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<span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif; color:rgba(0, 0, 0, 1.0);" class=""><b class="">From:
</b></span><span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif;" class="">Debbie Meinbresse <<a href="mailto:meinbres@mit.edu" class="">meinbres@mit.edu</a>><br class="">
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<span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif; color:rgba(0, 0, 0, 1.0);" class=""><b class="">Subject:
</b></span><span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif;" class=""><b class="">please share with your undergrad and grad students -- MIT Kavli Institute for Astrophysics and Space Research: IAP Activities January 28-31</b><br class="">
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<span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif; color:rgba(0, 0, 0, 1.0);" class=""><b class="">Date:
</b></span><span style="font-family: -webkit-system-font, Helvetica Neue, Helvetica, sans-serif;" class="">January 24, 2019 at 7:29:59 PM EST<br class="">
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<span style="font-size: large;" class="">MIT Kavli Institute for Astrophysics and Space Research (MKI)</span></div>
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<h3 class=""><font size="4" class="">IAP 2019 Activities: January 28-31</font></h3>
<div class=""><font class="" style="font-size: 14px;">Check out MKI’s upcoming IAP activities. <font color="#ff2600" class="">Please note: If you are interested in taking a tour of the Operations Control Center for the Chandra X-ray Observatory, the sign-up
deadline is January 28 @ 12noon.</font></font></div>
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<div class=""><span class="" style="font-size: large;"><b class="">Monday, January 28</b></span></div>
<h3 class="">How Stars are Born</h3>
<h3 class=""><span class="" style="font-size: 12px;">Dr. Moritz Guenther, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">2:30 – 3:00pm in 37-252</span></em></span></h3>
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<p class="">While our Sun is almost 5 billion years old, stars still form in the the dark clouds of our Milky Way. When we observe those regions we can learn how star and planet formation works, so that we also understand the formation of our own solar system
and the Earth better. I will describe how we observe those regions that are hidden to the naked eye using infrared and X-ray telescopes to obtain stunning images of stellar nurseries. Zooming in on just a few of the young stars, I show how a gas cloud collapses
to form a hot gas core that is the birth place of another sun and possibly a few planets. This is the stage of star formation where I concentrate my own research and I will describe how professional astronomers gain access to space telescopes, share my experiences
of how to use the Hubble Space Telescope (HST) for my observations of young stars and I will show an example of how we process the observations to extract scientific conclusions. Star formation is a very active area of research with many open questions to
solve and certainly one of the areas in astronomy that delivers extremely beautiful images of the Milky Way that surrounds us.<o:p class=""></o:p></p>
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<h3 class="">Modern Cyclopses – The Era of Giant Telescopes</h3>
<h3 class=""><span class="" style="font-size: 12px;">Dr. Gabor Furesz, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">3:00 – 3:30pm in 37-252</span></em></span></h3>
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<p class="">While astronomical observations have been carried out for thousands of years it is only the past four centuries when our naked eyes have been aided by telescopes. With today’s ‘giant eyes’ we can peer really deep into the night sky, literally reaching
the edge of the (observable) Universe. But to get there we have to build larger and larger, ever more sensitive, better telescopes and instruments. It has been really just the past few decades when progress was exponential, just like in other fields: thanks
to computers, highly sensitive digital detectors and other modern design and manufacturing technologies. But progress in astronomical instrumentation is also influenced by commercialization, the consumer market, as well as history and politics – as these extremely
large and complex scientific machines require collaboration and unique technology developments that point beyond a single nation, even the U.S. One could rightfully ask: do we really need these even larger giant telescopes, if they are so expensive and we
already can see to the edge of the Universe? I will argue for the “yes” answer by showing a few very exciting science cases, like the detection and characterization of extrasolar planets and understanding the chemical evolution of the Universe. To investigate
these questions it is not enough to simply detect the light but also to analyze it in detail. While spectroscopy is a well established and great method to do so, it requires a lot of photons to be captured – which hopefully will be delivered by the next generation
of giant light buckets.<o:p class=""></o:p></p>
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<h3 class="">Exoplanet Science in the era of TESS</h3>
<h3 class=""><span class="" style="font-size: 12px;">Dr. Jenn Burt, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">3:30-4:00pm in 37-252</span></em></span></h3>
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<p class="">The beginning of the TESS spacecraft’s science mission in mid 2018 promises the detection of thousands of exoplanets orbiting bright, nearby stars. These planets will provide astronomers with our best ever opportunity to mount extensive follow up
observation efforts and try to understand the composition, distribution and evolution of planets in our galaxy. This talk will describe the anticipated TESS planet yield, its impact on the exoplanet field, and some of the follow up methods that astronomers
will use to probe the composition of the planets’ rocky cores and/or gaseous outer atmospheres.<o:p class=""></o:p></p>
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<h3 class=""><font size="4" class="">Tuesday, January 29</font></h3>
<div class=""><b class="" style="font-size: 14px;">Artificial Intelligence in Science</b></div>
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<h4 class="" style="margin-top: 0in;">Dr. Victor Pankratius, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">1:00-1:30pm in 37-252</span></em></h4>
<p class="MsoNormal">How can Artificial Intelligence help advance science? This presentation will outline new avenues for Computer-Aided Discovery in astronomy and geoscience.</p>
<h3 class="" style="margin: 0in 0in 0.0001pt;"><span class="" style="font-size: 11pt;"><br class="">
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<h3 class="" style="margin: 0in 0in 0.0001pt;">Roman warships in Experiment: Reconstruction and Sailing Tests<font size="4" class=""><o:p class=""></o:p></font></h3>
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<h4 class="" style="margin-top: 0in;">Dr. Moritz Gunther, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">1:30 – 2:30pm in 37-252<o:p class=""></o:p></span></em></h4>
<p class="MsoNormal">Warning: This talk is non-astronomical and contains actual videos and possibly sound. After the climax of its power internal struggle weakened the military position of the Roman Empire. A series of attacks in the 2nd and 3rd century AD
forced an adjustment of the military strategy in central Europe. Instead of further expansion, the borders of the empire were increasingly fortified. In Germany this lead to the construction of an impressive naval fleet on the rivers Rhine and Danube. Several
of the boats have been excavated. Our team has attempted a reconstruction of two types of vessel, the “navis lusoria” and the “Oberstimm” with a level of detail down to the hand-smithened nails with the correct metallurgy. A series of three working boats have
been built in original size. I will show pictures of the reconstruction phase, but concentrate on the on-the-water tests we have performed with different teams to access the speed, maneuverability and sailing performance of these boats. Particularly in sailing
the possibilities far exceeded the expectations. This result indicates a much larger operating radius of these vessels than previously estimated and thus a much higher flexibility of the river defense scheme which the empire relied on to keep the barbarians
at bay. See, e.g.: <a href="https://www.youtube.com/watch?v=8nV16slhP_s" class="">this movie</a></p>
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<h3 class="" style="margin: 0in 0in 0.0001pt;">The Future of X-ray Polarimetry in Astronomy<font size="4" class=""><o:p class=""></o:p></font></h3>
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<h4 class="" style="margin-top: 0in;">Dr. Herman Marshall, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">2:30-3:30pm in 37-252<o:p class=""></o:p></span></em></h4>
<p class="MsoNormal">I will present several projects to measure the X-ray polarizations of astronomical sources over the next 5-10 years. Previous observations were obtained in the 1970s for bright Galactic sources such as X-ray binaries and the Crab Nebula
using a Bragg reflection from graphite crystals, limiting the measurements to 2.6 and 5.2 keV. Recently, a few detections have been reported using Compton scattering at hard X-rays. A newly approved NASA mission is the Imaging X-ray Polarization Explorer (IXPE).
It would operate in the 2-8 keV range and is expected to launch in late 2020. It has an imaging capability, with a resolution of about a half arc-minute, and should detect X-ray polarizations as low as 1-5 percent for a dozen or more active galaxies, supernova
remnants, neutron stars, and X-ray binaries during a mission lifetime of a few years. I will describe the instrument and a few of the science goals. I will also describe a design for a sounding rocket based polarimeter to work in the 0.2-0.6 keV band. The
method uses gratings developed at MIT and multilayer coated mirrors. Potential targets include active galaxies, isolated neutron stars, and nearby black hole binaries in outburst. The configuration is extensible to orbital use, possibly to be combined with
other instruments to provide a bandpass from 0.2 to 50 keV.</p>
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<div class="" style="margin: 0in 0in 0.0001pt;"> <o:p class=""></o:p></div>
<h3 class="" style="margin: 0in 0in 0.0001pt;">Tour of the X-ray Polarimetry Lab — please note tour limit and prerequisite below<o:p class=""></o:p></h3>
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<h4 class="" style="margin-top: 0in;">Dr. Alan Garner, <em class=""><span class="" style="font-family: Calibri; font-style: normal;">3:45 – 4:45pm tour departs from 37-252<o:p class=""></o:p></span></em></h4>
<p class="MsoNormal">Tour of MIT’s X-ray Polarimetry Lab, where new X-ray instrumentation is currently being developed.</p>
<div class="" style="margin: 0in 0in 0.0001pt;"><b class="">Please Note:</b></div>
<div class="" style="margin: 0in 0in 0.0001pt;"><b class="">20 people max for tour. Advance sign-up required starting at 2:25pm in 37-252 immediately before Dr. Marshall’s talk. Attendance of talk is required for tour of the Lab. Tour will leave from 37-252
at 3:30pm. Tour attendees will walk as a group to NE83.</b><o:p class=""></o:p></div>
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<h3 class=""><font size="4" class="">Wednesday, January 30</font></h3>
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<div class="" style="margin: 0in 0in 0.0001pt;"><strong class=""><span class="" style="font-size: 14px;">Formation of Gold and other heavy elements via the R(apid neutron capture)-process</span></strong></div>
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<div class="" style="margin: 0in 0in 0.0001pt;"><strong class=""><i class="">Dr. Rana Ezzeddine,</i></strong><strong class=""> 1:30-2:00pm in NW22 interaction area</strong><span class="" style="color: rgb(84, 141, 212); font-family: Cambria; font-size: 12pt;"> </span></div>
<p class="MsoNormal">Most chemical elements up to Iron are formed in the core of the stars via nucleosynthesis fusion processes of lighter elements into heavier ones. Elements heavier than iron, however, require neutron-capture processes to take place. I will
talk about our current understanding of the formation of the heaviest elements, such as Gold and Uranium, via the (r)apid neutron-capture process in stars, especially within the latest exciting and ground-breaking multi-wavelength LIGO discovery of the GW170817
neutron star merger gravitational waves event.</p>
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<div class="" style="margin: 0in 0in 0.0001pt;"><strong class=""><span class="" style="font-size: 13pt; font-family: Cambria;"> </span></strong></div>
<div class="" style="margin: 0in 0in 0.0001pt;"><strong class=""><span class="" style="font-size: 14px;">An Explanation of the Science Behind LIGO</span><font face="Cambria" class="" style="font-size: 13pt;"><o:p class=""></o:p></font></strong></div>
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<strong class=""><i class="">Dr. Evan Hall and Mr. Benjamin Lane</i></strong><strong class="">, 2:00-3:00pm in NW22 interaction area</strong></b><span class="" style="font-size: 13pt; font-family: Cambria; color: rgb(54, 95, 145);"><o:p class=""></o:p></span></div>
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<div class="" style="margin: 0in 0in 0.0001pt;">How can we build a machine that can detect dead stars colliding with each other a billion light-years away? Come hear about the physics that goes into building the LIGO gravitational wave observatories, and the
astrophysics behind recent detections. Black holes, neutron stars, high-power lasers, and quantum optics!<font face="Cambria" class="" style="font-size: 13pt;"><o:p class=""></o:p></font></div>
<div class="" style="margin: 0in 0in 0.0001pt;"><span class="" style="font-family: Cambria; font-size: 13pt;"> </span></div>
<div class="" style="margin: 0in 0in 0.0001pt;"><strong class="" style="font-size: 14px;">Tour of the LIGO Lab</strong><span class="" style="font-size: 13pt; font-family: Cambria;"><o:p class=""></o:p></span></div>
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<div class="" style="margin: 0in 0in 0.0001pt;">Come see how the quantum optics research here at MIT will improve detections of binary neutron stars and black holes in LIGO to be more often and more informative.<o:p class=""></o:p></div>
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<div class="" style="margin: 0in 0in 0.0001pt;">Attendees will be divided into two groups of 10. Group A will hear talk by Dr. Evan Hall, while the Group B starts with the lab tour led by Mr. Benjamin Lane. Group A will take the lab tour following the talk,
while Group B will get the talk after the lab tour. Talk and tour 30 minutes each.<span class="" style="font-family: Cambria; font-size: 13pt;"><o:p class=""></o:p></span></div>
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<h3 class=""><font size="4" class="">Thursday, January 31</font></h3>
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<h2 class="" style="margin: 0in 0in 0.0001pt;"><span class="" style="font-size: 14px;">Solar Observing</span></h2>
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<h2 class="" style="margin: 0in 0in 0.0001pt;"><span class="" style="font-size: 12px;"><b class=""><i class="">Dr. Duane Lee, Dr. Michael Person, and MIT Astrogazers</i></b><b class="">, 12:00noon-2:00pm </b></span><b class="" style="font-size: 12px;">W20 MIT
Student Center (upper plaza area) <font color="#ff2600" class="">Weather Permitting!</font></b></h2>
<p class="MsoNormal">Join us for daytime stargazing! We will have solar telescopes set up so you can safely observe our closest star, the Sun. Swing on by for a quick look, and feel free to stay and chat with MIT astronomers.<o:p class=""></o:p></p>
<p class="MsoNormal">Sponsored by Kavli Institute for Astrophysics & Space Research, Earth, Atmospheric and Planetary Sciences, and Wallace Astrophysics Observatory. Special thanks to MIT Astrogazers for their assistance!<o:p class=""></o:p></p>
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<p class="MsoNormal"><b class=""><span class="" style="font-size: 14px;">Heavier than the Sun, Smaller than a City: The Neutron Star</span></b></p>
<p class="MsoNormal"><b class=""><i class="">Dr. Paul Hemphill,</i></b><b class=""> 1:30-2:00pm in 37-252</b></p>
<p class="MsoNormal">Neutron stars are some of the most extreme objects in the known Universe. More massive than the Sun, but just a few miles across, they have some of the highest densities, strongest magnetic fields, and highest temperatures of any celestial
objects. In this talk I will give an overview of the origins and properties of the various types of neutron stars that we observe, as well as how we can detect them and their usefulness for astrophysics as a whole.<b class=""><span class="" style="font-size: 10pt;"> </span></b></p>
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<p class="MsoNormal"><b class=""><span class="" style="font-size: 14px;">Exploring the Universe from Near to Far with the Chandra X-ray Observatory</span></b></p>
<p class="MsoNormal"><b class=""><i class="">Dr. Norbert Schulz,</i></b><b class=""> 2:00-2:30pm in 37-252</b></p>
<p class="MsoNormal">In the summer of 1999, NASA launched the third of its great observatories–the Chandra X-ray telescope. Like the Hubble Space telescope which preceded it, Chandra is designed to have an unprecedented ability to create images and spectra
of astrophysical objects, except working with high energy X-rays instead of optical light. This means that Chandra views some of the universe’s most exotic and energetic phenomena: supernovae, neutron stars, black holes, jets traveling at nearly the speed
of light emanating from near the center of clusters of galaxies. In this talk, we’ll take a tour of the discoveries made by the Chandra X-ray telescope, starting with studies of our own solar system, moving outward to nearby stars, to the center of our own
Galaxy where a black hole 40 millions times the mass of our Sun lurks, to distant clusters of Galaxies where the most massive black holes, billions of times the mass of our Sun, reside.</p>
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<p class="MsoNormal"><b class=""><span class="" style="font-size: 14px;">Tour of Operations Control Center for Chandra X-ray Observatory</span></b></p>
<p class="MsoNormal"><b class="">Tour departs 37-252 shortly after 2:30pm. Walk as a group to NE83.</b></p>
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<ul type="disc" class="" style="margin-top: 0in;">
<li class="MsoNormal"><b class=""><font color="#ff2600" class="">Tour signup deadline: Monday, Jan 28 @ 12noon. </font></b><o:p class=""></o:p></li><li class="MsoNormal"><b class="">Email <a href="mailto:meinbres@mit.edu" class="">meinbres@mit.edu</a> your first & last name (as it appears on your ID) & country of your citizenship. Tour attendance will be confirmed by end of day Jan 29.</b><o:p class=""></o:p></li><li class="MsoNormal"><b class=""><span class="" style="color: red;">The tour is limited to the first 20 people who sign up by Jan 28 @ noon.</span></b><b class=""> No enrollment limit for talks preceding tour.</b><o:p class=""></o:p></li></ul>
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<div class="">Please email me if you have questions about any of our IAP activities.</div>
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<div style="orphans: 2; widows: 2;" class=""><span class="x_x_Apple-style-span"><font class="x_x_Apple-style-span" face="'Franklin Gothic Medium'">Debbie Meinbresse | Assistant to the Director </font></span></div>
<div style="orphans: 2; widows: 2;" class=""><span style="font-family: 'Franklin Gothic Medium';" class="">MIT Kavli Institute for Astrophysics and Space Research</span></div>
<div style="orphans: 2; widows: 2;" class=""><span class="x_x_Apple-style-span" style="border-collapse: separate;">
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<div class="" style="font-family: Helvetica;"><font class="x_x_Apple-style-span" color="#103ffb"><font class="x_x_Apple-style-span" color="#1f497d" face="Franklin Gothic Medium"><span class="x_x_Apple-style-span" style="color: rgb(192, 0, 0);">Massachusetts
Institute of Technology (MIT)</span></font></font></div>
<div class="" style="font-family: Helvetica;"><font class="x_x_Apple-style-span" color="#414141"><font class="x_x_Apple-style-span" face="Franklin Gothic Medium">77 Massachusetts Av</font><font class="x_x_Apple-style-span" face="Franklin Gothic Medium">en</font><font class="x_x_Apple-style-span" face="Franklin Gothic Medium">ue,
37-241 Cambridge, MA 02139</font></font></div>
<div class="" style="font-family: Helvetica;"><font class="x_x_Apple-style-span" face="Franklin Gothic Medium" color="#414141">Tel: (617) 253-1456 | Fax: (617) 253-3111 |</font><font class="x_x_Apple-style-span" face="Franklin Gothic Medium" style="color: rgb(75, 75, 75);"> <a href="mailto:meinbres@mit.edu" class="">meinbres@mit.edu</a></font></div>
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