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<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesdays at 11am, CAPT Foyer – Astro Coffee<o:p></o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesday 1<sup>st</sup> October, A113 CAPT at 11am – Astronomy Journal Club<o:p></o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif"><o:p> </o:p></span></b></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos",sans-serif">Tuesday 1<sup>st</sup> October, A113 CAPT at 1pm – Particle Cosmology Seminar<o:p></o:p></span></b></p>
<p class="MsoNormal"><span style="font-size:12.0pt">Dibya Chakraborty (Indian Institute of Technology, Madras)</span><o:p></o:p></p>
<p class="MsoNormal"><i><span style="font-size:12.0pt">Inflationary Models in String Theory<o:p></o:p></span></i></p>
<p class="MsoNormal"><i><span style="font-size:12.0pt"><o:p> </o:p></span></i></p>
<p class="MsoNormal"><span style="font-size:12.0pt;color:black;mso-ligatures:none">In this talk, I will discuss a phenomenon called cosmic inflation in which the Universe went through accelerated expansion to solve the horizon problem of Cosmological Microwave
Background within a billionth of a trillionth of a trillionth of a second, in the very early Universe. This accelerated expansion, in its minimal form, is driven by a scalar field (inflaton) and it takes place when this scalar field slowly rolls down a potential
well. However, the origin of this scalar field and the correct form of the scalar potential remains an open question in cosmology. I will present a string theory motivated model where the inflaton is connected to the geometry of the internal space -- the overall
volume of it drives the inflation. In particular, I will present a construction where the overall volume modulus (scalar field) is dynamically stabilized to an exponentially large value only via perturbative corrections, also known as perturbative large volume
scenario (LVS). In this framework, the robustness of the single-field inflationary model is checked against possible sub-leading corrections. In the later part of my talk, I will focus on the global embedding of the fibre inflation in perturbative LVS and
show how our constructions pose less challenge in realizing a successful period of inflation.<o:p></o:p></span></p>
<p class="MsoNormal"><i><span style="font-size:12.0pt"> </span></i><o:p></o:p></p>
<p class="MsoNormal"><span style="color:black">Link to join: <a href="https://teams.microsoft.com/l/meetup-join/19%3ameeting_OGM3OTk5NzQtZWEwZS00ZmUyLTk3MGUtZjFhY2M5OTU2MjI1%40thread.v2/0?context=%7b%22Tid%22%3a%2267bda7ee-fd80-41ef-ac91-358418290a1e%22%2c%22Oid%22%3a%22f3250584-4b5f-48fa-a897-08e77f2246b7%22%7d" target="_blank">
https://teams.microsoft.com/l/meetup-join/19%3ameeting_OGM3OTk5NzQtZWEwZS00ZmUyLTk3MGUtZjFhY2M5OTU2MjI1%40thread.v2/0?context=%7b%22Tid%22%3a%2267bda7ee-fd80-41ef-ac91-358418290a1e%22%2c%22Oid%22%3a%22f3250584-4b5f-48fa-a897-08e77f2246b7%22%7d</a><o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt"> </span></b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">Wednesday 2<sup>nd</sup> October, C5 Physics at 3.45pm – Astronomy Seminar</span></b><o:p></o:p></p>
<p class="MsoNormal"><span style="font-size:12.0pt">Amy Bonsor (IoA, Cambridge)<o:p></o:p></span></p>
<p class="MsoNormal"><i><span style="font-size:12.0pt">Rocky planets and the potential for life beyond the Solar System<o:p></o:p></span></i></p>
<p class="MsoNormal"><i><o:p> </o:p></i></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",sans-serif;color:black;mso-fareast-language:EN-US">We live in an epoch of exoplanet discovery. Within the next decade the discovery of rocky planets orbiting other stars will be commonplace.
However, in order to fully understand these exoplanetary systems and their potential to host life, we have to consider the planetary system as a whole. Information from host-star compositions, system architectures and white dwarfs that have accreted planetary
material add to our intuition. I will discuss how we can start to think about whether exoplanetary systems have the right material available and the right physical conditions for the origin of life. Our exploration of planetary systems beyond the Solar System
goes hand in hand with the journey of discovery of how life on Earth came to be.</span><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif"><o:p></o:p></span></p>
<p class="xmsonormal"><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">---<o:p></o:p></span></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">Thursday 3<sup>rd</sup> October at 1pm, A113 CAPT – Astronomy Seminar</span></b><o:p></o:p></p>
<p class="MsoNormal"><span style="font-size:12.0pt">Arif Babul (Victoria)<o:p></o:p></span></p>
<p class="MsoNormal"><i><span style="font-size:12.0pt">The Formation and Evolution Massive Galaxies in the Cosmos and their Circumgalactic Environment<o:p></o:p></span></i></p>
<p class="MsoNormal"><i><o:p> </o:p></i></p>
<p class="xmsonormal"><span style="font-size:12.0pt;font-family:"Aptos",sans-serif;color:black;mso-fareast-language:EN-US">Contrary to many stereotypes about massive galaxies, the observed systems are diverse in their star formation rates, kinematic properties,
and morphologies. Studying how they evolve into and express such diverse characteristics is an important piece of the galaxy formation puzzle. Here, we focus on a subset of massive galaxies, the brightest group galaxies (BGGs). We use a high-resolution
cosmological suite of simulations based on the Romulus galaxy formation model, and compare simulated central galaxies in group-scale halos at
</span><span style="font-size:12.0pt;font-family:"Cambria Math",serif;color:black;mso-fareast-language:EN-US">𝑧</span><span style="font-size:12.0pt;font-family:"Aptos",sans-serif;color:black;mso-fareast-language:EN-US"> = 0 to their observed counterparts.
Since most galaxy formation models are calibrated using measures that are strongly influenced by the properties and evolution of “normal” Milky-Way like galaxies, this exercise is also an opportunity to test the limits of these models. The comparison encompasses
the stellar mass-halo mass relation, various kinematic properties and scaling relations, morphologies, and the star formation rates. We find Romulus BGGs that are early-type S0 and elliptical galaxies as well as late-type disk galaxies; we find BGGs that are
fast-rotators as well as slow-rotators; and we observe BGGs transforming from late-type to early-type following strong dynamical interactions with satellites. In short, we find that Romulus reproduces the full spectrum of diversity in the properties of the
BGGs very well. Additionally, due to its superb mass and spatial resolution, Romulus also offers a unique window onto the joint evolution of the BGGs and the surrounding intragroup medium. With respect to the latter, we are able to observe the emergence
of multiphase structure - in the form of cold clouds - in the intragroup medium. Groups also experience repeated AGN feedback episodes that drive large-scale collimated outflows into the IGrM. While the present resolution does not allow direct exploration
of the coupling between the clouds and the AGN jets, we argue that the clouds will cause the SMBHs (and hence, the jets) to change direction every so often. Returning back to the BGGs, we find that early type galaxies can rejuvenate by growing disks, in agreement
with recent observations. However, we also note a tendency towards lower than the observed fraction of quenched BGGs, with increasing halo mass. The problem appears to be due to decreasing effectiveness of AGN feedback with increasing halo mass. Examining
some of the other galaxy formation models, we find that they too run into trouble on the same scale — but in an opposite sense. I will conclude by discussing what we are to make of this and what the path forward looks like.<o:p></o:p></span></p>
<p class="xmsonormal"><o:p> </o:p></p>
<p class="xmsonormal"><b><span style="font-size:16.0pt;font-family:"Aptos Display",sans-serif">Thursday 3<sup>rd</sup> October, A113 CAPT at 3pm – Particle Cosmology Journal Club</span></b><o:p></o:p></p>
<p class="MsoNormal"><span style="font-size:12.0pt">Oliver Gould<i><o:p></o:p></i></span></p>
<p class="MsoNormal"><span style="font-size:16.0pt">---</span><o:p></o:p></p>
<p class="MsoNormal"><b><span style="font-size:16.0pt">Fridays at 4pm, CAPT Foyer – CAPT Cakes</span></b><o:p></o:p></p>
<p class="MsoNormal">---<o:p></o:p></p>
<p class="MsoNormal"><span style="font-size:12.0pt">If you have any events/visitors you would like including in next week’s bulletin, please let me know.</span><o:p></o:p></p>
<p class="MsoNormal"><o:p> </o:p></p>
<p class="MsoNormal"><span style="mso-fareast-language:EN-GB">Best wishes</span><span style="mso-ligatures:none;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:6.0pt;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial",sans-serif;mso-fareast-language:EN-GB">Ella<o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:6.0pt;font-family:"Calibri",sans-serif;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal"><b><span style="font-family:"Arial",sans-serif;color:#009BBD;mso-fareast-language:EN-GB">Ella Batchelor
</span></b><span style="font-family:"Arial",sans-serif;color:#009BBD;mso-fareast-language:EN-GB">(she/her)</span><o:p></o:p></p>
<p class="MsoNormal"><b><span lang="EN-US" style="font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">Administrator</span></b><span style="mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">School of Physics & Astronomy</span><span lang="ZH-CN" style="font-size:9.0pt;font-family:"MS Gothic";color:#0F1245;mso-fareast-language:ZH-CN">
</span><span lang="EN-US" style="font-size:9.0pt;font-family:"MS Mincho";color:#0F1245;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">University of Nottingham</span><span lang="EN-US" style="font-size:9.0pt;font-family:"Calibri",sans-serif;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">A112a Centre for Astronomy & Particle Theory</span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">University Park</span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">Nottingham, NG7 2RD</span><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"><o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;mso-fareast-language:EN-GB"> <o:p></o:p></span></p>
<p class="MsoNormal" style="text-autospace:none"><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">+44 (0) 115 74 86778<b> </b></span><b><span lang="EN-US" style="font-size:9.0pt;color:#0F1245;mso-fareast-language:EN-GB">| </span></b><b><span lang="EN-US" style="font-size:9.0pt;font-family:"Arial",sans-serif;color:#0F1245;mso-fareast-language:EN-GB">
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<p class="MsoNormal" style="text-autospace:none"><span style="mso-fareast-language:EN-GB"><o:p> </o:p></span></p>
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