully explained many aspects of structure formation, but as is appropriate for such a broad framework there have also been multiple challenges along the way. One recent challenge involves the existence of structure in the satellite galaxy distributions of the Galaxy and M31, such as thin planes with apparent kinematic coherence, which have been claimed to be inconsistent with the results from dark matter simulations. However, these are a posteriori claims: a pattern is seen in data, and then that particular pattern is analyzed for significance, which can easily lead to misleading assessments of improbability. I will discuss different statistical methods to determine more objectively whether observed patterns are consistent with data, and will also discuss planned future work to help compare different models of cold dark matter.
Tuesday Oct 25:
The Standard Model of Cosmology?
Johns Hopkins University
Host: J. Hewitt
As cosmological observations accumulated in the 1980s and 1990s a strange model emerged, a hot big bang universe dominated by nonbaryonic dark matter and an unexpected dark energy driving an accelerated expansion of the universe. Epic advances in measurement accuracy and precision in the decade of the 2000s put this model to an enormously rigorous test leaving us with a Standard Model of Cosmology: the LCDM model with 6 well-specified parameters. New measurements from just the past 3 years now raise the question, do we still have a standard model of cosmology: a LCDM model with 6 well-specified parameters? In this talk I will examine recent results of supernovae measurements of the Hubble Constant, measurements of baryon acoustic oscillations, and multiple measurements of the cosmic microwave background in the context of the LCDM model. I will also discuss some next experimental steps in observational cosmology.
Tuesday Nov 1:
Observations of Quasar Feedback
Johns Hopkins University
Host: P. Schechter
Quasars are now thought to have made critical impact on galaxy formation. Feedback from accretion onto supermassive black holes is implicated in establishing the black hole mass vs galaxy bulge correlations and in limiting the maximal mass of galaxies. In this talk, I will review the indirect evidence for quasar feedback as required by galaxy formation models. I will then present recent multi-wavelength observations of powerful quasar-driven winds and outflows on galaxy-wide scales. These data may provide direct observational evidence for one of the long-standing paradigms in galaxy formation.
Tuesday Nov 8:
Abstract: Tuesday Nov 15:
A Galactic Scale Gravitational Wave Observatory
West Virginia University
Host: S. Hughes
Pulsars are rapidly rotating neutron stars with phenomenal rotational stability that can be used as celestial clocks in a variety of fundamental physics experiments. One of these experiments involves using an array of precisely timed millisecond pulsars to detect perturbations due to gravitational waves. The gravitational waves detectable through pulsar timing will most likely result from an ensemble of supermassive black hole binaries. I will describe the efforts of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), a collaboration which monitors an array of over 50 millisecond pulsars with the Green Bank Telescope and Arecibo Observatory. The most recent limits on various types of gravitational wave sources will be presented, and I will show how these limits are already constraining models for galaxy formation and evolution. I will then describe the dramatic gains in sensitivity that are expected from discoveries of millisecond pulsars, more sensitive instrumentation, improved detection algorithms, and international collaboration and show that detection is possible before the end of the decade.
Tuesday Nov 22:
Frontiers in Massive Stellar Death
Michigan State University
Core-collapse supernovae are the luminous explosions that herald the death of massive stars. While core-collapse supernovae are observed on a daily basis in nature, the details of the mechanism that reverses stellar collapse and drives these explosions remain unclear. While the most recent high-fidelity simulations show promise at explaining the explosion mechanism, there remains tension between theory and observation. I will discuss the recent developments in the study of the supernova mechanism that could lead to a predictive theory of massive stellar death. In particular, I will describe our efforts to develop more realistic initial conditions for supernova simulations with fully 3D massive stellar evolution calculations. Such realistic 3D initial conditions turn out to be favorable for successful explosions, in large part because they result in stronger turbulence behind the stalled supernova shock. I will also discuss the important role turbulence is playing in the supernova mechanism and what might be required for accurately modeling the turbulence in our simulations. I will also mention recent work aimed at explaining the origin of pre-supernova outbursts from massive stars in the months and years prior to core collapse and explosion.
Tuesday Nov 29:
Turbulence in the Intracluster Medium
Host: M. Bautz
Intracluster medium (ICM) is filled with hot and dilute gas. Global thermodynamic properties of this gas are now routinely measured from Chandra and XMM-Newton data. However, our understanding of gas motions is very limited mainly due to insufficient spectral resolution of current X-ray observatories. This limits our ability to probe important physical process in the ICM such as, e.g., heating of the gas, biases in hydrostatic mass measurements, mechanisms of particle acceleration and the origin of radio halos. I will show how we can overcome the problem of limited spectral resolution and measure the velocities of gas motions through high-resolution X-ray images of galaxy clusters. I will discuss the effective equation of state of gas fluctuations in the ICM, the measurements of velocity power spectra on a broad range of spatial scales and the role of turbulent dissipation in mechanical radio-mode AGN feedback. Finally, I will overview first direct velocity measurements with the Hitomi observatory and discuss their consistency with other indirect velocity probes.
Tuesday Dec 6:
Joint MKI/EAPS Colloquium: The Fastest Road to Finding Life Beyond Earth
Co-Host: R. Binzel
Abstract: Tuesday Dec 13:
The Evolution of Exoplanets Orbiting Low-mass Stars
Host: E. Newton