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<div style="direction: ltr;font-family: Tahoma;color: #000000;font-size: 10pt;"><span id="docs-internal-guid-ae24a741-a9d3-5c44-f746-66a0c78eed34">
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 28pt; font-family: 'Times New Roman'; color: rgb(192, 0, 0); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Spring 2017 Colloquium</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 16pt; font-family: 'Times New Roman'; font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Department of Physics & Astronomy</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 16pt; font-family: 'Times New Roman'; color: rgb(192, 0, 0); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Mar 9, Thursday, 4-5 PM in Science Building 127</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 14pt; font-family: 'Times New Roman'; vertical-align: baseline; white-space: pre-wrap;">(coffee and cookies will be served at 3:50 PM)</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 18pt; font-family: 'Times New Roman'; color: rgb(0, 176, 80); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Astrophysics</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 18pt; font-family: 'Times New Roman'; color: rgb(0, 0, 255); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Mapping out dense matter inside neutron stars
</span><span style="font-size: 18pt; font-family: 'Times New Roman'; color: rgb(0, 0, 255); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;"><br class="kix-line-break">
</span><span style="font-size: 18pt; font-family: 'Times New Roman'; color: rgb(0, 0, 255); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">using accreting transients</span><span style="font-size: 18pt; font-family: 'Times New Roman'; color: rgb(0, 0, 255); font-weight: 700; vertical-align: baseline; white-space: pre-wrap;"><br class="kix-line-break">
</span><span style="font-size: 14pt; font-family: 'Times New Roman'; font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Dr. Andrew Cumming</span></p>
<p dir="ltr" style="line-height:1.7999999999999998;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<span style="font-size: 14pt; font-family: 'Times New Roman'; font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">McGill University, Canada </span></p>
<p dir="ltr" style="line-height:1.7999999999999998;margin-top:0pt;margin-bottom:0pt;text-align: center;">
<img src="https://lh3.googleusercontent.com/hfv1Ax2KjE0loxeDDPtpsCxN44gGm-ORwXz2UsQb1izBQ4105cXmh_tpWxAnVi4ziYAKWQnMb53E_k5V0lB0qx2zMmk6pFdu-tYK0PAfSYmQg3ug_tl3kHT287BQSe5idnXhkGiJ" width="154" height="200" style="border: none; transform: rotate(0.00rad); -webkit-transform: rotate(0.00rad);" originalwidth="154" originalheight="200"></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: justify;">
<span style="font-size: 11pt; font-family: Cambria; vertical-align: baseline; white-space: pre-wrap; background-color: rgb(255, 255, 255);">Dr. Andrew Cumming earned B.S. (1995) and M.S. (1996) degrees from the University of Cambridge, and received Ph.D. (2000)
from the University of California, Berkeley. He was a postdoc at the Kavli Institute for Theoretical Physics (KITP) in Santa Barbara, and then a Hubble Fellow at the University of California, Santa Cruz. Dr. Cumming joined the McGill Department of Physics
in September 2004, becoming Associate Professor in 2009. He is an adjunct member of the Department of Physics, University of Montreal, a member of the Centre de Recherche en Astrophysique du Quebec (CRAQ), the Institut de Recherche sur les Exoplanetes (iREx),
the JINA Center for the Evolution of the Elements (JINA-CEE), and Associate Director of the McGill Space Institute (MSI). More information about Dr. Cumming and his research can be found at</span><span style="font-size: 11pt; font-family: Cambria; vertical-align: baseline; white-space: pre-wrap; background-color: rgb(255, 255, 255);"><br class="kix-line-break">
</span><a href="http://www.physics.mcgill.ca/~cumming/" style="text-decoration:none;"><span style="font-size: 11pt; font-family: Cambria; color: rgb(17, 85, 204); text-decoration: underline; vertical-align: baseline; white-space: pre-wrap; background-color: rgb(255, 255, 255);">http://www.physics.mcgill.ca/~cumming/</span><span style="font-size: 12pt; font-family: 'Times New Roman'; color: rgb(0, 0, 0); vertical-align: baseline; white-space: pre-wrap; background-color: rgb(255, 255, 255);"><br class="kix-line-break">
<br class="kix-line-break">
</span></a></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: justify;">
<span style="font-size: 14pt; font-family: Cambria; vertical-align: baseline; white-space: pre-wrap;"></span><span style="font-size: 14pt; font-family: Cambria; font-weight: 700; vertical-align: baseline; white-space: pre-wrap;">Abstract:</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: justify;">
<span style="font-size: 12pt; font-family: Cambria; vertical-align: baseline; white-space: pre-wrap; background-color: rgb(255, 255, 255);">Monitoring the response of neutron stars to transient events is emerging as a powerful new way to probe neutron star
interiors. In this talk I will discuss the constraints on neutron star interiors coming from observations of accreting neutron stars. When accreting neutron star transients go into quiescence, X-ray observations on timescales of months to years show that the
neutron star, heated by accretion, gradually cools. I will discuss the different pieces of physics that determine how quickly the star cools, and what we can learn from these observations. I will show that they give us access to the full range of physical
conditions from the surface to the core. This includes an observational signature of the deepest regions of the inner crust, where the matter is likely in the form of nuclear pasta, and the core, including the neutrino emissivity and the first limits on the
core heat capacity.</span></p>
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